FN Thomson Reuters Web of Science™ VR 1.0 PT J AU ROUBIK, DW AF ROUBIK, DW TI TROPICAL POLLINATORS IN THE CANOPY AND UNDERSTORY - FIELD DATA AND THEORY FOR STRATUM PREFERENCES SO JOURNAL OF INSECT BEHAVIOR LA English DT Article DE APIS; BEES; CENTRIS; EUGLOSSINAE; MEGALOPTA; MELIPONINAE; POLLINATION; STRATOORIENTATION; STRATUM FIDELITY; TROPICAL FOREST CANOPY AB Claims have been made for a canopy preference by large bees pollinating tropical flowers-without data or tests that support or refute this opinion. The working hypothesis for bee foraging behavior in three dimensions is that forager experience can produce stratum fidelity, just as rewarding foraging produces floral fidelity. Wide-ranging search behavior should allow bees to track spatio-temporal distribution of resources. A systematic study of 20 bee species and 10 genera: Apis, Trigona, Eulaema, Centris, Euglossa, Scaptotrigona, Partamona, Megalopta, Rhinetula, and Oxytrigona was made in two forests in Panama. Two traps were operated simultaneously at canopy height and in the understory to test whether there were consistent stratum associations. Studies were continuous for 1 and 8 years. The only high-canopy foragers were two nocturnal bees, all the rest flew at both heights with similar probability or consistently came to lower traps. Large euglossines showed a tendency to forage high, which was directly related to their capacity for heat loss during flight, compared to smaller euglossines. They are also more conspicuous in warning coloration, another expected correlate of foraging more often in the open. Although large variance in stratum association predominates, some medium-sized diurnal forest bees avoid the exposed upper canopy, while some nocturnal bees tend to forage there. RP ROUBIK, DW (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 0 TC 55 Z9 63 U1 1 U2 11 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0892-7553 J9 J INSECT BEHAV JI J. Insect Behav. PD NOV PY 1993 VL 6 IS 6 BP 659 EP 673 DI 10.1007/BF01201668 PG 15 WC Entomology SC Entomology GA MH121 UT WOS:A1993MH12100001 ER PT J AU CHANCE, KV VARBERG, TD PARK, K ZINK, LR AF CHANCE, KV VARBERG, TD PARK, K ZINK, LR TI THE FAR-INFRARED SPECTRUM OF HI SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID HIGH-RESOLUTION MEASUREMENTS; REGION C1 MACALESTER COLL,DEPT CHEM,ST PAUL,MN 55105. NOAA,COOPERAT INST RES ENVIRONM SCI,BOULDER,CO 80303. UNIV OREGON,DEPT PHYS,EUGENE,OR 97403. UNIV COLORADO,BOULDER,CO 80303. RP CHANCE, KV (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. OI Chance, Kelly/0000-0002-7339-7577 NR 17 TC 18 Z9 18 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD NOV PY 1993 VL 162 IS 1 BP 120 EP 126 DI 10.1006/jmsp.1993.1272 PG 7 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA MC296 UT WOS:A1993MC29600009 ER PT J AU EMRY, RJ KORTH, WW AF EMRY, RJ KORTH, WW TI EVOLUTION IN YODERIMYINAE (EOMYIDAE, RODENTIA), WITH NEW MATERIAL FROM THE WHITE RIVER FORMATION (CHADRONIAN) AT FLAGSTAFF RIM, WYOMING SO JOURNAL OF PALEONTOLOGY LA English DT Article AB Three species of Yoderimyinae (Eomyidae: Rodentia) are recognized from the lower part of the White River Formation (early to medial Chadronian) in the Flagstaff Rim area, Wyoming. The new material allows an improved diagnosis for the subfamily. The enamel microstructure of Yoderimyinae supports its inclusion in the Eomyidae. A new genus, Zemiodontomys, is established for Yoderimys burkei Black, and new material, including upper dentition, is referred to this species. This genus differs from Yoderimys in having higher crowned and more lophodont teeth and in lacking P3. A second new genus, Litoyoderimys, is established for Yoderimys lustrorum Wood, and a new species, L. auogoleus, is referred to the genus. This genus has lower crowned, more cuspate teeth than Yoderimys. Through early and medial Chadronian time, evolution in yoderimyines includes the following morphologic transformations: increase in size; increase in crown height and lophodonty of cheek teeth; reduction of P3 (from double-rooted, to single-rooted, to absent); increase in relative size of P4 and p4; and increased longitudinal torsion of the mandible. C1 UNIV ROCHESTER,DEPT GEOL SCI,ROCHESTER,NY 14625. HOBART & WILLIAM SMITH COLL,DEPT GEOSCI,GENEVA,NY 14456. RP EMRY, RJ (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. NR 19 TC 8 Z9 9 U1 0 U2 2 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD NOV PY 1993 VL 67 IS 6 BP 1047 EP 1057 PG 11 WC Paleontology SC Paleontology GA ML948 UT WOS:A1993ML94800018 ER PT J AU MONFORT, SL ASHER, GW WILDT, DE WOOD, TC SCHIEWE, MC WILLIAMSON, LR BUSH, M RALL, WF AF MONFORT, SL ASHER, GW WILDT, DE WOOD, TC SCHIEWE, MC WILLIAMSON, LR BUSH, M RALL, WF TI SUCCESSFUL INTRAUTERINE INSEMINATION OF ELDS DEER (CERVUS-ELDI THAMIN) WITH FROZEN-THAWED SPERMATOZOA SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article ID FARMED FALLOW DEER; WHITE-TAILED DEER; DAMA-DAMA; ARTIFICIAL-INSEMINATION; RED DEER; PLASMA PROGESTERONE; ESTRUS; SEMEN; SYNCHRONIZATION; OVULATION AB This study tested the efficacy of assisted reproduction (synchronization of oestrus and intrauterine artificial insemination (AI)) in contributing to the captive propagation of an endangered species, the Eld's deer (Cervus eldi thamin). Semen was collected from males preselected on the basis of under-represented genotype. Motility of spermatozoa after thawing from ejaculates diluted with BF5F extender (8% glycerol), frozen on dry ice in 0.5 mi straws and stored in liquid nitrogen was 60-70%. Intravaginal progesterone-releasing devices (controlled internal drug release, CIDR-type G) were inserted into 20 adult EId's deer hinds for 14 days. In air hinds, semen (7.5-10 x 10(6) motile spermatozoa per uterine hem) was deposited by laparoscopy performed 70 h after removal of the CIDR device. Ovarian activity, before and after AI, was monitored by analysing pregnanediol-3 alpha-glucuronide (PdG) concentrations in voided urine collected three to seven times per week. During the period of CIDR device insertion, urinary PdG profiles were equal to, or above, normal luteal phase concentrations in all hinds. Within 48 h of device withdrawal, PdG concentrations returned to baseline values in 17 of the to females, and the onset of behavioural oestrus occurred at this time in 12 hinds. On the basis of sustained increases in urinary PdG, 9 of the 20 hinds were diagnosed as pregnant by 90 days after AI, all of which delivered offspring after a mean gestation of 241.1 days (range, 235-245). Seven singletons (two females, five males) were born alive and survived, and one singleton and one set of twins were stillborn (three females). This is the greatest number of pregnancies and offspring produced in a single AI trial for any endangered mammal. These results demonstrate that genotype preselection can be combined with assisted reproductive technologies, including use of frozen semen, to produce genetically valuable offspring useful for conserving a rare species. C1 GEORGE MASON UNIV,DEPT BIOL ENVIRONM BIOL & PUBL POLICY,FAIRFAX,VA 22039. NEW ZEALAND PASTORAL AGR RES INST LTD,RUAKURA AGR CTR,HAMILTON,NEW ZEALAND. RP MONFORT, SL (reprint author), SMITHSONIAN INST,CONSERVAT & RES CTR,NATL ZOOL PK,FRONT ROYAL,VA 22630, USA. FU NICHD NIH HHS [HD 00903] NR 34 TC 73 Z9 74 U1 2 U2 7 PU J REPROD FERTIL INC PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE, ENGLAND CB5 8DT SN 0022-4251 J9 J REPROD FERTIL JI J. Reprod. Fertil. PD NOV PY 1993 VL 99 IS 2 BP 459 EP 465 PG 7 WC Reproductive Biology SC Reproductive Biology GA MV127 UT WOS:A1993MV12700023 PM 8107027 ER PT J AU BROWN, JL BUSH, M WILDT, DE RAATH, JR DEVOS, V HOWARD, JG AF BROWN, JL BUSH, M WILDT, DE RAATH, JR DEVOS, V HOWARD, JG TI EFFECTS OF GNRH ANALOGS ON PITUITARY-TESTICULAR FUNCTION IN FREE-RANGING AFRICAN ELEPHANTS (LOXODONTA-AFRICANA) SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article ID POTENT LHRH AGONIST; LUTEINIZING-HORMONE; SERUM TESTOSTERONE; OVARIECTOMIZED EWES; ASIATIC ELEPHANT; MUSTH; RAT; ANTAGONISTS; INHIBITION; SECRETION AB We tested the ability of several GnRH analogues to suppress pituitary-testicular activity and potentially musth in free-ranging African elephants (Loxodonta africana). In Study I, adult bulls were given 4 or 12 mg GnRH antagonist (Detirelix) or saline i.m. on day 0 (n = 3 bulls per treatment). Animals were then recaptured on day 2 (about 48 h later) and given 300 mu g GnRH i.v. to assess the ability of the antagonist to block pituitary activity. Detirelix reduced (P < 0.05) basal concentrations of serum LH and testosterone on day 2 compared with day 0, with no effect of dose. Similarly LH and testosterone release induced by GnRH were also reduced (P < 0.05) in the Detirelix-treated bulls (50-70% reduction in peak concentrations). In Study 2, elephants were given 30 mg of a structurally similar GnRH antagonist (103-201-40; n = 6), 22.5 mg of a long-acting GnRH agonist (Lupron Depot; n = 4) or D-mannitol carrier (n = 4) i.m. on day 0. All bulls were recaptured and given GnRH on day 2 (103-201-40 treatment) or on days 2 and 20 (Lupron Depot treatment) after the initial injection. In contrast to Detirelix, 103-201-40 did not inhibit basal or GnRH-induced LH or testosterone secretion. Pituitary-testicular responses to Lupron Depot were initially stimulatory, as evidenced by increased (P < 0.05) LH and testosterone secretion on days 0 and 2. By day 20, basal LH concentrations had returned to baseline values and the response to GnRH was markedly reduced (P < 0.05), indicating that the pituitary was at least partially desensitized. Basal testosterone concentrations had also returned to baseline values by day 20 after Lupron Depot treatment. However, despite the attenuated LH response to GnRH, subsequent testosterone secretion was increased (P < 0.05) compared with controls, suggesting the testes of agonist-treated bulls had instead, become hyper-responsive to small increases in LH secretion. These results suggest that GnRH analogues can suppress the pituitary-gonadal axis in African elephants; however, longer treatment periods, more frequent injection intervals or higher doses are probably needed to inhibit testosterone secretion completely and, thus, musth. C1 CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. KRUGER NATL PK,SHUKUZA 1350,SOUTH AFRICA. RP BROWN, JL (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ANIM HLTH,WASHINGTON,DC 20008, USA. NR 38 TC 15 Z9 15 U1 2 U2 7 PU J REPROD FERTIL INC PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE, ENGLAND CB5 8DT SN 0022-4251 J9 J REPROD FERTIL JI J. Reprod. Fertil. PD NOV PY 1993 VL 99 IS 2 BP 627 EP 634 PG 8 WC Reproductive Biology SC Reproductive Biology GA MV127 UT WOS:A1993MV12700045 PM 8107048 ER PT J AU PISANO, DA AF PISANO, DA TI THE DIVIDED SKIES - ESTABLISHING SEGREGATED FLIGHT TRAINING AT TUSKEGEE, ALABAMA, 1934-1942 - JAKEMAN,RJ SO JOURNAL OF SOUTHERN HISTORY LA English DT Book Review RP PISANO, DA (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOUTHERN HISTORICAL ASSN PI ATHENS PA UNIV GEORGIA HISTORY DEPT, ATHENS, GA 30602 SN 0022-4642 J9 J SOUTHERN HIST JI J. South. Hist. PD NOV PY 1993 VL 59 IS 4 BP 789 EP 790 DI 10.2307/2210586 PG 2 WC History SC History GA MH724 UT WOS:A1993MH72400052 ER PT J AU AIELLO, A AF AIELLO, A TI BUGS OF THE WORLD - MCGAVIN,GC SO LIBRARY JOURNAL LA English DT Book Review RP AIELLO, A (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD NOV 1 PY 1993 VL 118 IS 18 BP 76 EP 76 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA ME965 UT WOS:A1993ME96500027 ER PT J AU FAUST, MA AF FAUST, MA TI 3 NEW BENTHIC SPECIES OF PROROCENTRUM (DINOPHYCEAE) FROM TWIN-CAYS, BELIZE - P-MACULOSUM SP-NOV, P-FORAMINOSUM SP-NOV AND P-FORMOSUM SP-NOV SO PHYCOLOGIA LA English DT Article ID PYRROPHYTA AB Three new benthic dinoflagellate species, Prorocentrum maculosum sp. nov., Prorocentrum foraminosum sp. nov. and Prorocentrum formosum sp. nov., are described from floating detritus and sediments in a subtropical mangrove island, Twin Cays, Belize, Central America, using scanning electron microscopy. Differences in the following characters of surface morphology separated the species: ornamentation of thecal plates (shape, size and number of valve pores) and the architecture of the periflagellar area and intercalary band. RP FAUST, MA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,MUSEUM SUPPORT CTR,SUITLAND,MD 20746, USA. NR 37 TC 42 Z9 45 U1 0 U2 2 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD NOV PY 1993 VL 32 IS 6 BP 410 EP 418 DI 10.2216/i0031-8884-32-6-410.1 PG 9 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA MG606 UT WOS:A1993MG60600002 ER PT J AU DAVIS, JL ELGERED, G NIELL, AE KUEHN, CE AF DAVIS, JL ELGERED, G NIELL, AE KUEHN, CE TI GROUND-BASED MEASUREMENT OF GRADIENTS IN THE WET RADIO REFRACTIVITY OF AIR SO RADIO SCIENCE LA English DT Article ID MILLIMETER-WAVE-PROPAGATION; INTERFEROMETRY; GEODESY; MODEL; FREQUENCIES; LENGTH; WATER AB We have used a ground-based microwave radiometer, known as a water vapor radiometer, to investigate the local spatial and temporal variation of the wet propagation delay for a site on the west coast of Sweden. The data were obtained from a wide range of azimuths and from elevation angles greater than 23.6-degrees (air mass 2.5). Visual inspection of the data suggested a simple ''cosine azimuth'' variation, implying that a first-order gradient model was required. This model was adequate for short time spans up to approximately 15 min, but significant temporal variations in the gradient suggested to us that we include gradient rate terms. The resulting six-parameter model has proven adequate (rms delay residual approximately 1 mm) for up to 30 min of data. Assuming a simple exponential profile for the wet refractivity gradient, the estimated gradient parameters imply average surface wet-refractivity horizontal gradients of order of 0.1-1 N km-1. These gradients are larger, by 1-2 orders of magnitude, than gradients determined by others by averaging over long (approximately 100-km) distances. This result implies that for applications that are sensitive to local gradients, such as wet propagation-delay models for radio-interferometric geodetic studies, the use of meteorological data from widely spread stations may be inadequate. The gradient model presented here is inadequate for times longer than about 30 min. even if no gradients are present, because of the complicated stochastic like temporal behavior of the wet atmosphere. When gradients are present, they can change magnitude by approximately 50% over 10-15 min. Nevertheless, our ability to fit the radiometer data implies that on timescales <30 min and for elevation angles >23.6-degrees, the local structure of the wet atmosphere can be described with a simple model. (The model is not limited to this range of elevation angles in principle.) The estimated gradient and gradient rate vectors have preferred directions, which indicates a prevailing structure in the three-dimensional temperature and humidity fields, possibly related to systematic behavior in large-scale weather systems and/or the local air-land-sea interaction at this site. C1 CHALMERS UNIV TECHNOL,ONSALA SPACE OBSERV,S-43900 ONSALA,SWEDEN. NASA,GODDARD SPACE FLIGHT CTR,INTERFEROMETR INC,GREENBELT,MD 20771. HAYSTACK OBSERV,NEROC,WESTFORD,MA 01886. RP DAVIS, JL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MAIL STOP 42,CAMBRIDGE,MA 02138, USA. RI Davis, James/D-8766-2013; Elgered, Gunnar/B-7052-2016 OI Davis, James/0000-0003-3057-477X; Elgered, Gunnar/0000-0001-5711-0073 NR 30 TC 86 Z9 90 U1 2 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0048-6604 J9 RADIO SCI JI Radio Sci. PD NOV-DEC PY 1993 VL 28 IS 6 BP 1003 EP 1018 DI 10.1029/93RS01917 PG 16 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA ML354 UT WOS:A1993ML35400006 ER PT J AU KENNICUTT, RC OEY, MS ZARITSKY, D HUCHRA, JP AF KENNICUTT, RC OEY, MS ZARITSKY, D HUCHRA, JP TI SYSTEMATICS OF H-II REGION ABUNDANCES IN GALAXIES SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article; Proceedings Paper CT 4th Texas Mexico Conference on Astrophysics CY MAR 01-02, 1993 CL AUSTIN, TX DE GALAXIES, ABUNDANCES; GALAXIES, ISM; H-II REGIONS ID SOUTHERN GALAXIES; SPIRAL GALAXIES; GRADIENTS; POPULATIONS AB Previous studies of gas-phase abundances in disk galaxies have favored late-type field spirals with bright H II regions. Here we report preliminary results from two surveys undertaken to delineate the abundance properties of the full range of galaxy types, luminosities, and structural properties. The galaxies in our sample show a wide range of mean disk abundances and abundance gradients. The mean abundances are correlated with galaxy type, luminosity, and circular velocity along what is predominantly a single-parameter sequence, though it is difficult to determine which of these variables is more fundamentally coupled to the disk abundance. The abundance-luminosity relation for spirals maps almost directly onto those for Magellanic irregular and elliptical galaxies. The slope of the abundance gradient is not closely coupled to Hubble type or luminosity, but appears to be correlated with bar structure. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CARNEGIE OBSERV,PASADENA,CA 91101. RP KENNICUTT, RC (reprint author), UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721, USA. NR 25 TC 7 Z9 7 U1 0 U2 0 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD NOV PY 1993 VL 27 SI SI BP 21 EP 28 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MQ642 UT WOS:A1993MQ64200003 ER PT J AU SCOWEN, P HESTER, J CODE, A MACKIE, G AF SCOWEN, P HESTER, J CODE, A MACKIE, G TI HST IMAGING OF THE WIND-BLOWN LOBE NGC 6165 SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article; Proceedings Paper CT 4th Texas Mexico Conference on Astrophysics CY MAR 01-02, 1993 CL AUSTIN, TX DE HYDRODYNAMICS; STARS, MASS LOSS ID SUPER-GIANTS; O-STARS; VELOCITIES; HD-148937 AB WFC observations of the lobe NGC 6165 have resolved clumps that are being photoevaporated by the intense UV radiation from HD 148937, in addition to the erosive effects of the strong stellar wind. The central object is a massive superluminous young star that is thought to be undergoing mass loss as it descends onto the main sequence. Analysis of several of these clumps in more detail indicates the presence of strong shocks between the photoevaporated gas from the clump and the stellar wind itself. Typical sizes of the clumps appear to be around 10(17) cm. Calculations are made of the mass flow rates and of the gasdynamic properties of the flows, revealing that the clump is behaving much like a cometary structure. Ejection mechanisms from the central star are discussed with regard to the observed morphology of the nebula. C1 UNIV WISCONSIN,WASHBURN OBSERV,MADISON,WI 53706. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP SCOWEN, P (reprint author), ARIZONA STATE UNIV,DEPT PHYS & ASTRON,TEMPE,AZ 85287, USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD NOV PY 1993 VL 27 SI SI BP 181 EP 185 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MQ642 UT WOS:A1993MQ64200037 ER PT J AU SCHULMAN, FY MONTALI, RJ BUSH, M CITINO, SB TELL, LA BALLOU, JD HUTSON, TL STPIERRE, M DUFOUR, JF GATMAITAN, Z JOHNSON, FB ARIAS, IM AF SCHULMAN, FY MONTALI, RJ BUSH, M CITINO, SB TELL, LA BALLOU, JD HUTSON, TL STPIERRE, M DUFOUR, JF GATMAITAN, Z JOHNSON, FB ARIAS, IM TI DUBIN-JOHNSON-LIKE SYNDROME IN GOLDEN LION TAMARINS (LEONTOPITHECUS-ROSALIA ROSALIA) SO VETERINARY PATHOLOGY LA English DT Article DE DUBIN-JOHNSON SYNDROME; GOLDEN LION TAMARINS; HYPERBILIRUBINEMIA; LIVER; PIGMENT ID MUTANT TR RATS; CONJUGATED HYPERBILIRUBINEMIA; TRANSPORT AB On routine blood screens, persistent conjugated hyperbilirubinemia was discovered in two groups of closely related adult female golden lion tamarins (Leontopithecus rosalia rosalia, n = 8). Bromosulfophthalein (BSP) retention tests were performed on four hyperbilirubinemic and three control tamarins. BSP excretion was delayed in hyperbilirubinemic tamarins as compared with controls. Grossly, liver of affected tamarins was dark brown to black, with a prominent reticulated pattern. Histologic examination revealed abundant intrahepatic pigment, primarily in a centrilobular and midzonal distribution. Most of the pigment did not react with Perls' Prussian blue method for iron, Hall's method for bilirubin, or the Armed Forces Institute of Pathology acid-fast method for lipofuscin but was positive with Fontana and lipofuscin-ferric ferricyanide reduction techniques. Liver from control golden lion tamarins had intrahepatocellular Perls' iron-positive pigment diffusely throughout the lobule with a small amount of Fontana method-positive pigment. Ultrastructurally, hepatocytes from a hyperbilirubinemic tamarin contained pleomorphic electron-dense structures within lysosomes. Transport studies demonstrated secretion of fluorescein isothiocyanate-labeled glycocholic acid, a fluorescent bile acid analog, into bile canaliculi and no secretion of carboxydichlorofluorescein diacetate, a non-bile acid organic anion, by liver from a hyperbilirubinemic tamarin. In contrast, control liver secreted carboxydichlorofluorescein diacetate readily into bile canaliculi. The clinicopathologic presentation of this syndrome in golden lion tamarins is similar to that described for Dubin-Johnson syndrome of human beings. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT PATHOL,WASHINGTON,DC 20008. SMITHSONIAN INST,NATL ZOOL PK,DEPT ANIM HLTH,WASHINGTON,DC 20008. SMITHSONIAN INST,NATL ZOOL PK,DEPT RES,WASHINGTON,DC 20008. ARMED FORCES INST PATHOL,WASHINGTON,DC. TUFTS UNIV,SCH MED,DEPT PHYSIOL,BOSTON,MA 02111. FU NIDDK NIH HHS [DK34928, DK35652] NR 22 TC 7 Z9 7 U1 0 U2 1 PU AMER COLL VET PATHOLOGIST PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 SN 0300-9858 J9 VET PATHOL JI Vet. Pathol. PD NOV PY 1993 VL 30 IS 6 BP 491 EP 498 PG 8 WC Pathology; Veterinary Sciences SC Pathology; Veterinary Sciences GA MN540 UT WOS:A1993MN54000001 PM 8116141 ER PT J AU PERIVOLAROPOULOS, L AF PERIVOLAROPOULOS, L TI EXISTENCE OF DOUBLE VORTEX SOLUTIONS SO PHYSICS LETTERS B LA English DT Article ID UNIFICATION AB We show analytically and numerically the existence of double vortex solutions in two-Higgs systems. These solutions are generalizations of the Nielsen-Olesen vortices and exist for all values of the parameters in the Lagrangians considered. We derive analytically the asymptotic behavior of the solutions and confirm it numerically by solving the field equations. Finally, we show that these solutions can be embedded in realistic theories like the two-doublet extension of the standard model. C1 BROWN UNIV, DEPT PHYS, PROVIDENCE, RI 02912 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, DIV THEORET ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. OI Perivolaropoulos, Leandros/0000-0001-9330-2371 NR 12 TC 8 Z9 8 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-2693 EI 1873-2445 J9 PHYS LETT B JI Phys. Lett. B PD OCT 28 PY 1993 VL 316 IS 4 BP 528 EP 533 DI 10.1016/0370-2693(93)91039-P PG 6 WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA MD457 UT WOS:A1993MD45700012 ER PT J AU RUIZLAPUENTE, P JEFFERY, DJ CHALLIS, PM FILIPPENKO, AV KIRSHNER, RP HO, LC SCHMIDT, BP SANCHEZ, F CANAL, R AF RUIZLAPUENTE, P JEFFERY, DJ CHALLIS, PM FILIPPENKO, AV KIRSHNER, RP HO, LC SCHMIDT, BP SANCHEZ, F CANAL, R TI A POSSIBLE LOW-MASS TYPE-IA SUPERNOVA SO NATURE LA English DT Article ID DA WHITE-DWARFS; SPACE DENSITY; SPECTRA; SN-1991T; DETONATIONS; EVOLUTION; EXPLOSION; HELIUM; STARS AB IN the standard model for type Ia supernovae1, a massive white dwarf in a binary system accretes matter from the companion star until it reaches the Chandrasekhar mass (the stability limit for degenerate-electron stars, corresponding to approximately 1.4 solar masses), and a runaway thermonuclear explosion ensues. In a popular variant of this model2, the companion star is also a white dwarf. But regardless of the nature of the companion, the invariance of the Chandrasekhar mass implies that all type Ia supernovae will be similar in luminosity3, making them ideal 'standard candles' for determining extragalactic distances, and hence the Hubble constant. In the context of the standard model, the recent type Ia supernova SN1991bg is hard to explain: it was underluminous at all observed epochs, leading to suggestions4,5 that the mass of the progenitor was unusually low. Here we present model calculations, based on more recent spectra, which point to a mass of the white dwarf of approximately 0.7 solar masses-well below the Chandrasekhar mass. Moreover, the late spectrum shows evidence of emission from low-velocity hydrogen gas, which might originate in material stripped from an extended, hydrogen-rich companion star. If our interpretation is correct, SN1991bg challenges both the double white-dwarf scenario, and the standard model for type Ia supernovae. C1 UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. UNIV CALIF BERKELEY,CTR PARTICLE ASTROPHYS,BERKELEY,CA 94720. INST ASTROFIS CANARIAS,LA LAGUNA,SPAIN. UNIV BARCELONA,DEPT ASTRON METEOROL,BARCELONA 7,SPAIN. RP RUIZLAPUENTE, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 30 TC 58 Z9 58 U1 0 U2 2 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD OCT 21 PY 1993 VL 365 IS 6448 BP 728 EP 730 DI 10.1038/365728a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA MC812 UT WOS:A1993MC81200053 ER PT J AU CAWTHORNE, TV WARDLE, JFC ROBERTS, DH GABUZDA, DC BROWN, LF AF CAWTHORNE, TV WARDLE, JFC ROBERTS, DH GABUZDA, DC BROWN, LF TI MILLIARCSECOND POLARIZATION STRUCTURE OF 24 OBJECTS FROM THE PEARSON-READHEAD SAMPLE OF BRIGHT EXTRAGALACTIC RADIO-SOURCES .1. THE IMAGES SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL LACERTAE OBJECTS, GENERAL; POLARIZATION; QUASARS, GENERAL; SURVEYS; TECHNIQUES, INTERFEROMETRIC ID CORE-DOMINATED QUASARS; ACTIVE GALACTIC NUCLEI; RANGE VLA OBSERVATIONS; BL LACERTAE OBJECTS; LINEAR-POLARIZATION; VLBI OBSERVATIONS; SUPERLUMINAL MOTION; INTERSTELLAR-MEDIUM; LAC OBJECTS; S5 SURVEY AB This paper presents the first survey of the milliarcsecond-scale linear polarization properties of compact extragalactic radio sources. Global VLBI observations in total intensity and linear polarization at a frequency of 5 GHz (lambda6 cm) of 24 sources from the Pearson-Readhead complete sample are presented. We have observed 12 quasars, eight BL Lacertae objects, and four galaxies, constituting about half of the Pearson-Readhead list. We show total intensity and polarization images of all 16 sources in which we detected significant polarized flux on milliarcsecond scales, and total intensity images of two additional sources. The properties of the individual sources are discussed at some length. A detailed analysis of the sample is given in an accompanying paper. C1 BRANDEIS UNIV,DEPT PHYS,WALTHAM,MA 02254. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALGARY,DEPT PHYS & ASTRON,CALGARY T2N 1N4,ALBERTA,CANADA. NR 81 TC 78 Z9 78 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1993 VL 416 IS 2 BP 496 EP 518 DI 10.1086/173253 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MA826 UT WOS:A1993MA82600009 ER PT J AU CAWTHORNE, TV WARDLE, JFC ROBERTS, DH GABUZDA, DC AF CAWTHORNE, TV WARDLE, JFC ROBERTS, DH GABUZDA, DC TI MILLIARCSECOND POLARIZATION STRUCTURE OF 24 OBJECTS FROM THE PEARSON-READHEAD SAMPLE OF BRIGHT EXTRAGALACTIC RADIO-SOURCES .2. DISCUSSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL LACERTAE OBJECTS, GENERAL; GALAXIES, JETS; GALAXIES, MAGNETIC FIELDS; POLARIZATION; QUASARS, GENERAL ID BL LACERTAE OBJECTS; SHOCKED RELATIVISTIC JETS; ACTIVE GALACTIC NUCLEI; RANGE VLA OBSERVATIONS; SUPERLUMINAL MOTION; SYNCHROTRON EMISSION; OPTICAL POLARIZATION; LINEAR-POLARIZATION; PARENT POPULATION; VLBI OBSERVATIONS AB The observations (Paper I) of the milliarcsecond-scale linear polarization properties of compact extragalactic radio sources from the Pearson-Readhead sample are discussed, In general, the linear polarization properties correlate strongly with optical identification, and, for the sources in this sample, galaxies, quasars, and BL Lacertae objects are quite distinct None of the compact radio sources identified with galaxies was detected in polarization on milliarcsecond scales. In contrast, most quasars and BL Lacertae objects have polarized structures, especially if they have prominent jets. We find systematic differences between quasars and BL Lacertae objects in the core polarizations, the orientations of the inferred magnetic fields in the jets, the visible lengths of the jets, and the behavior of the run of fractional polarization along the jets. Many of these differences may be caused by differences in the parsec-scale environment in quasars and BL Lacertae objects, such as in the density of the line-emitting gas. In BL Lacertae objects the inferred magnetic fields in the milliarcsecond scale jets are perpendicular to the jet axes, while observations of the best resolved quasars indicate that the fields are often quite closely parallel to the jet axes. This shows that BL Lacertae objects are not simply quasars whose jets make a particularly small angle to the line of sight. nor are they microlensed images of more distant quasars. There is also an anticorrelation between the degree of polarization and the total intensity of quasar jet components. Together, these results suggest a picture in which the knots of emission in the jets are associated with transverse shocks acting on a jet containing a mainly tangled magnetic field. In quasars the jets also contain a significant longitudinal component whose relative strength increases with distance from the core. If this is the case, the shocks in quasars must be weak so that the transverse field amplified by the shock never dominates the polarization. Our observations suggest that, in general, the magnetic field orientations in the milliarcsecond jets continue to scales intermediate between those resolved by VLBI and those accessible to the VLA. C1 BRANDEIS UNIV,DEPT PHYS,WALTHAM,MA 02254. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALGARY,DEPT PHYS & ASTRON,CALGARY T2N 1N4,ALBERTA,CANADA. NR 65 TC 98 Z9 98 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1993 VL 416 IS 2 BP 519 EP 535 DI 10.1086/173254 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MA826 UT WOS:A1993MA82600010 ER PT J AU BERTSCH, DL DAME, TM FICHTEL, CE HUNTER, SD SREEKUMAR, P STACY, JG THADDEUS, P AF BERTSCH, DL DAME, TM FICHTEL, CE HUNTER, SD SREEKUMAR, P STACY, JG THADDEUS, P TI DIFFUSE GAMMA-RAY EMISSION IN THE GALACTIC PLANE FROM COSMIC-RAY, MATTER, AND PHOTON INTERACTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC RAYS; DIFFUSE RADIATION; GALAXY, STRUCTURE; GAMMA RAYS, OBSERVATIONS ID INTERSTELLAR RADIATION-FIELD; MOLECULAR CLOUD COMPLEXES; LARGE-SCALE DISTRIBUTION; SOUTHERN MILKY-WAY; CO SURVEY; SOLAR CIRCLE; NEUTRAL HYDROGEN; CARBON-MONOXIDE; ATOMIC-HYDROGEN; ROTATION CURVE AB On the basis of the spatial distribution, intensity, and energy spectrum, the diffuse Galactic high-energy gamma radiation is believed to be the result of cosmic-rav interactions with matter, and to a lesser extent photons. This paper describes a model calculation of diffuse gamma-ray emission based on these interactions. Recent radio observations of the main interstellar components of matter on a scale of 0.5-degrees are used for the entire region within 10-degrees of the Galactic plane. A three-dimensional spatial model of the Galaxy is used to compute the emission from each volume element based on the matter, cosmic ray, and photon densities using well know interaction processes. Provisions are incorporated to account for the near-far ambiguity in determining the distance of matter in the inner Galaxy that results from Galactic rotation velocity-distance relationship. Cosmic-rav densities are modeled from the matter distribution using dynamical balance arguments, and they are expressed as a coupling scale length. This length, together with the normalization factor used to convert the observed CO line intensity to the molecular hydrogen density, are the only two adjustable parameters in the model. This approach provides a framework for calculating the observed intensity without invoking symmetries in longitude which can dilute spatial differences related to interesting spiral arm features, and it provides for a wide range of assumptions regarding the cosmic-ray distribution to be readily tested. The calculations are compared with existing data, and the values of the parameters are given. It is expected that new results from the EGRET instrument, when used with this model, will contribute to a better understanding of the cosmic ray distribution and the relation between CO and atomic hydrogen. Both of these issues are significant for studies of the dynamics and structure of the Galaxy. C1 UNIV NEW HAMPSHIRE,DURHAM,NH 03824. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV SPACE RES ASSOC,COLUMBIA,MD. RP BERTSCH, DL (reprint author), NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771, USA. RI Hunter, Stanley/D-2942-2012 NR 87 TC 171 Z9 172 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1993 VL 416 IS 2 BP 587 EP 600 DI 10.1086/173261 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MA826 UT WOS:A1993MA82600017 ER PT J AU GOMEZ, Y RODRIGUEZ, LF MORAN, JM AF GOMEZ, Y RODRIGUEZ, LF MORAN, JM TI DETECTION OF THE ANGULAR EXPANSION RATE AND DETERMINATION OF THE DISTANCE OF THE PLANETARY-NEBULA NGC-6302 SO ASTROPHYSICAL JOURNAL LA English DT Article DE PLANETARY NEBULAE, INDIVIDUAL (NGC-6302); TECHNIQUES, INTERFEROMETRIC AB Using VLA data from epochs separated by 2.75 yr, we measured the angular expansion of the planetary nebula NGC 6302 to be 1.75 +/- 0.3 milliarcseconds yr-1. Adopting an expansion velocity of 13 km s-1 for the ionized gas and a simple model for the structure and dynamics of the nebula, we estimate a distance of 1.6 +/- 0.6 kpc for NGC 6302. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP GOMEZ, Y (reprint author), Univ Nacl Autonoma Mexico, INST ASTRON, APDO POSTAL 70-264, MEXICO CITY 04510, DF, MEXICO. NR 8 TC 27 Z9 27 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1993 VL 416 IS 2 BP 620 EP 622 DI 10.1086/173263 PN 1 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MA826 UT WOS:A1993MA82600019 ER PT J AU SOON, WH ZHANG, Q BALIUNAS, SL KURUCZ, RL AF SOON, WH ZHANG, Q BALIUNAS, SL KURUCZ, RL TI THE MOUNT-WILSON-OBSERVATORY METALLICITY INDEX, CRV - COMPARISON WITH OTHER PHOTOMETRIC SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, ABUNDANCES; STARS, LATE-TYPE; TECHNIQUES, SPECTROSCOPIC ID DEFICIENT RED GIANTS; MAIN-SEQUENCE STARS; CA-II H; ABUNDANCE; EMISSION; GALAXY AB A new spectrophotometric index, C(RV), is assessed as a metallicity indicator for late-type stars. The index is the ratio of the measured photospheric fluxes in 20 angstrom wide passbands centered at 4001 and 3901 angstrom. C(RV) correlates directly with the metallicity index, m1, of the Stromgren uvby system and with the metallicity index hk, of Anthony-Twarog et al. (1991). Using observations of 236 dwarfs and 140 giants combined with stellar atmosphere models (Kurucz 1991), we compared the sensitivity of the C(RV) m1, and hk indices to metal abundance. We also studied the sensitivity of the C(RV), c1, and hk indices to surface gravity. The effect of interstellar extinction on all the indices was also studied from published mean extinction laws. We find that the C(RV) index is sensitive to the variation of metal abundance, [M], over the range examined (- 5.0 less than or similar to [M] less than or similar to 0.5). C(RV) is also more sensitive than the m, index at metal-poor conditions ([M] less than or similar to - 2.0). The C(RV) index has the following advantages: (1) the passbands of C(RV) are dominated by Fe lines, which reduce the uncertainty that may be introduced by the presence of lines of alpha-process elements with enhanced abundances at metal-poor conditions; (2) the effect of interstellar reddening is limited because the two passbands are separated in wavelength by only 100 angstrom. We also find that the atmospheric models produce results that agree qualitatively with the trends of observed indices on stellar parameters such as effective temperature, metallicity, and surface gravity. RP SOON, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 29 TC 16 Z9 16 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1993 VL 416 IS 2 BP 787 EP 805 DI 10.1086/173277 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MA826 UT WOS:A1993MA82600033 ER PT J AU SCHOMBERT, JM BARSONY, M HANLON, PC AF SCHOMBERT, JM BARSONY, M HANLON, PC TI LOW-MASS STAR-FORMATION IN COOLING FLOW GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE COOLING FLOWS; GALAXIES, PHOTOMETRY ID ELLIPTICAL GALAXIES; STANDARD STARS; H-I; CLUSTERS; PHOTOMETRY; SAMPLE; MATTER; VIRGO AB Observations are presented based on optical and near-IR imaging to support the idea that isolated and cluster cooling flow galaxies are enriched in low-mass stars, the result of recent, truncated IMF star formation from accreting gas. Galaxies with low accretion rates (M < 5 M. yr-1) have normal optical colors and gradients, but red V - K colors signaling an IMF enhanced in low-mass main-sequence stars. Cluster cooling flow ellipticals (M > 50 M. yr-1) selected to have blue optical colors indicative of recent star formation also show redder V-K colors with respect to expected values for a weak starburst. The strength of the starburst in the U - V, V - K diagram indicates an efficiency which places only 5% of the accreting matter into an IMF similar to that found in the Galactic disk and the remaining mass is again sited in low-mass stars. C1 CALTECH,JET PROPULS LAB,CTR INFRARED PROC & ANAL,MS100-22,PASADENA,CA 91125. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. RP SCHOMBERT, JM (reprint author), KITT PEAK NATL OBSERV,TUCSON,AZ 85726, USA. NR 32 TC 6 Z9 6 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 1993 VL 416 IS 2 BP L61 EP L65 DI 10.1086/187071 PN 2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MA827 UT WOS:A1993MA82700005 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI ON THE MUSEUMS RUINS - CRIMP,D, LAWLER,L SO LIBRARY JOURNAL LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIBS,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 15 PY 1993 VL 118 IS 17 BP 64 EP 64 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA MB315 UT WOS:A1993MB31500035 ER PT J AU RILEY, S AF RILEY, S TI ME AND MY MOM - HAUSER,M SO LIBRARY JOURNAL LA English DT Book Review RP RILEY, S (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD OCT 15 PY 1993 VL 118 IS 17 BP 88 EP 88 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA MB315 UT WOS:A1993MB31500186 ER PT J AU SEWARD, F AF SEWARD, F TI ISOLATED PULSARS - VANRIPER,KA, EPSTEIN,R, HO,C SO SCIENCE LA English DT Book Review RP SEWARD, F (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD OCT 15 PY 1993 VL 262 IS 5132 BP 444 EP 445 DI 10.1126/science.262.5132.444 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA MB859 UT WOS:A1993MB85900070 PM 17789956 ER PT J AU MCLAUGHLIN, BM BELL, KL AF MCLAUGHLIN, BM BELL, KL TI ELECTRON COLLISIONAL EXCITATION OF INTERMULTIPLET 1S(2)2S(2)2P(3) TO 1S(2)2S2P(4) AND 1S(2)2S(2)2P(2)3S OPTICALLY ALLOWED TRANSITIONS IN O-II SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID IMPACT EXCITATION; OSCILLATOR-STRENGTHS; OPACITY CALCULATIONS; ATOMIC OXYGEN; IONS AB Electron collisional excitation strengths are calculated, using an 11-state ab initio R-matrix method in LS coupling, for singly ionized atomic oxygen. All intermultiplet allowed transitions are investigated from the 1s(2)2s(2)2p3 S-4(o) 2D(o) and P-2(o) states to the 1s(2)2s2p4 P-4(e), 2D(e), P-2(e), S-2(e) and to a selected number of the n = 3 states, namely, 1s(2)2s(2)2p(2)3s P-4(e), 2D(e), P-2(e) and S-2(e). Effective collision strengths and rate coefficients are also presented for all possible allowed transitions between these multiplets over the temperature range 5000 to 1000 000 K. For many of these transitions no such data have previously been available. C1 QUEENS UNIV BELFAST,DEPT APPL MATH & THEORET PHYS,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. RP MCLAUGHLIN, BM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 25 TC 8 Z9 8 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD OCT 14 PY 1993 VL 26 IS 19 BP 3313 EP 3325 DI 10.1088/0953-4075/26/19/020 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA MC979 UT WOS:A1993MC97900020 ER PT J AU BROWN, GJN CROTHERS, DSF AF BROWN, GJN CROTHERS, DSF TI THE EXACT NATURE OF THE ELASTIC CONVERGENCE IN PHASE-INTEGRAL HALF-WAY HOUSE VARIATIONAL CONTINUUM DISTORTED-WAVE THEORY SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Letter AB The highest order term in an asymptotic expansion of a typical target-centred phase-integral half-way house variational continuum distorted-wave (PIVCDW) matrix element is obtained, with reference to a specific example. From this result we show that the probability amplitude for elastic scattering in PIVCDW theory is finite. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. RP BROWN, GJN (reprint author), QUEENS UNIV BELFAST,DEPT APPL MATH & THEORET PHYS,DIV THEORET & COMPUTAT PHYS RES,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. NR 8 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD OCT 14 PY 1993 VL 26 IS 19 BP L633 EP L639 DI 10.1088/0953-4075/26/19/001 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA MC979 UT WOS:A1993MC97900001 ER PT J AU CHRISTODOULOU, DM TOHLINE, JE STEIMANCAMERON, TY AF CHRISTODOULOU, DM TOHLINE, JE STEIMANCAMERON, TY TI KINEMATICAL MODELING OF WARPS IN THE H-I DISKS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, KINEMATICS AND DYNAMICS; GALAXIES, STRUCTURE; RADIO LINES, GALAXIES ID APERTURE-SYNTHESIS OBSERVATIONS; PREFERRED ORBIT PLANES; NEUTRAL HYDROGEN; NEWTONIAN DYNAMICS; TRIAXIAL GALAXIES; ROTATIONAL PROPERTIES; SPIRAL GALAXIES; GALACTIC WARPS; MASS PROBLEM; HIDDEN MASS AB In order to gain an appreciation for the general structure of warped gas layers in galaxies, we have con-structed kinematical, tilted-ring models of 21 galaxies for which detailed H I observations already exist in the literature. In this paper we present results for the 15 normal spiral galaxies of this sample that are not viewed edge-on. A comparison between our models and tilted-ring models of the same galaxies previously constructed by other authors shows that there is generally good agreement. We make an attempt to unify the notation of different authors who have published radio observations and/or kinematical models of individual galaxies in this sample. We also suggest how, in future work of this nature, model parameters should be presented and referenced in order to maintain a reasonable degree of consistency in the liteature. When viewed in the perspective of dynamical models, a twisted warped gas layer can be understood as arising from orbiting gas which is in the process of settling to a preferred orientation in the nonspherical, gravitational potential well of the galaxy. Hence, detailed kinematical modeling of a specific galaxy disk can provide not only information regarding the orientation and structure of its warp but also information about the shape (whether oblate or prolate) of the dark halo in which the disk is embedded. By examining a large number of galaxies in a consistent manner, we have deduced some general characteristics of warped disks that have heretofore gone unnoticed. We have also identified uniqueness problems that can arise in this type of modeling procedure which can considerably cloud one's ability to completely decipher an individual disk's structure. For 14 out of 15 spiral galaxies modeled here, we have been able to determine the local kinematical structure of the warp. Gas layers do not appear to warp more than approximately 40-degrees out of the plane defined by the central disk of the galaxy, but they can twist through angles as large as 170-degrees. The overall position of the warp and the gross geometric shape of the halo have been determined unambiguously only in cases where the twisting of the warp is relatively strong. (Examples of galaxies whose disks sit in an oblate halo are M33, M83, NGC 2805, NGC 2841, and NGC 3718; prolate halos appear to surround NGC 5033 and NGC 5055; and ambiguous cases, at present permitting equally good oblate and prolate halo models, are M31, NGC 300, NGC 3079, NGC 3198, NGC 6946, NGC 7331, and IC 342.) There appears to be a high degree of correlation between the twisting angles of kinematical models and precession angles derived from dynamical arguments. This correlation gives us considerable confidence that the kinematically identified twists in warped H I layers are real and that the general dynamical picture that has been put forward to explain their existence is correct. Adopting a scale-free, logarithmic halo potential having a quadrupole distortion eta, we conclude specifically that in each of these twisted warped disk systems the product etatau8 is approximately equal to 1, where tau8 is the age of the warped layer in 10(8) yr. C1 UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. LOUISIANA STATE UNIV,DEPT PHYS & ASTRON,BATON ROUGE,LA 70803. RP CHRISTODOULOU, DM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 76 TC 12 Z9 12 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1993 VL 416 IS 1 BP 74 EP 103 DI 10.1086/173216 PN 1 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MA328 UT WOS:A1993MA32800007 ER PT J AU COLLURA, A MAGGIO, A MICELA, G SCIORTINO, S HARNDEN, FR ROSNER, R AF COLLURA, A MAGGIO, A MICELA, G SCIORTINO, S HARNDEN, FR ROSNER, R TI ROSAT X-RAY-DETECTION OF EPSILON TAURUS - REVISITING THE CORONAL AND TRANSITION REGION EMISSION OF THE HYADES GIANTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE OPEN CLUSTERS AND ASSOCIATIONS, INDIVIDUAL (HYADES); STARS, CORONAE; STARS, GIANT; X-RAYS, STARS ID K-GIANTS; STARS; IUE; LITHIUM AB We report on a recent pointed X-ray observation of the Hyades giant epsilon Tau, obtained with the ROSAT PSPC. We confirm at higher significance the earlier ROSAT all-sky survey detection of this star, with an X-ray luminosity of approximately 10(28) ergs s-1. Epsilon Tau turns out to be the X-ray faintest among the four giants of the Hyades cluster, and the only one with no evidence of binarity. We rediscuss possible explanations, already put forward in previous studies, for the large spread in coronal and transition region emission observed among these stars. We revisit this issue in the light of our most recent knowledge on X-ray and UV emission properties of other Hyades and field stars. C1 IST OSSERV ASTRON,I-90134 PALERMO,ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CHICAGO,DEPT ASTRON & ASTROPHYS,CHICAGO,IL 60637. RP COLLURA, A (reprint author), CNR,IST APPLICAZ INTERDISCIPLINARI FIS,VIA ARCHIRAFI 36,PALERMO,ITALY. RI Maggio, Antonio/P-5700-2015 OI Maggio, Antonio/0000-0001-5154-6108 NR 26 TC 7 Z9 7 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1993 VL 416 IS 1 BP 204 EP 207 DI 10.1086/173226 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MA328 UT WOS:A1993MA32800017 ER PT J AU MELNICK, GJ MENTEN, KM PHILLIPS, TG HUNTER, T AF MELNICK, GJ MENTEN, KM PHILLIPS, TG HUNTER, T TI DISCOVERY OF INTERSTELLAR WATER LINES AT 437 GHZ, 439 GHZ, AND 471 GHZ - STRONG CASE FOR WATER MASER FORMATION BEHIND C-TYPE SHOCKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; MASERS; MOLECULAR PROCESSES; SHOCK WAVES; STARS, LATE-TYPE ID SUBMILLIMETER AB We report the first astronomical detections of the 7(53) --> 6(60), 6(43) --> 5(50), and 6(42) --> 5(51) transitions of water vapor (H2O) at frequencies near 437, 439, and 471 GHz, respectively. Using the Caltech Submillimeter Observatory we detected the 439 and 471 GHz lines toward a number of star-forming regions and the 437, 439, and 471 GHz lines toward several evolved stars. Maser action is likely to be present in all of these lines. The previously detected 325 GHz 5(15) --> 4(22) H2O maser line was also observed toward these sources. Assuming that these transitions are collisionally pumped, as is almost certainly the case for the water masers in star-forming regions, the luminosity ratios of these newly discovered masers, along with the 325 GHz maser line, clearly indicate that the gas temperature within the masing region is greater than or similar to 900 K. This finding is inconsistent with models that predict that H2O masers form behind fast (greater-than-or-equal-to 50 km s-1) dissociative shocks. Instead, these new data suggest that slow (less-than-or-equal-to 50 km s-1) nondissociative shocks are a more probable source for the observed maser emission. C1 CALTECH,INST TECHNOL,DIV PHYS MATH & ASTRON,PASADENA,CA 91125. RP MELNICK, GJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS 66,CAMBRIDGE,MA 02138, USA. OI Hunter, Todd/0000-0001-6492-0090 NR 14 TC 45 Z9 45 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 1993 VL 416 IS 1 BP L37 EP L40 DI 10.1086/187065 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA MA331 UT WOS:A1993MA33100010 ER PT J AU SHARMA, RD SUN, Y DALGARNO, A AF SHARMA, RD SUN, Y DALGARNO, A TI HIGHLY ROTATIONALLY EXCITED NITRIC-OXIDE IN THE TERRESTRIAL THERMOSPHERE SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID NONTHERMAL NITROGEN-ATOMS; EARTHS THERMOSPHERE; MARS AB Reaction of fast non-thermal N(4S) atoms with O2 molecules is shown to produce NO with large rotational and vibrational excitation. It is suggested that the process is responsible for the highly rotationally excited nitric oxide detected by the space shuttle experiment CIRRIS 1A. The influence of translationally hot atoms on the chemical composition and energetics of planetary thermospheres has been investigated by Logan and McElroy [1976], Solomon [1983], Fox and Dalgarno [1983], Nagy et al. [1990], and Gerard et al. [1991, 1993]. Shematovich et al. [1991], using a non-equilibrium kinetic model, have calculated the steady-state translational energy distribution of the ground state (4S) nitrogen atoms in the daylit atmosphere of the Earth at 140 km altitude. The calculated distribution shows a significant overpopulation of higher energy atoms over a Maxwell-Boltzmann distribution at the local translational temperature of 555K, of one and three orders of magnitude at energies of 0.5eV and 0.75eV, respectively, and the rate coefficient k(ne) for the process N(4S) + O2 --> NO + O + 1.385eV (1) is enhanced by several orders of magnitude over the thermal rate coefficient k(e). At an altitude of 110 km, where the temperature is about 275K, the thermal rate coefficient obtained from the standard expression k(e) = 4.4 x 10(-12)exp[-3220/T]cm3sec-1 [Rees, 1989] is 3.6 x 10(-17)cm3sec-1, whereas the nonequilibrium value is 2.0 x 10(-11)cm3s-1 [Shematovich et al. 1991]. The reaction of the hot N(4S) atoms with O2 provides an additional mechanism for the production of nitric oxide. Gerard et al. [1991] calculated that for solar minimum conditions at equatorial latitudes this additional mechanism contributes 6 to 30 percent of the nitric oxide,produced in the lower thermosphere. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP SHARMA, RD (reprint author), PHILLIPS LAB,DIV OPT ENVIRONM GPOS,BEDFORD,MA 01731, USA. NR 15 TC 40 Z9 40 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD OCT 8 PY 1993 VL 20 IS 19 BP 2043 EP 2045 DI 10.1029/93GL02486 PG 3 WC Geosciences, Multidisciplinary SC Geology GA MB580 UT WOS:A1993MB58000009 ER PT J AU ZABLUDOFF, AI GELLER, MJ HUCHRA, JP VOGELEY, MS AF ZABLUDOFF, AI GELLER, MJ HUCHRA, JP VOGELEY, MS TI THE KINEMATICS OF DENSE CLUSTERS OF GALAXIES .1. THE DATA SO ASTRONOMICAL JOURNAL LA English DT Article ID CLASSIFICATION REVISED RS; CFA REDSHIFT SURVEY; DARK MATTER THEORY; RICH CLUSTERS; X-RAY; ABELL CLUSTERS; LUMINOSITY FUNCTION; RADIAL-VELOCITIES; EVOLUTION; CANNIBALISM AB We have measured redshifts in the fields of the 31 R greater-than-or-equal-to 1 Abell clusters with 0.02 less-than-or-equal-to z less-than-or-equal-to 0.005 and Absolute value of b(II) > 30-degrees At least ten of the fields are severely contaminated by superimposed velocity peaks. We derive the mean velocities and velocity dispersions of the 25 dense peaks in the sample. The abundance of peaks, 6.6 x 10(-6)h3 Mpc-3, is consistent with the mean number density of R greater-than-or-equal-to 1 Abell clusters {Bahcall & Soneira [ApJ, 270, 20 (1983)]}. The range of velocity dispersions is 304-1346 km s-1. The median dispersion is 718 km s-1. The subset of eight systems with cD galaxies has a median velocity dispersion of 792 km s-1, close to that of non-cD systems (626 km s-1). When these data are combined with 16 cD cluster velocity dispersions from our previous study {Zabludoff et al. [ApJS, 74, 1 (1990) (ZHG)] and Dunn [Proceedings of NATO Conference (1991)]), eight of 25 cD galaxies have peculiar motions larger than half the cluster velocity dispersions. These findings further support the conclusions of Beers & Geller [ApJ, 274, 491 (1983)], ZHG, and Dunn (1991), who argue that cD galaxies do not lie in the global kinematic center, but in local potential minima. If so, systems with speeding cD's are probably a guide to substructure in dynamically evolving systems. RP ZABLUDOFF, AI (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 63 TC 112 Z9 112 U1 1 U2 2 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1993 VL 106 IS 4 BP 1273 EP 1300 DI 10.1086/116725 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LZ183 UT WOS:A1993LZ18300002 ER PT J AU ZABLUDOFF, AI GELLER, MJ HUCHRA, JP RAMELLA, M AF ZABLUDOFF, AI GELLER, MJ HUCHRA, JP RAMELLA, M TI THE KINEMATICS OF DENSE CLUSTERS OF GALAXIES .2. THE DISTRIBUTION OF VELOCITY DISPERSIONS SO ASTRONOMICAL JOURNAL LA English DT Article ID CFA REDSHIFT SURVEY; X-RAY; LUMINOSITY FUNCTION; RICH CLUSTERS; SURVEY SLICES; UNIVERSE AB From the survey of 31 Abell R greater-than-or-equal-to 1 cluster fields within 0.02 less-than-or-equal-to z less-than-or-equal-to 0.05 [Zabludoff et al., AJ, 106, 1273 (1993)] we extract 25 dense clusters with velocity dispersions sigma > 300 km s-1 and with number densities exceeding the mean for the Great Wall of galaxies [Geller & Huchra, Science, 246, 897, (1989)] by one deviation. From the CfA Redshift Survey (Huchra et al. 1993, in preparation), we obtain an approximately volume-limited catalog of 31 groups with velocity dispersions > 100 km s-1 and with the same number density limit. We combine these well-defined samples to obtain the distribution of cluster velocity dispersions. The group sample enables us to correct for incompleteness in the Abell catalog at low velocity dispersions. The clusters from the Abell cluster fields populate the high dispersion tail. For systems with velocity dispersions > 700 km s-1 approximately the median for R = 1 clusters [Zabludoff et al., ApJS, 74, 1 (1990)], the group and cluster abundances are consistent. The cumulative distributions of dispersions for clusters with or > 700 km s-1 and for groups are exponential laws of the form is-proportional-to 10-nsigma, n approximately 0.0015. The combined distribution is consistent with cluster x-ray temperature functions [Edge et al, MNRAS, 245, 559 (1990), and Henry & Arnaud, ApJ, 372, 410 (1991)]. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OSSERV ASTRON TRIEST,TRIESTE,ITALY. NR 37 TC 65 Z9 65 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1993 VL 106 IS 4 BP 1301 EP 1313 DI 10.1086/116726 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LZ183 UT WOS:A1993LZ18300003 ER PT J AU ZABLUDOFF, AI FRANX, M AF ZABLUDOFF, AI FRANX, M TI MORPHOLOGY AND KINEMATICS IN CLUSTERS OF GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article ID HYDRA-I CLUSTER; RICH CLUSTERS; CENTAURUS CLUSTER; COMA CLUSTER; SUBSTRUCTURE; CATALOG; EVOLUTION AB The existence of subclustering, infall, and the morphology-local density relation suggests that there should be differences in the kinematics of different morphological populations in clusters. From published data, we compile a sample of galaxy redshifts and types in six rich clusters of galaxies: A548, A1060, A1644, A1656, A2151, and DC 2048-52. In three clusters, the velocity distribution of spiral galaxies is different from those of other morphological populations: (1) spirals and ellipticals differ in A 1656 and A215 1, and (2) spirals and SO's differ in DC 2048 - 52. The differences in the distributions result primarily from differences in the mean velocities. The results are consistent with a picture in which a cluster irregularly accretes clumps of mostly spiral galaxies from the field, causing the combined velocity distribution to be asymmetric. These clumps might infall within the plane of a wall like the Great Wall of galaxies [Geller & Huchra, Science, 246, 897 (1989)]. Recent dynamical simulations show that the asymmetries may persist until after the clumps have merged with the central mass concentration [van Haarlem, PhD. thesis, Leiden University (1992)]. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 36 TC 31 Z9 31 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1993 VL 106 IS 4 BP 1314 EP 1323 DI 10.1086/116727 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LZ183 UT WOS:A1993LZ18300004 ER PT J AU POGGE, RW ESKRIDGE, PB AF POGGE, RW ESKRIDGE, PB TI STAR-FORMATION IN THE DISKS OF H I-RICH S0-GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article ID EARLY-TYPE GALAXIES; NEUTRAL HYDROGEN OBSERVATIONS; INTERSTELLAR-MEDIUM; LUMINOSITY FUNCTION; VIRGO CLUSTER; GAS; EMISSION; REGIONS; SPECTROPHOTOMETRY; CATALOG AB We present the results of a Halpha emission-line imaging survey of a sample of neutral-gas-rich SO galaxies. We find evidence of disk H II regions in 14 of our sample of 32 galaxies, detect nuclear or faint diffuse circumnuclear Halpha + [N II] emission in another 11 galaxies without disk H II regions, and obtain upper limits for 8 galaxies. We find a striking dichotomy between SO's with and without H II regions; either a galaxy has a number of H II regions, most often distributed into distinct rings or ringlike structures, or there are none down to detection limits equivalent to a single unreddened H II region ionized by single O stars. We find that the SO's without disk H II regions have a lower median M(HI)/L(B) than those with disk H II regions, but the distributions have a large range of dispersion. Our data suggest that SO's may lie in a regime where local threshold effects, perhaps primarily kinematic in origin, are more important in determining the star formation in these galaxies than the global stability mechanisms that recent empirical models for large-scale star formation have suggested prevail in later-type spirals. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP POGGE, RW (reprint author), OHIO STATE UNIV,DEPT ASTRON,COLUMBUS,OH 43210, USA. NR 66 TC 67 Z9 68 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1993 VL 106 IS 4 BP 1405 EP 1419 DI 10.1086/116735 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LZ183 UT WOS:A1993LZ18300012 ER PT J AU KENYON, SJ MIKOLAJEWSKA, J MIKOLAJEWSKI, M POLIDAN, RS SLOVAK, MH AF KENYON, SJ MIKOLAJEWSKA, J MIKOLAJEWSKI, M POLIDAN, RS SLOVAK, MH TI EVOLUTION OF THE SYMBIOTIC BINARY-SYSTEM AG PEGASI - THE SLOWEST CLASSICAL NOVA ERUPTION EVER RECORDED SO ASTRONOMICAL JOURNAL LA English DT Review ID ACCRETING WHITE-DWARFS; EMISSION-LINE SPECTRUM; HYDROGEN SHELL FLASHES; MAIN-SEQUENCE STARS; WOLF-RAYET STARS; MASS-LOSS; INFRARED-SPECTROSCOPY; COOL COMPONENTS; INHOMOGENEOUS-MEDIUM; STELLAR EVOLUTION AB We present an analysis of new and existing photometric and spectroscopic observations of the ongoing eruption in the symbiotic star AG Pegasi. These observations show that this binary has evolved considerably since the turn of the century. In particular, recent dramatic changes in both the UV continuum and the wind from the hot component allow a more detailed analysis than in previous papers. AG Peg is composed of a normal M3 giant (M(g) approximately 2.5M. and a hot, compact star (M(h) approximately 0.6M.) embedded in a dense, ionized nebula. The hot component powers the activity observed in this system, including a dense wind (v(r) approximately 1000 km s-1; M approximately 10(-6) M. yr-1) and a photoionized region within the outer atmosphere of the red giant. The hot component contracted in radius at roughly constant luminosity from 1850 to 1985. Its bolometric luminosity declined by a factor of approximately 4 during the past 5 yr, and it may now be evolving along the constant radius portion of the white dwarf cooling curve. Both the mass loss rate from the hot component and the emission activity decreased in step with the hot component's total luminosity, while photospheric radiation from the red giant companion remained essentially constant. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NICOLAUS COPERNICUS ASTRON CTR,PL-00716 WARSAW,POLAND. NICOLAUS COPERNICUS UNIV,INST ASTRON,PL-87100 TORUN,POLAND. NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. OI Kenyon, Scott/0000-0003-0214-609X NR 177 TC 72 Z9 72 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 1993 VL 106 IS 4 BP 1573 EP 1598 DI 10.1086/116749 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LZ183 UT WOS:A1993LZ18300026 ER PT J AU PYNE, T BIRKINSHAW, M AF PYNE, T BIRKINSHAW, M TI NULL GEODESICS IN PERTURBED SPACETIMES SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC MICROWAVE BACKGROUND; GRAVITATION; GRAVITATIONAL LENSING ID COSMIC BACKGROUND-RADIATION; DISTANCE-REDSHIFT RELATION; INHOMOGENEOUS UNIVERSE; APPROXIMATION SCHEME; GRAVITATIONAL-WAVES; GENERAL-RELATIVITY; ANISOTROPIES; FLUCTUATIONS; SKY AB We present a generalization and refinement of the Sachs-Wolfe technique, which unifies many of the approaches taken to date and clarifies both the physical and the mathematical character of the method. We illustrate the formalism with a calculation of the behavior of light passing a moving lens on a Minkowski back round. RP PYNE, T (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 29 TC 41 Z9 41 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1993 VL 415 IS 2 BP 459 EP 468 DI 10.1086/173178 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY327 UT WOS:A1993LY32700004 ER PT J AU KIRSHNER, RP JEFFERY, DJ LEIBUNDGUT, B CHALLIS, PM SONNEBORN, G PHILLIPS, MM SUNTZEFF, NB SMITH, RC WINKLER, PF WINGE, C HAMUY, M HUNTER, DA ROTH, KC BLADES, JC BRANCH, D CHEVALIER, RA FRANSSON, C PANAGIA, N WAGONER, RV WHEELER, JC HARKNESS, RP AF KIRSHNER, RP JEFFERY, DJ LEIBUNDGUT, B CHALLIS, PM SONNEBORN, G PHILLIPS, MM SUNTZEFF, NB SMITH, RC WINKLER, PF WINGE, C HAMUY, M HUNTER, DA ROTH, KC BLADES, JC BRANCH, D CHEVALIER, RA FRANSSON, C PANAGIA, N WAGONER, RV WHEELER, JC HARKNESS, RP TI SN-1992A - ULTRAVIOLET AND OPTICAL STUDIES BASED ON HST, IUE, AND CTIO OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (NGC-1380); SUPERNOVAE, INDIVIDUAL (SN-1992A); ULTRAVIOLET, STARS ID WHITE-DWARF MODELS; I SUPER-NOVA; SN-1987A POLARIMETRY; INTERSTELLAR LINES; SPECTRAL-LINES; MAXIMUM LIGHT; SPECTROPOLARIMETRY; POLARIZATION; NUCLEOSYNTHESIS; SPECTROSCOPY AB The Type Ia supernova SN 1992A in the S0 galaxy NGC 1380 was observed as a target of opportunity by the International Ultraviolet Explorer (IUE) and with great alacrity by the Hubble Space Telescope (HST). Here we present the HST and IUE spectra and photometry that we obtained, as well as optical spectra obtained at the Cerro Tololo Inter-American Observatory (CTIO). The HST Faint Object Spectrograph (FOS) spectra, from 5 and 45 days past maximum light, are the best UV spectra of a Type Ia supernova and reveal for the first time with good signal-to-noise ratio the Type Ia spectral region blueward of approximately 2650 angstrom. The UV photometry taken in the F175W, F275W, and F342W bands defined by the HST filters shows light curves that resemble the Type Ia template U light curve. Using data from SN 1992A and SN 1990N, we have constructed a Type Ia template light curve for the flux region near 2750 angstrom that is quite detailed from 14 days before maximum light to 22 days after maximum light and that extends to 77 days after maximum light. This light curve also resembles the template U light curve. A high-resolution HST Goddard High Resolution Spectrograph (GHRS) spectrum of SN 1992A shows no evidence for any interstellar lines attributable to NGC 1380 or to Galactic high-velocity clouds; low-velocity Galactic gas gives rise to relatively weak Mg II UV resonance absorption lines. These results are consistent with low extinction along the line of sight to SN 1992A. We have done a parameterized LTE analysis of the SN 1992A spectra using a slightly modified version of Woosley's delayed-detonation model DD4. We find that the features in the region blueward of approximately 2650 angstrom in the HST spectra are P Cygni absorptions due to blends of iron peak element multiplets and the Mg II resonance multiplet. Newly synthesized magnesium, sulfur, and silicon probably extend to velocities at least as high as approximately 19,000 km s-1. Newly synthesized Ni-Co may dominate the iron peak element abundances out to approximately 13,000 km s-1 in the ejecta of SN 1992A as in model DD4. However, further investigation of the extent of Ni-Co material in SN 1992A and other Type Ia supernovae is needed; this investigation could greatly help constrain Type Ia models. An analysis of the O I lambda7773 line in SN 1992A and other Type Ia supernovae implies that the oxygen-rich layer in typical Type Ia's extends over a velocity range of at least approximately 11,000-19,000 km s-1. None of the explosion models we considered, including model DD4, has an oxygen-rich layer that completely extends over this range. Model DD4, however, is promising, and further investigation of delayed-detonation models of its kind is merited. Spectropolarimetric observations taken by Spyromilio & Bailey of SN 1992A are consistent with the SN 1992A being spherically symmetric. We discuss these observations and the importance of taking spectropolarimetry of other Type Ia supernovae. C1 NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, GREENBELT, MD 20771 USA. NATL OPT ASTRON OBSERV, CERRO TOLOLO INTER AMER OBSERV, CASILLA 603, CHILE. MIDDLEBURY COLL, DEPT PHYS, MIDDLEBURY, VT 05753 USA. UNIV FED RIO GRANDE SUL, DEPT ASTRON, BR-91501-970 PORTO ALEGRE, RS, BRAZIL. LOWELL OBSERV, FLAGSTAFF, AZ 86001 USA. NORTHWESTERN UNIV, DEPT PHYS & ASTRON, EVANSTON, IL 60208 USA. SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. UNIV OKLAHOMA, DEPT PHYS & ASTRON, NORMAN, OK 73019 USA. UNIV VIRGINIA, DEPT ASTRON, CHARLOTTESVILLE, VA 22903 USA. STANFORD UNIV, DEPT PHYS, STANFORD, CA 94305 USA. STOCKHOLM OBSERV, S-13336 SALTSJOBADEN, SWEDEN. STANFORD UNIV, CTR SPACE SCI & ASTROPHYS, STANFORD, CA 94305 USA. UNIV TEXAS, DEPT ASTRON, AUSTIN, TX 78712 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, MS-19, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Hamuy, Mario/G-7541-2016 NR 110 TC 172 Z9 172 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1993 VL 415 IS 2 BP 589 EP 615 DI 10.1086/173188 PN 1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY327 UT WOS:A1993LY32700014 ER PT J AU JEFFERY, DJ AF JEFFERY, DJ TI THE RELATIVISTIC SOBOLEV METHOD APPLIED TO HOMOLOGOUSLY EXPANDING ATMOSPHERES SO ASTROPHYSICAL JOURNAL LA English DT Article DE LINE, FORMATION; RADIATIVE TRANSFER; RELATIVITY; STARS, ATMOSPHERES ID RADIATION-DRIVEN WINDS; HOT LUMINOUS STARS; WHITE-DWARF MODELS; LINE FORMATION; I SUPERNOVAE; RESONANCE LINES; P METHOD; APPROXIMATION; ENVELOPES; SPECTRUM AB In this paper, a detailed application of the relativistic Sobolev method of Hutsemekers & Surdej (HS) to homologously expanding atmospheres (with supernovae as the only example in mind) is described. The expressions for the common-direction (CD) and common-point (CP) frequency surfaces for homologous expansion are derived. The CP frequency surfaces are necessary for interacting line effects and were not considered by HS. Other important expressions of the relativistic Sobolev method are presented and briefly discussed. The validities for supernovae of the stationarity approximation and the relativistic Sobolev method's neglect of advection are briefly discussed. Some demonstration spectra calculated using the relativistic and classical Sobolev methods for models in homologous expansion are presented and compared. For the analysis of supernova atmospheres with the highest velocities observed, the relativistic Sobolev method treatment yields a small, but significant, improvement over the classical Sobolev method treatment. RP JEFFERY, DJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS-19,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 47 TC 15 Z9 16 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1993 VL 415 IS 2 BP 734 EP 749 DI 10.1086/173197 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY327 UT WOS:A1993LY32700023 ER PT J AU POPHAM, R NARAYAN, R HARTMANN, L KENYON, S AF POPHAM, R NARAYAN, R HARTMANN, L KENYON, S TI BOUNDARY-LAYERS IN PRE-MAIN-SEQUENCE ACCRETION DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; STARS, PRE-MAIN-SEQUENCE ID T-TAURI STARS; FU ORIONIS; EMISSION; OPACITY; MODEL; CYGNI AB We present self-consistent solutions, using alpha-viscosity, for the flow and energetics of optically thick boundary layers in accretion disks around pre-main-sequence stars. The solutions span a range of accretion rates from M = 10(-7) to 10(-4) M. yr-1 and are in qualitative agreement with observations of T Tauri and FU Orionis stars. The boundary layers in the solutions have two radial zones. The viscous dissipation occurs in a relatively narrow dynamical boundary layer, but most of the energy is actually radiated over a wider thermal boundary layer which extends to larger radii. We find that at low accretion rates, the boundary layer emission is clearly visible as a separate hot component in the combined spectrum of the disk and boundary layer, but this component is more difficult to distinguish at higher accretion rates. RP POPHAM, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 25 TC 56 Z9 56 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 1993 VL 415 IS 2 BP L127 EP L130 DI 10.1086/187049 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY329 UT WOS:A1993LY32900017 ER PT J AU WOODEN, DH RANK, DM BREGMAN, JD WITTEBORN, FC TIELENS, AGGM COHEN, M PINTO, PA AXELROD, TS AF WOODEN, DH RANK, DM BREGMAN, JD WITTEBORN, FC TIELENS, AGGM COHEN, M PINTO, PA AXELROD, TS TI AIRBORNE SPECTROPHOTOMETRY OF SN-1987A FROM 1.7 TO 12.6 MICRONS - TIME HISTORY OF THE DUST CONTINUUM AND LINE EMISSION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE DUST, EXTINCTION; INFRARED, STARS; SUPERNOVAE, INDIVIDUAL (SN-1987A) ID SPECTRAL IRRADIANCE CALIBRATION; BOLOMETRIC LIGHT-CURVE; LARGE MAGELLANIC CLOUD; SUPERNOVA 1987A; SN 1987A; INFRARED SPECTROPHOTOMETRY; PHOTOMETRIC-OBSERVATIONS; ABSOLUTE FLUXES; HYDROGENIC IONS; CARBON-MONOXIDE AB Spectrophotometric observations (1.7-12.6 mum) of SN 1987A from the Kuiper Airborne Observatory are presented for five epochs at 60, 260, 415, 615, and 775 days after the explosion. A variety of emission lines is seen, including members of the hydrogen Humphreys, Pfund, Brackett, and Paschen series, fine-structure lines of metals (including [Ni II] 6.634 mum, [Ni I] 7.507 mum, [Ar II] 6.985 mum, and [Co II] 10.521 mum), and CO and SiO molecular bands. The temporal evolution of the seven strongest H lines follows case C recombination theory and yields large values Of tau(Halpha) at 260 and 415 days. A mass of approximately 2 x 10(-3) M. is derived for stable nickel, and the ratio of the [Ni I] 7.507 mum and [Ni II] 6.634 mum line intensities yields a high ionization fraction of 0.9 in the nickel zone. Dust condensation is clearly detected at 615 days for the first time in a Type II supernova. At no time is there a 9.7 mum emission feature characteristic of interstellar astronomical silicates in the spectra of SN 1987A, nor are the 6.2 or 7.7 mum emission features attributed to polycyclic aromatic hydrocarbons seen. These airbome data are combined with other airbome and ground-based measurements taken at (or near) the same time to form five composite spectra of SN 1987A with wavelength coverage from approximately 3200 angstrom to 100 mum. The IR continuum emission between approximately 2 and 100 mum is compared with a three-component model-(1) hot photospheric continuum, (2) free-free and free-bound H emission, and (3) dust continuum-with the best fit determined using a nonlinear chi2 method. The dust continuum component is well characterized by a single-temperature graybody emission spectrum, i.e., by the radiation from gray grains or dust in optically thick clumps. At early times (less than 400 days after core collapse), the dust emission tracks the bolometric luminosity at about the 2% level. By 615 days, the fraction of the total luminosity contributed by the IR dust continuum increases dramatically to 0.45, and then to 0.83 at 775 days. We suggest that this dichotomy in the temporal evolution of the dust emission arises from dust with different origins. Circumstellar dust present before the supernova and then heated by it may account for the early emission. Newly condensed dust in the ejecta accounts for the later emission. A lower limit to the dust mass at 775 days is approximately 10(-4) M., but much more dust could be present. Since the emission is well fitted by a graybody, no information on the dust composition can be directly discerned from our data. C1 UNIV CALIF SANTA CRUZ OBSERV,LICK OBSERV,SANTA CRUZ,CA 95064. UNIV CALIF BERKELEY,RADIO ASTRON LAB,BERKELEY,CA 94720. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. LAWRENCE LIVERMORE NATL LAB,INST GEOPHYS & PLANETARY PHYS,LIVERMORE,CA 94550. RP WOODEN, DH (reprint author), NASA,AMES RES CTR,MAIL STOP 245-6,MOFFETT FIELD,CA 94035, USA. NR 109 TC 153 Z9 154 U1 0 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 1993 VL 88 IS 2 BP 477 EP 507 DI 10.1086/191830 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY026 UT WOS:A1993LY02600006 ER PT J AU Chambers, JE AF Chambers, J. E. TI A SIMPLE MAPPING FOR COMETS IN RESONANCE SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE Comets; short-period comets; dynamics; mean-motion resonance AB The dynamical evolution of a low inclination, intermediate period comet in mean-motion resonance with a giant planet can be described by a simple mapping giving the comet's heliocentric energy and ecliptic longitude at successive aphelia. Provided that the energy oscillations produced by the resonance are not too large, this mapping is linear. When the amplitude of the oscillations is close to the maximum possible within the resonance, the mapping can be improved by adding non-linear terms. C1 [Chambers, J. E.] Univ Manchester, Dept Astron, Manchester M13 9PL, Lancs, England. [Chambers, J. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chambers, JE (reprint author), Univ Manchester, Dept Astron, Manchester M13 9PL, Lancs, England. NR 4 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD OCT PY 1993 VL 57 IS 1-2 BP 131 EP 136 DI 10.1007/BF00692469 PG 6 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA V05NK UT WOS:000207132500014 ER PT J AU Lin, WA Delos, JB Jensen, RV AF Lin, W. A. Delos, J. B. Jensen, R. V. TI Order and chaos in semiconductor microstructures SO CHAOS LA English DT Article AB The semiclassical theory of ballistic electron transport in semiconductor microstructures provides a description of the quantum conductance fluctuations in terms of the classical distributions for the lengths and directed areas of the scattering trajectories. Because the classical dynamics differs for integrable (circular) and chaotic (stadium) scattering domains, experimental measurements of the conductance of these microstructures provide a unique probe of the quantum properties of classically regular and chaotic systems. To advance these theoretical and experimental studies we compare geometrical formulas for the classical distributions of lengths and areas with numerical simulations for microstructures examined in recent experiments, we assess the effects of lead size and placement, and we provide a critical analysis of the role of scattering "noise" on the classical and semiclassical predictions. Finally, we present a detailed comparison of the semiclassical theory with recent experimental measurements of the conductance fluctuations in circular-and stadium-shaped microstructures. C1 [Lin, W. A.; Delos, J. B.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Lin, W. A.; Delos, J. B.] Coll William & Mary, Dept Phys, Williamsburg, VA 23185 USA. [Jensen, R. V.] Texas A&M Univ, Dept Phys, College Stn, TX 77844 USA. RP Lin, WA (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. FU Office of Naval Research; National Science Foundation FX We would like to thank C. M. Marcus, H. Baranger, M. W. Keller, E. J. Heller, J. D. Meiss, and M. J. Berry for helpful discussions, communications, and/or conversations. This research was supported by the Office of Naval Research and the National Science Foundation. It was also partially supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic and Molecular Physics at Harvard University and Smithsonian Astrophysical Observatory. NR 18 TC 58 Z9 58 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1054-1500 J9 CHAOS JI Chaos PD OCT PY 1993 VL 3 IS 4 BP 655 EP 664 DI 10.1063/1.165994 PG 10 WC Mathematics, Applied; Physics, Mathematical SC Mathematics; Physics GA V22XU UT WOS:000208308700022 ER PT J AU DANIEL, P AF DANIEL, P TI NOT SLAVE, NOT FREE - THE AFRICAN-AMERICAN ECONOMIC EXPERIENCE SINCE THE CIVIL-WAR - MANDLE,JR SO ETHNIC AND RACIAL STUDIES LA English DT Book Review RP DANIEL, P (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ROUTLEDGE PI LONDON PA 11 NEW FETTER LANE, LONDON, ENGLAND EC4P 4EE SN 0141-9870 J9 ETHNIC RACIAL STUD JI Ethn. Racial Stud. PD OCT PY 1993 VL 16 IS 4 BP 738 EP 739 PG 2 WC Ethnic Studies; Sociology SC Ethnic Studies; Sociology GA MF756 UT WOS:A1993MF75600020 ER PT J AU CHEETHAM, AH JACKSON, JBC HAYEK, LAC AF CHEETHAM, AH JACKSON, JBC HAYEK, LAC TI QUANTITATIVE GENETICS OF BRYOZOAN PHENOTYPIC EVOLUTION .1. RATE TESTS FOR RANDOM CHANGE VERSUS SELECTION IN DIFFERENTIATION OF LIVING SPECIES SO EVOLUTION LA English DT Article DE BRYOZOA; NATURAL SELECTION; PHENOTYPIC VARIANCE; SKELETAL MORPHOLOGY; STYLOPOMA ID NATURAL-SELECTION; MORPHOLOGICAL-DIFFERENTIATION; NEOGENE BRYOZOAN; DARWIN FINCHES; CHARACTERS; SPECIATION; POPULATION; TEMPO; DRIFT; MACROEVOLUTION AB The possible roles of random genetic change and natural selection in bryozoan speciation were analyzed using quantitative genetic methods on breeding data for traits of skeletal morphology in two closely related species of the cheilostome Stylopoma. The hypothesis that morphologic differences between the species are caused entirely by mutation and genetic drift could not be rejected for reasonable rates of mutation maintained for as few as 10(3) to 10(4) generations. Divergence times this short or shorter are consistent with the abrupt appearances of many invertebrate species in the fossil record, commonly followed by millions of years of morphologic stasis. To produce these differences over 10(3) generations or fewer, directional selection acting alone would require unrealistically high levels of minimum selective mortality throughout divergence. Thus, selection is unnecessary to explain the divergence of these species, except as a means of accelerating the effects of random genetic change on shorter time scales (directional selection), or decelerating them over longer ones (stabilizing selection). These results are consistent with a variety of models of phenotypic evolution involving random shifts between multiple adaptive peaks. Similar results were obtained by substituting trait heritabilities and genetic covariances reconstructed by partitioning within- and among-colony phenotypic variance in place of the values based on breeding data. Quantitative genetic analysis of speciation in fossil bryozoan lineages is thus justified. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP CHEETHAM, AH (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. NR 51 TC 39 Z9 39 U1 0 U2 6 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 SN 0014-3820 J9 EVOLUTION JI Evolution PD OCT PY 1993 VL 47 IS 5 BP 1526 EP 1538 DI 10.2307/2410165 PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA NM707 UT WOS:A1993NM70700018 ER PT J AU CAILLET, C MACPHERSON, GJ ZINNER, EK AF CAILLET, C MACPHERSON, GJ ZINNER, EK TI PETROLOGIC AND AL-MG ISOTOPIC CLUES TO THE ACCRETION OF 2 REFRACTORY INCLUSIONS ONTO THE LEOVILLE PARENT BODY - ONE WAS HOT, THE OTHER WASNT SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID EARLY SOLAR-SYSTEM; RICH INCLUSIONS; ALLENDE METEORITE; CRYSTALLIZATION SEQUENCES; ORDINARY CHONDRITES; ION MICROPROBE; TRACE-ELEMENT; ORIGIN; AL-26; ABUNDANCES AB Two type B refractory inclusions found within several centimeters of each other in the foliated Leoville meteorite differ greatly in their styles of deformation, textures, and Mg-Al isotopic characteristics. One is a subspheroidal type B1 with textures similar to those observed previously in many type B1s from other CV3 meteorites, and whose deformation (fracturing, some granulation) has been almost entirely brittle in nature. Its isotopic composition shows Mg-26/Mg-24 correlated with Al-27/Mg-24 which, although disturbed, indicates a lower limit for initial Al-26/Al-27 of approximately 4.9 X 10(-5). The other inclusion is a highly elongate (L/W approximately 6) object whose long axis lies in the plane of foliation of the Leoville meteorite. It has a predominantly metamorphic texture, but relict islands of an earlier and more ''normal'' type B precursor are preserved in its core. The isotopic compositions of the two textural variants in this inclusion are different, anorthite in the metamorphic region mostly showing little or no excess Mg-26 [(Al-26/Al-27)0 < approximately 1.9 X 10(-6)] that would be attributable to in situ decay of Al-26 whereas anorthite in the relict islands shows well-resolved excess Mg-26 that gives a lower limit for initial Al-26/Al-27 of approximately 4.6 X 10(-5). The effects of shock metamorphism on the Leoville meteorite are clearly seen in both inclusions, including brittle deformation and local shock melting, but are not responsible for the major textural differences between the two inclusions. The most likely origin for the deformed and recrystallized features of the elongate inclusion is that it accreted onto the Leoville parent body while still very hot, and deformed into its present shape at the instant it impacted. If the resetting of the Al-Mg system occurred during this event, it must have taken place at least approximately 3.3 million years after formation of the precursor inclusion. The possibility that other deformed Leoville components accreted while hot should not be discounted. C1 SMITHSONIAN INST,US NATL MUSEUM NAT HIST,DEPT MINERAL SCI,WASHINGTON,DC 20560. WASHINGTON UNIV,DEPT PHYS,ST LOUIS,MO 63130. WASHINGTON UNIV,MCDONNELL CTR SPACE SCI,ST LOUIS,MO 63130. NR 45 TC 29 Z9 29 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD OCT PY 1993 VL 57 IS 19 BP 4725 EP 4743 DI 10.1016/0016-7037(93)90196-4 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA MD265 UT WOS:A1993MD26500016 ER PT J AU MARSDEN, BG WILLIAMS, GV KRONK, GW WADDINGTON, WG AF MARSDEN, BG WILLIAMS, GV KRONK, GW WADDINGTON, WG TI UPDATE ON COMET SWIFT-TUTTLE SO ICARUS LA English DT Article RP MARSDEN, BG (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 36 TC 20 Z9 20 U1 0 U2 0 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD OCT PY 1993 VL 105 IS 2 BP 420 EP 426 DI 10.1006/icar.1993.1138 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA ML417 UT WOS:A1993ML41700015 ER PT J AU OFTEDAL, OT AF OFTEDAL, OT TI THE ADAPTATION OF MILK SECRETION TO THE CONSTRAINTS OF FASTING IN BEARS, SEALS, AND BALEEN WHALES SO JOURNAL OF DAIRY SCIENCE LA English DT Article DE MILK SECRETION; FASTING; BEARS; MARINE MAMMALS ID HOODED SEAL; LEPTONYCHOTES-WEDDELLII; CYSTOPHORA-CRISTATA; ELEPHANT SEAL; ENERGETICS; LACTATION; INVESTMENT; MASS; BODY; HARP AB Although lactation is accompanied by increased nutrient demands for milk synthesis, many species of bears, true seals, and baleen whales fast for much or all of lactation. Large body mass in these species confers the advantage of greater stores of fat and protein relative to rates of milk production. Given the constraints on substrate availability during fasting, the milks of fasting mammals are predicted to be low in carbohydrate, protein, and water and to be high in fat. The milks of bears, true seals, and baleen whales conform to this prediction. Mammals that lactate while fasting may lose up to 40% of initial BW. The production of milk entails the export of up to one-third of body fat and 15% of body protein in the dormant black bear and in several seal species, which greatly depletes maternal resources and may represent a physiological threshold, because higher protein and fat outputs have only been measured in species that start feeding. The low K:Na ratio of seal and whale milks and the low Ca:casein and inverse Ca:P ratios in seal milks are unusual and warrant further study. RP OFTEDAL, OT (reprint author), SMITHSONIAN INST,DEPT ZOOL RES,WASHINGTON,DC 20008, USA. NR 68 TC 76 Z9 77 U1 2 U2 22 PU AMER DAIRY SCIENCE ASSN PI CHAMPAIGN PA 309 W CLARK ST, CHAMPAIGN, IL 61820 SN 0022-0302 J9 J DAIRY SCI JI J. Dairy Sci. PD OCT PY 1993 VL 76 IS 10 BP 3234 EP 3246 PG 13 WC Agriculture, Dairy & Animal Science; Food Science & Technology SC Agriculture; Food Science & Technology GA MB187 UT WOS:A1993MB18700040 PM 8227643 ER PT J AU GUPTA, MP CORREA, MD SOLIS, PN JONES, A GALDAMES, C GUIONNEAUSINCLAIR, F AF GUPTA, MP CORREA, MD SOLIS, PN JONES, A GALDAMES, C GUIONNEAUSINCLAIR, F TI MEDICINAL PLANT INVENTORY OF KUNA INDIANS .1. SO JOURNAL OF ETHNOPHARMACOLOGY LA English DT Article DE ETHNOPHARMACOGNOSY; KUNA INDIANS; PANAMA; MEDICINAL PLANTS ID NATURAL TERPENE DERIVATIVES; CARICA-PAPAYA FRUIT; PIPER-AURITUM; ANTIMICROBIAL ACTIVITY; EUPHORBIACEOUS PLANTS; TRADITIONAL MEDICINE; BIOLOGICAL-ACTIVITY; MUTAGENICITY TESTS; ROSA-SINENSIS; ACID AB Results of an ethnopharmacognostic survey of 90 plants used by the Kuna Indians of San Blas Islands, who live in Ailigandi, are listed. Results of a literature search are also reported, including medical uses, known constituents and pharmacological effects. C1 UNIV PANAMA HERBARIUM,PANAMA CITY,PANAMA. UNIV PANAMA,COLL HUMANITIES,ANTHROPOL RES,PANAMA CITY,PANAMA. SMITHSONIAN TROP RES INST,PANAMA CITY,PANAMA. RP GUPTA, MP (reprint author), ESTAFETA UNIV,COLL PHARM,CTR PHARMACOGNOST RES PANAMANIAN FLORA,APARTADO 10767,PANAMA CITY,PANAMA. OI Gupta, Mahabir/0000-0002-9302-7864 NR 327 TC 32 Z9 32 U1 0 U2 2 PU ELSEVIER SCI IRELAND LTD PI CLARE PA CUSTOMER RELATIONS MANAGER, BAY 15, SHANNON INDUSTRIAL ESTATE CO, CLARE, IRELAND SN 0378-8741 J9 J ETHNOPHARMACOL JI J. Ethnopharmacol. PD OCT PY 1993 VL 40 IS 2 BP 77 EP 109 DI 10.1016/0378-8741(93)90054-9 PG 33 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA MQ168 UT WOS:A1993MQ16800001 PM 8133656 ER PT J AU COFFEY, WT CROTHERS, DSF KALMYKOV, YP MASSAWE, ES WALDRON, JT AF COFFEY, WT CROTHERS, DSF KALMYKOV, YP MASSAWE, ES WALDRON, JT TI EXACT ANALYTIC FORMULAS FOR THE CORRELATION TIMES FOR SINGLE-DOMAIN FERROMAGNETIC PARTICLES SO JOURNAL OF MAGNETISM AND MAGNETIC MATERIALS LA English DT Letter AB Exact solutions for the longitudinal relaxation time T-parallel to and the complex susceptibility x(parallel to)(omega) of a thermally agitated single domain ferromagnetic particle are presented for the simple uniaxial (Maier-Saupe) potential of the crystalline anisotropy considered by Brown [Phys. Rev.130 (1963) 1677]. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RUSSIAN ACAD SCI,INST RADIOENGN & ELECTR,FRYAZINO 141120,RUSSIA. DUBLIN CITY UNIV,SCH COMP APPLICAT,DUBLIN 9,DUBLIN,IRELAND. QUEENS UNIV BELFAST,DEPT APPL MATH & THEORET PHYS,DIV THEORET & COMPUTAT PHYS RES,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. RP COFFEY, WT (reprint author), UNIV DUBLIN TRINITY COLL,DEPT MICROELECTR & ELECT ENGN,DUBLIN 2,DUBLIN,IRELAND. RI Kalmykov, Yuri /F-6400-2012 OI Kalmykov, Yuri /0000-0002-7665-8189 NR 11 TC 26 Z9 26 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-8853 J9 J MAGN MAGN MATER JI J. Magn. Magn. Mater. PD OCT PY 1993 VL 127 IS 3 BP L254 EP L260 DI 10.1016/0304-8853(93)90039-5 PG 7 WC Materials Science, Multidisciplinary; Physics, Condensed Matter SC Materials Science; Physics GA MF529 UT WOS:A1993MF52900002 ER PT J AU EBERHARD, WG PEREIRA, F AF EBERHARD, WG PEREIRA, F TI FUNCTIONS OF THE MALE GENITALIS SURSTYLI IN THE MEDITERRANEAN FRUIT-FLY, CERATITIS-CAPITATA (DIPTERA, TEPHRITIDAE) SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article AB The male surstyli of the medfly, Ceratitis capitata, are used both to nip the female and thus apparently to induce her to extend her aculeus and to clamp her aculeus after it is extended so that intromission can occur. The design of the surstyli results in a very strong mechanical clamp. C1 UNIV COSTA RICA,ESCUELA BIOL,SAN JOSE,COSTA RICA. RP EBERHARD, WG (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 11 TC 18 Z9 18 U1 0 U2 2 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD OCT PY 1993 VL 66 IS 4 BP 427 EP 433 PG 7 WC Entomology SC Entomology GA NE350 UT WOS:A1993NE35000009 ER PT J AU WHITE, PJ RALLS, K AF WHITE, PJ RALLS, K TI REPRODUCTION AND SPACING PATTERNS OF KIT FOXES RELATIVE TO CHANGING PREY AVAILABILITY SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Article AB The occurrence of drought and a corresponding decline in the availability of the primary prey of San joaquin kit foxes (Vulpes macrotis mutica) during 1990 and early 1991 provided a unique opportunity to document the effect of changing food resources on kit fox productivity and spacing patterns. Thus, we studied reproduction and spacing patterns of 38 kit foxes on a 110-km2 study area of the Carrizo Plain Natural Area, California from December 1988 through November 1991. The primary effect of prey scarcity on kit foxes was to decrease reproductive success; none of 9 collared females reproduced in 1990. Home ranges of members of the same social group overlapped extensively (xBAR = 70.0 +/- 3.0 [SE] %, n = 20), whereas those of foxes in adjacent social groups overlapped only slightly (xBAR = 14.0 +/- 2.0%, n = 73). Individual home ranges averaged 11.6 +/- 0.9 km2 (n = 21) and did not change in size for foxes monitored among years (P = 0.31). Overlap between home ranges of adjacent, same-sex foxes decreased (P = 0.02) during prey scarcity. Foxes apparently maintained relatively exclusive home ranges of sufficient size to sustain their own body mass and condition during periods of prey scarcity. The maintenance of large and relatively non-overlapping home ranges in kit foxes may be an adaptation to drought-induced periods of prey scarcity that are episodic and temporary in this region of the country. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RP WHITE, PJ (reprint author), UNIV WISCONSIN,DEPT WILDLIFE ECOL,MADISON,WI 53706, USA. NR 24 TC 61 Z9 62 U1 3 U2 15 PU WILDLIFE SOC PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814-2197 SN 0022-541X J9 J WILDLIFE MANAGE JI J. Wildl. Manage. PD OCT PY 1993 VL 57 IS 4 BP 861 EP 867 DI 10.2307/3809090 PG 7 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA MB571 UT WOS:A1993MB57100027 ER PT J AU GALANTE, G AF GALANTE, G TI EARLY PLAINS INDIAN PAINTED HIDES SO MAGAZINE ANTIQUES LA English DT Article RP GALANTE, G (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER INDIAN,NEW YORK,NY, USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU BRANT PUBL, INC PI NEW YORK PA 575 BROADWAY, NEW YORK, NY 10012 SN 0161-9284 J9 MAG ANTIQUES JI Mag. Antiq. PD OCT PY 1993 VL 144 IS 4 BP 530 EP 539 PG 10 WC Art SC Art GA LY518 UT WOS:A1993LY51800014 ER PT J AU SMITH, PL LEAN, JL CHRISTENSEN, AB HARVEY, KL JUDGE, DL MOORE, RL TORR, MR WOODS, TN AF SMITH, PL LEAN, JL CHRISTENSEN, AB HARVEY, KL JUDGE, DL MOORE, RL TORR, MR WOODS, TN TI SOURCE - THE SOLAR ULTRAVIOLET-RADIATION AND CORRELATIVE EMISSIONS MISSION SO METROLOGIA LA English DT Article ID IRRADIANCE VARIATIONS; FLUX; MODEL AB The Solar Ultraviolet Radiation and Correlative Emissions (SOURCE) mission is intended to advance our ability to specify the spectral irradiance of the Sun in the extreme ultraviolet (EUV) wavelength range through simultaneous, radiometrically accurate measurements of the solar EUV spectral irradiance and measurements, including EUV and visible images, of solar parameters that are correlated with the EUV flux. The data will be used in combination with empirical modelling to develop and validate a more accurate system of proxy, or surrogate, indices for the solar EUV flux. C1 AEROSP CORP,LOS ANGELES,CA 90009. SOLAR PHYS RES CORP,TUCSON,AZ 85718. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. UNIV SO CALIF,CTR SPACE SCI,LOS ANGELES,CA 90089. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. HIGH ALTITUDE OBSERV,BOULDER,CO 80307. RP SMITH, PL (reprint author), USN,RES LAB,DIV SPACE SCI,WASHINGTON,DC 20375, USA. OI Lean, Judith/0000-0002-0087-9639 NR 24 TC 0 Z9 0 U1 0 U2 0 PU BUREAU INT POIDS MESURES PI SEVRES CEDEX PA B1 PM PAVILLION DE BRETUEIL, F-92312 SEVRES CEDEX, FRANCE SN 0026-1394 J9 METROLOGIA JI Metrologia PD OCT PY 1993 VL 30 IS 4 BP 275 EP 277 DI 10.1088/0026-1394/30/4/011 PG 3 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA MN836 UT WOS:A1993MN83600012 ER PT J AU SMITH, PL SANDEL, BR HOLBERG, JB AF SMITH, PL SANDEL, BR HOLBERG, JB TI USING THE VOYAGER SPACECRAFT FOR SOLAR EUV SPECTRAL RADIOMETRY SO METROLOGIA LA English DT Article ID UPPER-ATMOSPHERE; FLUX; MODEL; PHOTOELECTRON; OCCULTATIONS; IRRADIANCE; ENCOUNTER; AIRGLOW; MISSION AB The ultraviolet spectrometers on the Voyager spacecraft are radiometrically stable and presently capable of making long-term, precise measurements of the solar spectral irradiance between 50 nm and 170 nm. If the detection efficiencies of these spectrometers were confirmed through a dedicated program of underflights, and if a campaign of regular Voyager observations of the Sun was instituted, some of the needs for timely, long-term solar EUV flux data could be efficiently met in this decade. C1 UNIV ARIZONA,LUNAR & PLANETARY LAB,TUCSON,AZ 85721. RP SMITH, PL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 47 TC 1 Z9 1 U1 1 U2 1 PU BUREAU INT POIDS MESURES PI SEVRES CEDEX PA B1 PM PAVILLION DE BRETUEIL, F-92312 SEVRES CEDEX, FRANCE SN 0026-1394 J9 METROLOGIA JI Metrologia PD OCT PY 1993 VL 30 IS 4 BP 397 EP 401 DI 10.1088/0026-1394/30/4/035 PG 5 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA MN836 UT WOS:A1993MN83600036 ER PT J AU PHILLIPS, WC LI, YL STANTON, M XIE, JH OMARA, D KALATA, K AF PHILLIPS, WC LI, YL STANTON, M XIE, JH OMARA, D KALATA, K TI A CCD-BASED AREA DETECTOR FOR X-RAY CRYSTALLOGRAPHY USING SYNCHROTRON AND LABORATORY SOURCES SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT LA English DT Article ID DATA-COLLECTION SYSTEM; IMAGING PLATE; PROTEIN CRYSTALLOGRAPHY; QUANTUM EFFICIENCY; DIFFRACTION DATA; DIFFRACTOMETER; PERFORMANCE; CRYSTALS; DESIGN AB The design and characteristics of a CCD-based area detector suitable for X-ray crystallographic studies using both synchrotron and laboratory sources are described. The active area is 75 mm in diameter, the FWHM of the point response function is 0.20 mm, and for Bragg peaks the dynamic range is 900 and the DQE approximately 0.3. The 1320x1035-pixel Kodak CCD is read out into an 8 Mbyte memory system in 0.14 s and digitized to 12 bits. X-ray crystallographic data collected at the NSLS synchrotron from cubic insulin crystals are presented. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP PHILLIPS, WC (reprint author), BRANDEIS UNIV,ROSENSTIEL BASIC MED SCI RES CTR,WALTHAM,MA 02254, USA. NR 23 TC 16 Z9 16 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-9002 J9 NUCL INSTRUM METH A JI Nucl. Instrum. Methods Phys. Res. Sect. A-Accel. Spectrom. Dect. Assoc. Equip. PD OCT 1 PY 1993 VL 334 IS 2-3 BP 621 EP 630 DI 10.1016/0168-9002(93)90830-B PG 10 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Nuclear; Physics, Particles & Fields SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA LV786 UT WOS:A1993LV78600049 ER PT J AU WOLDA, H DENNIS, B AF WOLDA, H DENNIS, B TI DENSITY-DEPENDENCE TESTS, ARE THEY SO OECOLOGIA LA English DT Article DE DENSITY DEPENDENCE TESTS; TIME SERIES; INSECTS; BIRDS; REGULATION OF NUMBERS ID ANIMAL NUMBERS; ANNUAL CENSUSES; STABILIZATION; FLUCTUATIONS; STRATEGIES; TREES; POWER; WOOD; SIZE AB A large number of time series of abundances of insects and birds from a variety of data sets were submitted to a new density dependence test. The results varied enormously between data sets, but the relation between the frequency of statistically significant density dependence (SSDD) and the length of the series was similar to that of the power curve of the test, making the results consistent with the hypothesis of the density-dependent model being universally applicable throughout the data used. Pest and non-pest species did not-differ in the incidence of SSDD. The more sampling error present in the data, the higher the percentages of SSDD. This was expected given that the power of the test increases with increasing sampling error in the data. Many of the data used here, as well as in the literature, clearly violate the basic assumption of the test that the organism concerned should be univoltine and semelparous. Yet the incidence of SSDD was the same in univoltine as in bi/polyvoltine species and the same in semelparous organisms as in birds that are reproductively active in more than one year. The seasonal migrant Autographa gamma in Britain and Czechoslovakia and even rainfall data were found to have SSDD. Statistical significance, however, does not automatically lead to the conclusion of density-dependent regulation. Any series of random variables which are in a stochastic equilibrium, such as a series of independent, identically distributed, random variables, is typically described better by the alternative (density-dependent) model than by the null (density-independent) model. Significant test results were often obtained with sloppy data, with data that clearly violate the basic assumptions of the test and with other data where an interpretation of the results in terms of density-dependent regulation was absurd. Given the fact that other explanations have to be found for significant test results for all these cases, mechanisms other than regulation may very well be applicable too where the data are entirely appropriate for the test. The test is simply a data-based choice between a model without and one with a stochastic equilibrium. A time series as such does not contain any information about the causes of the fluctuation pattern, so that one cannot expect statistics to produce such information from that time series. A significant test result using suitable data is entirely consistent with the hypothesis of density-dependent regulation, but also with any other suitable hypotheses. Because the test results were generally consistent with the hypothesis of a universal applicability of the density-dependence model, a negative test result may only mean that the time series was not long enough for the density dependence that was present to become statistically significant. Positive results are difficult to interpret, but so are negative results. A final decision needs to be based not so much on the test result as on much detailed information about the population concerned. Because the ''density-dependence test'' does not test for the presence of the mechanism of density-dependent regulation and because of the loaded, multiple meanings of the term ''density-dependence'', calling the test a ''test of statistical density dependence'' may be preferable. C1 UNIV IDAHO,DEPT FISH & WILDLIFE RESOURCES,MOSCOW,ID 83843. RP WOLDA, H (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO AA 34002-0948,ALBROOK AFS,PANAMA. NR 49 TC 80 Z9 81 U1 2 U2 16 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD OCT PY 1993 VL 95 IS 4 BP 581 EP 591 PG 11 WC Ecology SC Environmental Sciences & Ecology GA MB236 UT WOS:A1993MB23600018 PM 28313300 ER PT J AU JORGE, LF ARIAS, TD GRIESE, U NEBERT, DW EICHELBAUM, M AF JORGE, LF ARIAS, TD GRIESE, U NEBERT, DW EICHELBAUM, M TI EVOLUTIONARY PHARMACOGENETICS OF CYP2D6 IN NGAWBE-GUAYMI OF PANAMA - ALLELE-SPECIFIC PCR DETECTION OF THE CYP2D6B ALLELE AND RFLP ANALYSIS SO PHARMACOGENETICS LA English DT Article ID COMMON GENETIC-DEFECT; SPARTEINE OXIDATION; MITOCHONDRIAL-DNA; DEBRISOQUINE; POLYMORPHISM; METABOLISM; MUTATIONS; AMERINDIANS; LOCUS AB Gene cluster CYP2D controls the biosynthesis of enzyme CYP2D6, which is responsbile for the polymorphic oxidation of sparteine, debrisoquine and related drugs. This cluster consists of the functional gene D6 and of two pseudogenes, D7 and D8. RFLP Bam HI analysis of CYP2D in 37 unrelated and eight related Ngawbe Guaymi Amerindians of Panama showed a polymorphism characterized by the presence of two alleles: 4.7 + 7.9 and 2.3 + 6.0 (frequencies: 0.63 and 0.37, respectively, n = 35 unrelated subjects). The possible genotypes for these alleles follow the Hardy-Weinberg distribution (chi2 = 1.76; 0.10 < p < 0.25). All PMs of sparteine or debrisoquine (n = 7) were homozygotes for the second allele, but not all homozygotes (n = 10) were PMs, so there was not an exclusive association between the Bam HI genotype and the observed phenotype. A similar analysis with the endonuclease Xba I proved to be non-informative in relation to phenotype, since all subjects (n = 40) showed only the 29 kb allele. Allele-specific PCR studies of selected subjects indicated the existence of the CYP2D6B allele (freq = 0.17; C.I.95% = 0.085, 0.29: n = 30 unrelated subjects), in addition to the wild-type. The mutant CYP2D6B allele was responsible for the enzyme deficiency present in PMs. Its presence in Amerindians suggests that this allele has a far more ancient evolutionary history than previously thought. The over-all RFLP and PCR analyses point to a diminished genetic diversity for the Ngawbe subjects, consistent with their demographic history and population genetics. C1 DR MARGARETE FISCHER BOSCH INST CLIN PHARMACOL,PHARMAKOL KLIN,STUTTGART,GERMANY. SMITHSONIAN TROP RES INST,PANAMA CITY,PANAMA. UNIV PANAMA,COLL PHARM,PANAMA CITY,PANAMA. UNIV PANAMA,WHO,CTR DRUG QUAL CONTROL,PANAMA CITY,PANAMA. UNIV CINCINNATI,MED CTR,CTR ENVIRONM GENET,CINCINNATI,OH 45267. FU NIEHS NIH HHS [P30 ES06096] NR 31 TC 11 Z9 12 U1 0 U2 0 PU CHAPMAN HALL LTD PI LONDON PA 2-6 BOUNDARY ROW, LONDON, ENGLAND SE1 8HN SN 0960-314X J9 PHARMACOGENETICS JI Pharmacogenetics PD OCT PY 1993 VL 3 IS 5 BP 231 EP 238 DI 10.1097/00008571-199310000-00002 PG 8 WC Biotechnology & Applied Microbiology; Genetics & Heredity; Pharmacology & Pharmacy SC Biotechnology & Applied Microbiology; Genetics & Heredity; Pharmacology & Pharmacy GA MG989 UT WOS:A1993MG98900002 PM 7904509 ER PT J AU BOYLE, JJ AF BOYLE, JJ TI SINGLE-PARTICLE POTENTIAL FOR PHOTOEXCITED ELECTRON ORBITALS OF OPEN-SHELL ATOMS SO PHYSICAL REVIEW A LA English DT Article ID PHOTOIONIZATION CROSS-SECTION; RESONANCE STRUCTURE AB A single-particle potential for the calculation of photoexcited electron orbitals is introduced. This potential is defined to include exactly all of the first-order electron correlations that appear in the diagrammatic perturbation series of the dipole polarizability and that contain potential corrections in the intermediate state. The angular coefficients that are associated with this potential can be written in the form of an average term plus a correction to the average. It is demonstrated that the correction to the average contribution is dependent only upon the initial-state coupling of the atom. Additionally, a trivial relationship exists between the correction to the average contributions for conjugate initial-state configurations. The angular coefficients are tabulated for all of the s(n), p(n), and d(n) initial-state LS couplings that are possible. Supplementary analytic relationships are also presented. RP BOYLE, JJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Boyle, James/N-6634-2016 OI Boyle, James/0000-0003-0804-3390 NR 22 TC 4 Z9 4 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD OCT PY 1993 VL 48 IS 4 BP 2860 EP 2873 DI 10.1103/PhysRevA.48.2860 PG 14 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA MC717 UT WOS:A1993MC71700039 ER PT J AU ESSER, R HABBAL, SR AF ESSER, R HABBAL, SR TI OVERESTIMATING THE CORONAL DENSITY AND ITS EFFECT ON THE VELOCITIES DERIVED FROM L-ALPHA DOPPLER DIMMING SO SOLAR PHYSICS LA English DT Article ID SOLAR-WIND; ALFVEN WAVES; POLAR-REGION; ENERGY-FLOW; MODEL; HOLE; SUN AB It is shown that relatively small errors of the order of 10% in the electron densities, for example derived from polarization brightness measurements, might lead to large errors in the velocities inferred from intensity measurements of the Lalpha H I lambda 1216 spectral line in the inner corona. It is demonstrated that in some cases this effect can result in very high velocities close to the coronal base with subsequent small acceleration with heliocentric distance. It is also pointed out that the errors in the deduced velocities can be reduced if simultaneous observations that place constraints on the mass flux are available, and by ensuring that the mass flux computed from the derived velocities and densities is constant. RP ESSER, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 28 TC 3 Z9 3 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD OCT PY 1993 VL 147 IS 2 BP 241 EP 254 DI 10.1007/BF00690715 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LZ067 UT WOS:A1993LZ06700003 ER PT J AU ABUASAB, MS CANTINO, PD AF ABUASAB, MS CANTINO, PD TI SYSTEMATIC IMPLICATIONS OF POLLEN MORPHOLOGY IN TRIBE PROSTANTHEREAE (LABIATAE) SO SYSTEMATIC BOTANY LA English DT Article AB A palynological survey of Tribe Prostanthereae (Labiatae) reveals that the pollen is tricolpate or 6- (8) colpate, tectate-perforate to reticulate, with or without spinulose sculpturing; the columellae are simple and the colpal membranes bear sexine elements. Three sculpturing variants are distinguishable. None of the pollen types in the Prostanthereae have been observed elsewhere in the Labiatae s. str., but the one hypothesized to be ancestral in the tribe (tricolpate, microreticulate, lacking spinules) is widespread in the Labiatae s.l. (i.e., including many genera traditionally assigned to Verbenaceae). The two sections of Prostanthera differ in pollen size and number of colpi, providing a probable synapomorphy for sect. Klanderia (6-colpate pollen) and phenetic support for its segregation as a distinct genus (Cryphia). Conn's placement of Eichlerago in synonymy with Prostanthera is supported by their similar pollen morphology. The distribution of spinulose sculpturing (a derived state) suggests that Prostanthera, Wrixonia, and perhaps Hemiandra form a clade within the tribe, but the inclusion of Hemiandra conflicts with floral characters. The hypothesis that tribe Prostanthereae is closely related to subfam. Chloanthoideae sensu Briquet (the latter variably assigned to Verbenaceae s.l., Labiatae s.l., or its own family) is more consistent with pollen morphology than the traditional placement of the tribe within the Labiatae s. str. C1 OHIO UNIV,DEPT ENVIRONM & PLANT BIOL,ATHENS,OH 45701. SMITHSONIAN INST,DEPT ENTOMOL,WASHINGTON,DC 20560. NR 33 TC 8 Z9 9 U1 1 U2 4 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 1993 VL 18 IS 4 BP 563 EP 574 DI 10.2307/2419534 PG 12 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA ME155 UT WOS:A1993ME15500003 ER PT J AU GILLESPIE, LJ AF GILLESPIE, LJ TI A SYNOPSIS OF NEOTROPICAL PLUKENETIA (EUPHORBIACEAE) INCLUDING 2 NEW SPECIES SO SYSTEMATIC BOTANY LA English DT Article AB A synopsis of the eleven neotropical species of Plukenetia (Euphorbiaceae) is given. The genus Plukenetia is redefined to include the neotropical monotypic genera Eleutherostigma and Vigin (previously known as Fragariopsis). As treated here Plukenetia may be distinguished from all other members of the tribe Plukenetieae by its four-carpellate ovary. Two new species, P. supraglandulosa from French Guiana and the Brazilian state of Amapa and P. stipellata from Mexico and Central America, are described and illustrated. Plukenetia supraglandulosa is closely allied with P. penninervia and P. multiglandulosa and differs in the presence of scattered laminar glands on the upper leaf surface and longer inflorescences. The three species share a very similar androecium of dimorphic stamens, which is correctly described for the first time. Plukenetia stipellata differs from the closely related South American and West Indian species, P. volubilis, by its stipellate leaf blade base, shorter styles and longer slender stamens. Two new combinations, P. serrata and P. lehmanniana, are proposed. A key to the 11 species in the Neotropics is provided. RP GILLESPIE, LJ (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT NHB 166,WASHINGTON,DC 20560, USA. NR 16 TC 17 Z9 19 U1 1 U2 13 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD OCT-DEC PY 1993 VL 18 IS 4 BP 575 EP 592 PG 18 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA ME155 UT WOS:A1993ME15500004 ER PT J AU JOHNSTON, LA DONOGHUE, AM OBRIEN, SJ WILDT, DE AF JOHNSTON, LA DONOGHUE, AM OBRIEN, SJ WILDT, DE TI INFLUENCE OF CULTURE-MEDIUM AND PROTEIN SUPPLEMENTATION ON IN-VITRO OOCYTE MATURATION AND FERTILIZATION IN THE DOMESTIC CAT SO THERIOGENOLOGY LA English DT Article DE CAT; OOCYTE MATURATION; FERTILIZATION; EMBRYO ID FOLLICULAR OOCYTES; DEVELOPMENTAL COMPETENCE; MATURED INVITRO; CAPACITY; EMBRYOS AB Domestic cat oocytes were cultured either in Waymouth MB 753/1 Medium (WAY) or in Eagle's Minimum Essential Medium (MEM) containing FSH, LH and estradiol-17beta and supplemented with one of the following: 5% fetal calf serum (FCS); 4 mg/ml bovine serum albumin (BSA); or 3 mg/ml polyvinylalcohol (PVA, a non-protein control). The oocytes were evaluated for: nuclear maturation after 48 hours of culture (in vitro maturation, IVM); fertilization and cleavage 24 to 30 hours postinsemination (in vitro fertilization, IVF); and early embryo development 48 hours postinsemination. Maturation rates were similar (P>0.05) for WAY + BSA (29.4%), MEM + BSA (46.7%) and MEM + PVA (43.3%), but were different (P<0.05) from the other treatments (range, WAY + FCS, 9.6% to WAY + PVA, 14.9%). Fertilization and cleavage rates were also similar (P>0.05) for WAY + BSA (51.4%, 30.5%), MEM + BSA (45.8%, 40.1%) and MEM + PVA (56.1%, 37.4%) and were greater (P<0.05) than all other treatments. These IVM/IVF oocytes were capable of culturing beyond 2-cells, with the highest proportion of 4- and 8- cell embryos forming in WAY and MEM media in the presence of BSA or in MEM medium containing PVA. In the domestic cat IVM/IVF system: both the type of culture medium and protein supplement influence the proportion of oocytes reaching Metaphase II; the type of protein supplement has a more significant (P<0.05) impact than medium on fertilization, cleavage and early embryo development; and nuclear maturation and fertilization in vitro can proceed in this species in the absence of supplementary protein. C1 HENRY DOORLY ZOO,OMAHA,NE 68107. NCI,FREDERICK CANC RES & DEV CTR,VIRAL CARCINOGENESIS LAB,FREDERICK,MD 21701. RP JOHNSTON, LA (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 27 TC 22 Z9 22 U1 3 U2 6 PU BUTTERWORTH-HEINEMANN PI WOBURN PA 225 WILDWOOD AVE #UNITB PO BOX 4500, WOBURN, MA 01801-2084 SN 0093-691X J9 THERIOGENOLOGY JI Theriogenology PD OCT PY 1993 VL 40 IS 4 BP 829 EP 839 DI 10.1016/0093-691X(93)90218-T PG 11 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA LZ874 UT WOS:A1993LZ87400017 PM 16727364 ER PT J AU WOLDA, H AF WOLDA, H TI DIEL AND SEASONAL PATTERNS OF MATING CALLS IN SOME NEOTROPICAL CICADAS - ACOUSTIC INTERFERENCE SO PROCEEDINGS OF THE KONINKLIJKE NEDERLANDSE AKADEMIE VAN WETENSCHAPPEN-BIOLOGICAL CHEMICAL GEOLOGICAL PHYSICAL AND MEDICAL SCIENCES LA English DT Article ID NINO SOUTHERN OSCILLATION; 1982-1983 EL-NINO; BAT PREDATION; EQUATORIAL PACIFIC; INSECTS; SONG; PHONOTAXIS; GALAPAGOS; EVOLUTION; HOMOPTERA AB In Las Cumbres, Republic of Panama, the dusk chorus of three cicadas, Quesada gigas, Fidicina pronoe and F. mannifera was documented. Seasonal changes and the relation of their choruses to the timing of sunset were described. Temporal overlap between the choruses of Q. gigas and F. pronoe was maximal, presumably as an anti-predator defense. However, this overlap was obviously no impediment to the continuing flourishing of both populations. Overlap of these species with F. mannifera was minimal. Differences between Las Cumbres and Barro Colorado Island (BCI) in the seasonal pattern of the cicada Pacarina puella might be attributed to acoustic interference by Selymbria ahyetios on BCI. Dorisiana sp. nr. cachla became suddenly extinct in Las Cumbres between 1982 and 1983, possibly, but if so obscurely, related to El Nino. RP WOLDA, H (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO AA,MIAMI,FL 34002, USA. NR 56 TC 8 Z9 10 U1 1 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0023-3374 J9 P K NED AKAD WETENSC JI Proc. K. Ned. Akad. Wet.-Biol. Chem. Geol. Phys. Med. Sci. PD SEP 27 PY 1993 VL 96 IS 3 BP 369 EP 381 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA MC249 UT WOS:A1993MC24900008 ER PT J AU WATTERS, TR AF WATTERS, TR TI COMPRESSIONAL TECTONISM ON MARS SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID THARSIS REGION; LITHOSPHERIC STRESS; TERRESTRIAL PLANETS; WRINKLE RIDGES; ORIGIN; SERENITATIS; HIGHLANDS; EVOLUTION; THICKNESS; PROVINCE AB Contractional features on Mars were identified on the basis of photogeologic evidence of crustal shortening and comparison with terrestrial and planetary analogs. Three classes of structures, wrinkle ridges, lobate scarps and high-relief ridges, were mapped and their spatial and temporal distribution assessed. Wrinkle ridges account for over 80% of the total cumulative length of the mapped contractional features and occur in smooth plains material interpreted to be volcanic in origin. Lobate scarps, not wrinkle ridges, are the dominant contractional feature in Martian highland material. The pattern of contractional features in the western hemisphere reflects the hemispheric-scale influence of the Tharsis rise. Although no comparable hemispheric-scale pattern is observed in die eastern hemisphere, prominent regional-scale patterns exist, the most notable of which occurs in Hesperia Planum. Contractional features that locally parallel the trend of the crustal dichotomy boundary in the eastern hemisphere suggest the influence of stresses related to the evolution of die dichotomy. Compressional deformation apparently peaked during the Early Hesperia, if the tectonic features are roughly the same age as the units in which they occur. This peak in compressional deformation corresponds with Early Hesperian volcanic resurfacing of a large portion of the planet. Thermal history models for Mars, based on an initially hot planet, are inconsistent with estimates of die timing of peak compressional tectonism and the rate of volcanism. A pulse of global volcanism during the Early Hesperian may have resulted in a punctuated episode of rapid cooling and global contraction that contributed to compressional tectonism. Although global contraction may have contributed a significant component of die total stress that resulted in compressional deformation on Mars, nonhydrostatic horizontal stresses derived from local and regional-scale sources are necessary to account for the uniform orientations of die tectonic features. RP WATTERS, TR (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,CTR EARTH & PLANETARY STUDIES,WASHINGTON,DC 20560, USA. NR 67 TC 96 Z9 97 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP 25 PY 1993 VL 98 IS E9 BP 17049 EP 17060 DI 10.1029/93JE01138 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA MA452 UT WOS:A1993MA45200003 ER PT J AU FICH, M HODGE, P AF FICH, M HODGE, P TI MILLIMETER AND SUBMILLIMETER CONTINUUM EMISSION FROM EARLY-TYPE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE DUST, EXTINCTION; GALAXIES, ELLIPTIC AND LENTICULAR, CD; GALAXIES, ISM; INFRARED, GALAXIES; RADIO CONTINUUM, GALAXIES ID NEUTRAL-HYDROGEN CONTENT; H-I-OBSERVATIONS; INTERSTELLAR MATTER; ELLIPTICAL GALAXIES; STATISTICAL DISTRIBUTION; MOLECULAR GAS; SA-GALAXIES; NGC-205; CATALOG; CO AB Twenty-two early-type galaxies that were detected by IRAS have been searched for continuum emission at millimeter and submillimeter wavelengths using the James Clerk Maxwell Telescope (JCMT). IRAS was relatively insensitive to cold dust that emits primarily at these longer wavelengths. In this first survey we were able to detect or achieve useful limits on the emission from 14 of the 22 galaxies observed. From these data we estimate upper limits on the dust temperature and lower limits on the mass of dust within the JCMT beam. These results are compared with H I and CO data and with the blue luminosities of the galaxies. The results are consistent with a model where the dust-to-gas ratio is similar to the Galactic one, and the amount of cold dust is an order of magnitude greater than the amount of warm dust (as is also seen in our Galaxy). The total dust mass, normalized to the luminosity of the entire galaxy, is much lower than is found in spiral galaxies, as expected. C1 UNIV WATERLOO,GUELPH WATERLOO PROGRAM GRAD WORK PHYS,WATERLOO N2L 3G1,ONTARIO,CANADA. UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98195. RP FICH, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 27 TC 25 Z9 25 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1993 VL 415 IS 1 BP 75 EP 81 DI 10.1086/173144 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LW899 UT WOS:A1993LW89900008 ER PT J AU FIORE, F ELVIS, M MATHUR, S WILKES, BJ MCDOWELL, JC AF FIORE, F ELVIS, M MATHUR, S WILKES, BJ MCDOWELL, JC TI THE ROSAT SPECTRUM OF 3C-351 - A WARM ABSORBER IN AN X-RAY-QUIET QUASAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE QUASARS, INDIVIDUAL (3C-351); X-RAYS, GALAXIES ID ACTIVE GALACTIC NUCLEI; CROSS-SECTIONS; SEYFERT-GALAXIES; ABSORPTION; GINGA; HOT AB 3C 351 is one of the most X-ray-quiet radio quasars (alpha(OX) approximately 1.6). We have observed 3C 351 with the ROSAT position sensitive proportional counter (PSPC) and find a complex X-ray spectrum which is not well reproduced by a power law plus low-energy cutoff model. Soft excess, partial covering, and ''warm absorber'' models can all produce acceptable fits, although only the warm absorber model gives typical values for the high-energy continuum slope. The alpha(OX) measured by using quasi-simultaneous ROSAT, MMT, and HST observations is in the range 1.5-1.6, significantly above the average of 1.37 (sigma approximately 0.15) for a complete sample of 33 3CR quasars. If the soft excess or partial covering models are correct, 3C 351 appears X-ray-quiet in the PSPC band because it has an extremely steep or flat intrinsic high-energy spectral slope. However, if the warm absorber model is correct, the quasar is intrinsically X-ray-quiet; the normalization of the intrinsic (unabsorbed) X-ray emission is unusually low relative to the optical luminosity. We investigate the properties of our warm absorber model in some detail. The apparently complicated behavior of the fit parameters may be understood by considering the effects of changing absorbing column and ionization parameter on intrinsic power-law spectra of different slopes. RP FIORE, F (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Wilkes, Belinda/0000-0003-1809-2364; Fiore, Fabrizio/0000-0002-4031-4157 NR 48 TC 61 Z9 61 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1993 VL 415 IS 1 BP 129 EP 139 DI 10.1086/173150 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LW899 UT WOS:A1993LW89900014 ER PT J AU CURIEL, S RODRIGUEZ, LF MORAN, JM CANTO, J AF CURIEL, S RODRIGUEZ, LF MORAN, JM CANTO, J TI THE TRIPLE RADIO-CONTINUUM SOURCE IN SERPENS - THE BIRTH OF A HERBIG-HARO SYSTEM SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, JETS AND OUTFLOWS; RADIO CONTINUUM, INTERSTELLAR; STARS, FORMATION; STARS, PRE-MAIN-SEQUENCE ID LARGE PROPER MOTIONS; L1551 IRS-5; EMISSION; OBJECTS; BULLETS; IMAGES; KNOTS; FLOWS; JETS AB VLA observations of the triple radio continuum source in Serpens have revealed its extraordinary characteristics. While it is associated with a star-forming region, its outer components exhibit nonthermal spectra and large proper motions. Here, we present the results of high-sensitivity, multifrequency VLA radio continuum observations of this source. These observations show that (a) the radio source consists of a central component, and two lobes with enhanced brightness at their ends; (b) there is knotty and extended emission connecting the central source with the outer NW component which we identify as a radio jet; (c) the central source exhibits an almost flat spectrum with a spectral index alpha = 0.15 +/- 0.09, the NW component also has a flat spectrum with an index alpha = -0.05 +/- 0.05 (characteristic of optically thin thermal emission), and the SE component has a negative index alpha = -0.30 +/- 0.04 (consistent with nonthermal synchrotron emission); (d) the outer sources break into a number of components (which we identify as ''internal working surfaces'' or ''bullets'') with similar tangential velocities and directions; and (e) the central source has an elongated morphology, with its major axis nearly parallel to the outflow direction but having a significantly different direction, which suggests that the central source may be precessing or nutating. These observations confirm the unusually large proper motions of about 0.12'' yr-1, previously measured for the outer NW and SE components. Moreover, similar proper motions have been obtained for a time-variable knot in the NW radio jet, suggesting that probably all the knots in the body of the jet have velocities similar to those of the outer components. The spectral indices of the main three components differ from those obtained previously. We suggest that the brightness variability of the outer sources, as well as the change in their spectral indices, could be the result of the passage of locally enhanced condensations through the bow shock produced by the ejected bullets. We find that if the NW and SE clumps are moving through a medium with density of n0 approximately 10(5) cm-3, then the thermal free-free emission produced by the shock waves around these objects can account for the observed emission. However, a nonthermal particle acceleration mechanism is required to account for the negative spectral indices. We identify the triple radio continuum source in Serpens as a young radio jet, with a dynamical age of only approximately 60 yr, emanating from the central component. This radio jet exhibits a one-sided morphology that is very similar to that observed in optical Herbig-Haro jets, suggesting that jets associated with young stellar objects are intrinsically unipolar within the dynamical ages of the main jets and not an extinction effect. We believe that the knotty structure in the NW radio jet and the SE components are the result of discrete ejection of material (or ''bullets'') from the central source. Finally, based on the morphological and kinematical similarities between this radio jet and optical Herbig-Haro jets, and their different length scales and dynamical ages, we propose that the Serpens radio jet could be a proto-Herbig-Haro system, in an early stage of evolution. C1 Univ Nacl Autonoma Mexico, INST ASTRON, MEXICO CITY 04510, DF, MEXICO. RP CURIEL, S (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, MAIL STOP 42, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 31 TC 100 Z9 100 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1993 VL 415 IS 1 BP 191 EP 203 DI 10.1086/173155 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LW899 UT WOS:A1993LW89900019 ER PT J AU GUDEL, M SCHMITT, JHMM BOOKBINDER, JA FLEMING, TA AF GUDEL, M SCHMITT, JHMM BOOKBINDER, JA FLEMING, TA TI A TIGHT CORRELATION BETWEEN RADIO AND X-RAY LUMINOSITIES OF M-DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE RADIO CONTINUUM, STARS; STARS, LATE-TYPE; X-RAYS, STARS ID ACTIVE BINARY-SYSTEMS; RS-CANUM-VENATICORUM; FLARE STARS; VLA SURVEY; EMISSION; CONTINUUM AB We present results of a survey of nonflare radio and X-ray properties of dM/dMe stars. This survey was obtained during the ROSAT All-Sky Survey and is accompanied by mostly simultaneous VLA observations. We find that the X-ray and radio luminosities are correlated over three orders of magnitude, L(R) is-proportional-to L(X), irrespective of spectral type. This result improves if strictly simultaneous observations are considered. This correlation points to a physical relation between the particle populations responsible for the two emissions. C1 NATL INST STAND & TECHNOL,BOULDER,CO 80309. MAX PLANCK INST EXTRATERR PHYS,W-8046 GARCHING,GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP GUDEL, M (reprint author), UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309, USA. RI Guedel, Manuel/C-8486-2015 OI Guedel, Manuel/0000-0001-9818-0588 NR 22 TC 43 Z9 43 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1993 VL 415 IS 1 BP 236 EP 239 DI 10.1086/173158 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LW899 UT WOS:A1993LW89900022 ER PT J AU CALAMAI, AG SMITH, PL BERGESON, SD AF CALAMAI, AG SMITH, PL BERGESON, SD TI TRANSITION-PROBABILITIES FOR THE 3S(2)3P(P-2(0))-3S3P(2)(P-4) INTERSYSTEM LINES OF SI-II SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC DATA ID SPECTRUM AB Intensity ratios of lines of the spin-changing ''intersystem'' multiplet of Si II (4P --> 2P(o)) at 234 nm have been used to determine electron densities and temperatures in a variety of astrophysical environments. However, the accuracy of these diagnostic calculations have been limited by uncertainties associated with the available atomic data. We report the first laboratory measurement, using an ion-trapping technique, of the radiative lifetimes of the three metastable levels of the 3s3p2 4P term of Si II. Our results are 104 +/- 16, 406 +/- 33, and 811 +/- 77 mus for lifetimes of the J = 1/2, 5/2, and 3/2 levels, respectively. A-values were derived from our life-times by use of measured branching fractions. Our A-values, which differ from calculated values by 30% or more, should give better agreement between modeled and observed Si II line ratios. C1 UNIV WISCONSIN,DEPT PHYS,MADISON,WI 53706. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP CALAMAI, AG (reprint author), PHILADELPHIA COLL PHARM & SCI,DEPT MATH & PHYS,600 S 43RD ST,PHILADELPHIA,PA 19104, USA. RI Bergeson, Scott/L-8959-2013 OI Bergeson, Scott/0000-0002-3124-9226 NR 16 TC 25 Z9 25 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 1993 VL 415 IS 1 BP L59 EP L62 DI 10.1086/187032 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LW901 UT WOS:A1993LW90100015 ER PT J AU RICE, ME AF RICE, ME TI 2 NEW SPECIES OF PHASCOLION (SIPUNCULA, PHASCOLIONIDAE) FROM TROPICAL AND SUBTROPICAL WATERS OF THE CENTRAL-WESTERN ATLANTIC SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Phascolion (Isomya) gerardi, a new species of Sipuncula, is described from littoral waters of the Bahamas, Belize, and the Yucatan coast of Mexico where it inhabits rubble associated with coral reefs. A new interstitial species, Phascolion (Phascolion) psammophilum, is described from depths of 15-19 m off the coast of east central Florida. It is the first sipunculan, documented as an adult rather than juvenile, to be reported as a member of the meiofaunal community. Observations on development, resulting from laboratory spawnings, reveal a typical lecithotrophic trochophore and a short-lived lecithotrophic pelagosphera larva that transforms into a crawling juvenile at 4 days of age. Station data for these collections are presented in an appendix at the end of the paper. RP RICE, ME (reprint author), SMITHSONIAN MARINE STN LINK PORT,5612 OLD DIXIE HIGHWAY,FT PIERCE,FL 34946, USA. NR 14 TC 3 Z9 5 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD SEP 20 PY 1993 VL 106 IS 3 BP 591 EP 601 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA LY971 UT WOS:A1993LY97100019 ER PT J AU GARGAUD, M BACCHUSMONTABONEL, MC MCCARROLL, R AF GARGAUD, M BACCHUSMONTABONEL, MC MCCARROLL, R TI CHARGE-TRANSFER OF O2+ IN HELIUM AT THERMAL AND LOW ELECTRON-VOLT ENERGIES SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CROSS-SECTIONS; COLLISIONS; CAPTURE; IONS; HE; O-2+; H2; H+ AB Cross sections and rate coefficients in the thermal-eV energy range are calculated for the charge transfer reaction of O2+(3p) ions with helium. In agreement with earlier predictions, it is confirmed that the reaction populates preferentially the metastable (2P) state of the O+ ion. The computed cross sections are, however, considerably larger than previous experimental and theoretical estimations. A discussion is given of the reasons for this discrepancy. C1 UNIV LYON 1, SPECTROMETRIE ION & MOLEC LAB, CNRS, URA 171, F-69622 VILLEURBANNE, FRANCE. UNIV PARIS 06, DYNAM MOLEC & ATOM LAB, CNRS, URA 774, F-75252 PARIS 05, FRANCE. HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, CAMBRIDGE, MA 02138 USA. RP GARGAUD, M (reprint author), UNIV BORDEAUX 1 OBSERV, CNRS, URA 352, F-33270 FLOIRAC, FRANCE. RI bacchus, marie christine/F-4020-2010 OI bacchus, marie christine/0000-0002-0958-2380 NR 15 TC 27 Z9 27 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD SEP 15 PY 1993 VL 99 IS 6 BP 4495 EP 4499 DI 10.1063/1.466048 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA LX143 UT WOS:A1993LX14300023 ER PT J AU KUNC, JA AF KUNC, JA TI ANALYTICAL DEPENDENCE OF THE VISCOSITY CROSS-SECTIONS AND VISCOSITY COEFFICIENTS ON PARAMETERS OF INTERMOLECULAR POTENTIALS SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SCATTERING; MOLECULES; GASES AB General analytical expressions for viscosity cross sections and viscosity coefficients of gases as functions of the parameters of intermolecular potentials are derived from the first principle using the classical scattering theory. Two types (one repulsive-attractive and one purely repulsive) of the central-force potentials, suitable to represent molecule-molecule, atom-molecule and atom-atom interactions, are considered. The expressions for viscosity show good agreement with results of numerical calculations in high-temperature single-component gases (above 2000 K) where viscosity measurements are not available. C1 HARVARD UNIV,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 19 TC 6 Z9 6 U1 0 U2 2 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD SEP 15 PY 1993 VL 99 IS 6 BP 4705 EP 4717 DI 10.1063/1.466068 PG 13 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA LX143 UT WOS:A1993LX14300044 ER PT J AU CLAYTON, GC LAWSON, WA WHITNEY, BA POLLACCO, DL AF CLAYTON, GC LAWSON, WA WHITNEY, BA POLLACCO, DL TI HIGH-VELOCITY SPECTRAL FEATURES IN V854 CENTAURI - EVIDENCE FOR DUST FORMATION SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Letter DE CIRCUMSTELLAR MATTER; STARS INDIVIDUAL V854 CEN; STARS MASS-LOSS; STARS VARIABLES OTHER; DUST, EXTINCTION; ULTRAVIOLET STARS ID R-CORONAE-BOREALIS; MINIMUM LIGHT; STAR; DECLINE; NSV-6708 AB Low-dispersion IUE spectra of V854 Cen show apparent shifts or splitting in the lambda2325 C II], lambda2800 Mg II, A2851 Mg I and LAMBDA2965 C I lines which, if kinematic, indicate velocities in excess of 1000 km s-1. The variations are seen in all the UV emission lines simultaneously. The line splitting seems to occur at times near phase 0.0 (maximum light) of the pulsation cycle of the star. Dust formation episodes in V854 Cen also occur at this phase. New high-dispersion spectra of V854 Cen of the Na I D lines show many high-velocity features, both red- and blueshifted, including one at almost - 400 km s-1. The line profile variations may be a spectral signature of the gas from which the dust is condensing. C1 UNIV COLL UNSW,AUSTRALIAN DEF FORCE ACAD,DEPT PHYS,CANBERRA,ACT 2600,AUSTRALIA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV ST ANDREWS,DEPT PHYS & ASTRON,ST ANDREWS KY16 9SS,FIFE,SCOTLAND. RP CLAYTON, GC (reprint author), UNIV COLORADO,CTR ASTROPHYS & SPACE ASTRON,CAMPUS BOX 389,BOULDER,CO 80309, USA. NR 19 TC 10 Z9 10 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP 15 PY 1993 VL 264 IS 2 BP L13 EP L16 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LX326 UT WOS:A1993LX32600002 ER PT J AU CROTHERS, DSF OROURKE, SFC AF CROTHERS, DSF OROURKE, SFC TI GENERALIZED DEMKOV MODEL - STRONG-COUPLING APPROXIMATION SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Letter ID CHARGE-TRANSFER; COLLISIONS AB A recent discussion and derivation of the strong-coupling form of the transition probability in the generalized Demkov model is shown to be incorrect. By the same token, our previous derivations of the strong-coupling forms of the transition probabilities for both the generalized Demkov and the three-parameter exponential Nikitin models are shown to be correct. The recent error is traced to an inconsistent differentiation of the amplitude (as against the phase) of the semiclassical wavefunction at the classical turning point, at which by construction the non-analytic total wavefunction is discontinuous in its second-order derivative, which follows from the cusp-like discontinuity in the first-order derivative of at least the off-diagonal Hamiltonian potential matrix elements. It is concluded that caution must be exercised when invoking comparison equations and their asymptotics and that our recent generalizations to complex energies and interactions are also correct. It is also pointed out that the hyperbolic sine component of the transition amplitude in the recent incorrect discussion does not appear in the analytic Rosen-Zener model, and would otherwise deny the existence of Stueckelberg oscillations. It is concluded also that Stueckelberg phase-integral derivations are essential if transition probabilities and total cross sections are not to be under-estimated at large impact parameters, due to a neglect of the bending of double Stokes' lines. Also consistent with our established phase-integral analysis for the non-crossing collision, we confirm the small second-order correction to the Stueckelberg frequency of oscillation, which was derived by Vitanov, and which we interpret as the argument of a Stokes' constant; we use the method of steepest descent for this derivation, avoiding the unnecessary reversion of series by Debye and Watson. C1 INST PHYS & CHEM RES,WAKO,SAITAMA 35101,JAPAN. QUEENS UNIV BELFAST,DEPT APPL MATH & THEORET PHYS,DIV THEORET & COMPUTAT PHYS RES,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. RP CROTHERS, DSF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 18 TC 8 Z9 8 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD SEP 14 PY 1993 VL 26 IS 17 BP L547 EP L553 DI 10.1088/0953-4075/26/17/004 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LY840 UT WOS:A1993LY84000004 ER PT J AU RUDY, RJ COHEN, RD ROSSANO, GS ERWIN, P PUETTER, RC GREENHOUSE, MA WOODWARD, CE AF RUDY, RJ COHEN, RD ROSSANO, GS ERWIN, P PUETTER, RC GREENHOUSE, MA WOODWARD, CE TI STRONG [FE-II] EMISSION FROM NGC-1275 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (NGC-1275); GALAXIES, ISM; GALAXIES, NUCLEI; GALAXIES, SEYFERT; INFRARED, GALAXIES; SHOCK WAVES ID ACTIVE GALACTIC NUCLEI; LINE RADIO GALAXIES; INTER-STELLAR DUST; HIGH-VELOCITY; INFRARED-SPECTROSCOPY; SUPERNOVA-REMNANTS; STAR FORMATION; COOLING FLOWS; SEYFERT-GALAXIES; ORION NEBULA AB Infrared spectroscopy of the central region of NGC 1275 has revealed an unusually strong [Fe II] lamdba12567 feature. Although the redshift of this line matches those of the lines of the active nucleus, its much narrower profile signifies its origin in a different volume of gas. The strength of the [Fe II] feature compared to the other emission lines from the central region indicates that iron remains relatively undepleted from the interstellar medium of NGC 1275. While other agents may contribute to the [Fe II] emission, we propose that the bulk of the emission is excited by wide-spread shocks. These shocks enrich the iron content of the interstellar medium, excite the extensive low-ionization regions which produce the [Fe II] flux, and contribute to the other low-excitation features which are so distinctive in the spectrum of NGC 1275. These shocks could result from supernova explosions, the accretion on intracluster material, galaxy-galaxy interactions, or some process associated with the active nucleus, but our observations do not distinguish among these phenomena. However, if supernovae generate the shocks, then a very high, and observable, supernovae rate of approximately 3 yr-1 is implied by the [Fe II] luminosity. The presence of an [Fe II] feature comparable in brightness to the nuclear Pabeta emission, but exhibiting a very different profile, makes NGC 1275 an unambiguous example of a luminous active galaxy where the [Fe II] emission does not originate in the active nucleus, and probably is not powered by the nuclear continuum source. While this observation of NGC 1275 does not exclude the active nucleus as the principal source of the strong [Fe II] emission detected in other active galaxies, it does indicate that other agents (e.g., shocks) can compete favorably in the production of the [Fe II] lines. C1 UNIV CALIF SAN DIEGO,CTR ASTROPHYS & SPACE SCI,LA JOLLA,CA 92093. SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. UNIV WYOMING,WYOMING INFRARED OBSERV,LARAMIE,WY 82071. RP RUDY, RJ (reprint author), AEROSP CORP,CTR SPACE & ENVIRONM TECHNOL,M2-266,POB 92957,LOS ANGELES,CA 90009, USA. NR 73 TC 9 Z9 9 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1993 VL 414 IS 2 BP 527 EP 534 DI 10.1086/173100 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU946 UT WOS:A1993LU94600014 ER PT J AU STANCIL, PC BABB, JF DALGARNO, A AF STANCIL, PC BABB, JF DALGARNO, A TI THE RADIATIVE ASSOCIATION OF HE+ AND HE AND H+ AND H SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (NGC-7027); MOLECULAR PROCESSES; SUPERNOVAE, INDIVIDUAL (SN-1987A) ID ADIABATIC CALCULATIONS; MOLECULAR ION; HE-2(+); STATES; 2-SIGMA-U+; SN-1987A; ENERGY AB The rate coefficient for the radiative association of He+ and He to form He-2+ is determined for temperatures T between 20 K and 500,000 K. It can be represented by the relation 1.3 x 10(-21) T-0.008 exp (- T/67) + 2.1 X 10(-24) T1.8 exp (- T/22,800) cm3 s-1 to within 25% applicable up to 50,000 K. It is about an order of magnitude less than the rate coefficient for the radiative association of H+ and H to form H-2+. Cross sections for the He-2+ and H-2+ reactions calculated using a fully quantum-mechanical method reveal weak resonance features at low energies. Implications of the He+ + He radiative association process are discussed briefly in connection with the chemistry of supernova ejecta, planetary nebulae, and the early universe. C1 OLD DOMINION UNIV,DEPT PHYS,NORFOLK,VA 23529. RP STANCIL, PC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Babb, James/0000-0002-3883-9501 NR 22 TC 35 Z9 35 U1 2 U2 6 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1993 VL 414 IS 2 BP 672 EP 675 DI 10.1086/173113 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU946 UT WOS:A1993LU94600027 ER PT J AU KENYON, SJ CALVET, N HARTMANN, L AF KENYON, SJ CALVET, N HARTMANN, L TI THE EMBEDDED YOUNG STARS IN THE TAURUS-AURIGA MOLECULAR CLOUD .1. MODELS FOR SPECTRAL ENERGY-DISTRIBUTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, CLOUDS; RADIATIVE TRANSFER; STARS, FORMATION; STARS, PRE-MAIN-SEQUENCE ID HERBIG-HARO OBJECTS; FAR-INFRARED OBSERVATIONS; LOW-MASS STAR; T-TAURI; DARK CLOUDS; DENSE CORES; CIRCUMSTELLAR DISKS; EXCITING STARS; CONTINUUM OBSERVATIONS; RADIATIVE-TRANSFER AB We describe radiative transfer calculations of infalling, dusty envelopes surrounding pre-main-sequence stars and use these models to derive physical properties for a sample of 21 heavily reddened young stars (''protostars'') in the Taurus-Auriga molecular cloud. The density distributions needed to match the far-infrared peaks in the spectral energy distributions of these embedded sources suggest mass infall rates similar to those predicted for simple thermally supported clouds with temperatures approximately 10 K. Unless the dust opacities are badly in error, our models require substantial departures from spherical symmetry in the envelopes of all sources, as in Terebey, Shu, & Cassen's rotating infall solutions. These flattened envelopes may be produced by a combination of rotation and cavities excavated by bipolar flows. Terebey, Shu, & Cassen's models indicate a centrifugal radius of approximately 70 AU for many objects if rotation is the only important physical effect, and this radius is reasonably consistent with typical estimates for the sizes of circumstellar disks around T Tauri stars. C1 CTR INVEST ASTRON,MERIDA 5101A,VENEZUELA. RP KENYON, SJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 87 TC 221 Z9 221 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1993 VL 414 IS 2 BP 676 EP 694 DI 10.1086/173114 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU946 UT WOS:A1993LU94600028 ER PT J AU KENYON, SJ WHITNEY, BA GOMEZ, M HARTMANN, L AF KENYON, SJ WHITNEY, BA GOMEZ, M HARTMANN, L TI THE EMBEDDED YOUNG STARS IN THE TAURUS-AURIGA MOLECULAR CLOUD .2. MODELS FOR SCATTERED-LIGHT IMAGES SO ASTROPHYSICAL JOURNAL LA English DT Article DE INFRARED, STARS; RADIATIVE TRANSFER; STARS, FORMATION; STARS, PRE-MAIN-SEQUENCE ID LOW-MASS STARS; STELLAR OBJECTS; T-TAURI; DENSE CORES; CIRCUMSTELLAR DISKS; DARK CLOUDS; POLARIZATION; DUST; PROTOSTARS; EXTINCTION AB We describe near-infrared imaging observations of embedded young stars in the Taurus-Auriga molecular cloud. We find a large range in J-K and H-K colors for these class I sources. The bluest objects have colors similar to the reddest T Tauri stars in the cloud; redder objects lie slightly above the reddening line for standard ISM dust and have apparent K extinctions of up to 5 mag. Most of these sources also show extended near-IR emission on scales of 10''-20'', which corresponds to linear sizes of 1500-3000 AU. The near-IR colors and nebular morphologies for this sample and the magnitude of linear polarization in several sources suggest scattered light produces most of the near-IR emission in these objects. We adopt the Terebey, Shu, and Cassen solution for an infalling, rotating protostellar cloud and use a two-dimensional Monte Carlo radiative transfer code to model the near-IR colors and images for the embedded sample. Our results suggest mass infall rates that agree with predictions for cold clouds (T approximately 10-20 K) and are generally consistent with rates estimated from radiative equilibrium models in a previous paper (e.g., M approximately 2-10 x 10(-6) M. yr-1). For reasonable dust grain parameters, the range of colors and extinctions require flattened density distributions with polar cavities evacuated by bipolar outflows. These results support the idea that infall and outflow occur simultaneously in deeply embedded, bipolar outflow sources. The data also indicate fairly large centrifugal radii, R(c) approximately 100 AU, and large inclinations to the rotational axis, i approximately 60-degrees - 90-degrees, for a typical source. Our centrifugal radius estimates agree with the disk radii inferred for many T Tauri stars in the Taurus-Auriga cloud. Better maps of polarization and molecular outflows in these objects can test our inclination estimates. RP KENYON, SJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 61 TC 138 Z9 138 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1993 VL 414 IS 2 BP 773 EP 792 DI 10.1086/173122 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU946 UT WOS:A1993LU94600036 ER PT J AU BARBERA, M MICELA, G SCIORTINO, S HARNDEN, FR ROSNER, R AF BARBERA, M MICELA, G SCIORTINO, S HARNDEN, FR ROSNER, R TI X-RAY-EMISSION AT THE LOW-MASS END - RESULTS FROM AN EXTENSIVE EINSTEIN-OBSERVATORY SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, LATE-TYPE; X-RAY, STARS ID MAIN-SEQUENCE STARS; O-TYPE STARS; VELOCITY DISTRIBUTION; ASTRONOMICAL DATA; DWARF STARS; ROTATION; LUMINOSITY; PLEIADES; SAMPLES; CLUSTER AB We have used all the available data from the Einstein Observatory Imaging Proportional Counter (IPC), and a critical compilation of cataloged optical data, to measure the 0.16 3.5 keV X-ray emission from 88 K and 169 M stars of luminosity classes IV, V, and VI within 25 pc from the Sun. The IPC detected 54 out of the 88 K stars, 70 out of the 138 M stars with M, less than 13.4 (corresponding approximately to M5), and 15 out of the 31 fainter M stars. We have identified a subsample of surveyed stars that is statistically representative of the population of K and M stars in the solar neighborhood. On the basis of this subsample (1) we have shown the occurrence of a drop in the level of X-ray emission for M stars later than approximately M5; (2) we have built unbiased maximum likelihood X-ray luminosity functions for the K, early M, and late M stars; (3) we have confirmed, both for K and M stars, the decrease of X-ray luminosity with increasing stellar age in the range of ages of disk population stars: and (4) we have shown that no obvious correlation is present between X-ray and bolometric luminosities in the entire representative samples of K and M stars, but only within flare stars which also seem to mark a saturation in X-ray luminosity level. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CHICAGO,DEPT ASTRON,CHICAGO,IL 60637. UNIV CHICAGO,ENRICO FERMI INST,CHICAGO,IL 60637. RP BARBERA, M (reprint author), IST & OSSERV ASTRON PALERMO,PALAZZO NORMANNI,I-90134 PALERMO,ITALY. OI Barbera, Marco/0000-0002-3188-7420 NR 67 TC 62 Z9 62 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1993 VL 414 IS 2 BP 846 EP 866 DI 10.1086/173127 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU946 UT WOS:A1993LU94600041 ER PT J AU MAOZ, E AF MAOZ, E TI DO OBSERVATIONS EXCLUDE GAMMA-RAY BURSTS ORIGINATING IN THE OORT CLOUD OF COMETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COMETS, GENERAL; GAMMA-RAYS, BURSTS ID ORBITS AB The currently favored explanation for the origin of gamma-ray bursts puts them at cosmological distances, but as long as there is no distance indicator to these events, all possible sources which are isotropically distributed should remain under consideration. This is why the Oort cloud of comets is kept on the list, although there is no known mechanism for generating gamma-ray bursts from cometary nuclei. Unlikely as it may seem, the possibility that gamma-ray bursts originate in the solar cometary cloud cannot be excluded until it is disproved. We use the available data on the distribution of gamma-ray bursts (the BATSE catalog up to 1992 March), and the Catalogue of Cometary Orbits by Marsden & Williams (1992) to investigate whether there is any observational indication for correlations between the angular distributions of gamma-ray bursts and the aphelia of comets, assuming that the distribution of aphelia direction reflects, at least to some extent, true variations in the column density of the Oort cloud. We also apply the [V/V(max)] test to both distributions. We have performed a variety of statistical tests (a Kolmogorov-Smirnov test for the distributions in galactic latitude, a chi2 test for the spherical multiple moments, and a two-dimensional cross-correlation analysis), including testing subsamples for isolating the effect of possible observational biases. These tests imply that it is unlikely that the two distributions agree, but the statistical significance is not sufficient for ruling out any connection with complete confidence. We performed Monte Carlo simulations which show that only when the number of bursts exceeds approximately 800 is it possible to rule out a correlation between the angular distributions. Currently, it is only the combination of these tests with the large disagreement found for the [V/V(max)] parameter which makes the Oort cloud of comets unlikely to be related to gamma-ray bursts. RP MAOZ, E (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS 51 60,GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 22 TC 13 Z9 13 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 1993 VL 414 IS 2 BP 877 EP 882 DI 10.1086/173130 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU946 UT WOS:A1993LU94600044 ER PT J AU KARP, I AF KARP, I TI IN MY FATHERS HOUSE - AFRICA IN THE PHILOSOPHY OF CULTURE - APPIAH,KA SO AMERICAN ANTHROPOLOGIST LA English DT Book Review RP KARP, I (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD SEP PY 1993 VL 95 IS 3 BP 766 EP 767 DI 10.1525/aa.1993.95.3.02a00580 PG 2 WC Anthropology SC Anthropology GA LZ147 UT WOS:A1993LZ14700056 ER PT J AU TAYLOR, PM AF TAYLOR, PM TI OF PEOPLE AND PLANTS - A BOTANICAL ETHNOGRAPHY OF NOKOPO VILLAGE, MADANG AND MOROBE PROVINCES, PAPUA-NEW-GUINEA - SCHMID,CK SO AMERICAN ANTHROPOLOGIST LA English DT Book Review RP TAYLOR, PM (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD SEP PY 1993 VL 95 IS 3 BP 770 EP 771 DI 10.1525/aa.1993.95.3.02a00620 PG 2 WC Anthropology SC Anthropology GA LZ147 UT WOS:A1993LZ14700060 ER PT J AU BISH, DL POST, JE AF BISH, DL POST, JE TI QUANTITATIVE MINERALOGICAL ANALYSIS USING THE RIETVELD FULL-PATTERN FITTING METHOD SO AMERICAN MINERALOGIST LA English DT Article ID POWDER DIFFRACTION PATTERNS; CRYSTAL-STRUCTURES; PHASE-ANALYSIS; REFINEMENT; MIXTURES AB Quantitative phase analysis of a number of multicomponent standard and natural mineral mixtures has been done using an adaptation of the Rietveld method. Binary mixtures (most 50:50 by weight) of corundum with quartz, hematite, ilmenite, magnetite, biotite, analcime, mordenite, or clinoptilolite were analyzed, using digital powder X-ray diffraction (XRD) data. In addition, a suite of standard mixtures of hematite and corundum, a natural feldspar mixture, the G-1 standard granite, two natural bauxite samples, and a mixture of biogenic carbonate minerals were also analyzed. Quantitative information was extracted from refined individual scale factors and unit-cell volumes (derived from refined unit-cell parameters), obtained with a Rietveld refinement program modified to analyze up to ten phases. The quantitative results for standard mixtures were within 2.5% (absolute) of the true values, with the exception of the hematite, ilmenite, and magnetite mixtures. Results for the latter mixtures using CuKalpha data were severely affected by microabsorption, but analysis of the hematite mixtures using FeKalpha radiation gave results with absolute errors less-than-or-equal-to 2%. Results for the G-1 granite and the natural feldspar agreed well with optically determined modes, and the method facilitated separation of the significant overlaps in the pattern of the carbonate minerals. Quantitative mineralogical analysis by the Rietveld method has several significant advantages over conventional methods of quantitative analysis. The method uses all intensity data in a pattern rather than a few of the most intense reflections, partially compensating for preferred orientation and extinction. In addition, standard data are calculated for each phase during analysis, overcoming the troublesome requirement of obtaining standards representative of the materials in an unknown. It is also possible to pin a wealth of information from each sample in addition to amounts of phases. Because some of the most troublesome systematic errors, including sample displacement and zero-point shift, can be refined, the method yields unit-cell parameters of an accuracy comparable with that obtained when using an internal d-value standard. The method should find a wide application in geology, including in modal analysis and compositional determinations of individual mineral components using unit-cell parameter systematics. C1 SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560. RP BISH, DL (reprint author), LOS ALAMOS NATL LAB,DIV EARTH & ENVIRONM SCI,LOS ALAMOS,NM 87545, USA. NR 30 TC 214 Z9 218 U1 3 U2 50 PU MINERALOGICAL SOC AMER PI WASHINGTON PA 1130 17TH ST NW SUITE 330, WASHINGTON, DC 20036 SN 0003-004X J9 AM MINERAL JI Am. Miner. PD SEP-OCT PY 1993 VL 78 IS 9-10 BP 932 EP 940 PG 9 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA MC300 UT WOS:A1993MC30000007 ER PT J AU EBERHARD, WG AF EBERHARD, WG TI EVALUATING MODELS OF SEXUAL SELECTION - GENITALIA AS A TEST-CASE SO AMERICAN NATURALIST LA English DT Note ID FEMALE CHOICE; MECHANICAL ISOLATION; COPULATORY-BEHAVIOR; EVOLUTION; SPECIATION; HYPOTHESIS; COURTSHIP; TRAITS C1 UNIV COSTA RICA, ESCUELA BIOL, SAN JOSE, COSTA RICA. RP EBERHARD, WG (reprint author), UNIV COSTA RICA, SMITHSONIAN TROP RES INST, CIUDAD UNIV, SAN JOSE, COSTA RICA. NR 42 TC 62 Z9 63 U1 0 U2 10 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD SEP PY 1993 VL 142 IS 3 BP 564 EP 571 DI 10.1086/285556 PG 8 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA LY873 UT WOS:A1993LY87300011 PM 19425990 ER PT J AU PERELLI, C AF PERELLI, C TI FROM COUNTERREVOLUTIONARY WARFARE TO POLITICAL AWAKENING - THE URUGUAYAN AND ARGENTINE ARMED-FORCES IN THE 1970S SO ARMED FORCES & SOCIETY LA English DT Review AB This article presents an alternative way of considering the role of military ideology in Uruguay and Argentina in the 1970's. Although it refers to two case studies in the Southern Cone, some of the conclusions emerging from an analysis of the effect of military intervention in politics upon the military itself have a general and universal character and could be extrapolated to and tested in other contexts. C1 SMITHSONIAN INST,WOODROW WILSON CTR,WASHINGTON,DC 20560. RP PERELLI, C (reprint author), SOC ANAL POLIT,PEITHO,CORONEL ALEGRE 1162 BIS,MONTEVIDEO 11300,URUGUAY. NR 116 TC 1 Z9 1 U1 0 U2 0 PU TRANSACTION PERIOD CONSORTIUM PI NEW BRUNSWICK PA DEPT 3091 RUTGERS-THE STATE UNIV OF NJ, NEW BRUNSWICK, NJ 08903 SN 0095-327X J9 ARMED FORCES SOC JI Armed Forces Soc. PD FAL PY 1993 VL 20 IS 1 BP 25 EP 49 DI 10.1177/0095327X9302000103 PG 25 WC Political Science; Sociology SC Government & Law; Sociology GA ML223 UT WOS:A1993ML22300002 ER PT J AU SCHOMBERT, JM HANLAN, PC BARSONY, M RAKOS, KD AF SCHOMBERT, JM HANLAN, PC BARSONY, M RAKOS, KD TI METALLICITY GRADIENTS IN EARLY-TYPE GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article ID CCD SURFACE PHOTOMETRY; ABSOLUTE MAGNITUDE RELATION; COMPOSITE STELLAR-SYSTEMS; BRIGHT ELLIPTIC GALAXIES; GLOBULAR-CLUSTERS; SPECTRAL EVOLUTION; JHK OBSERVATIONS; COLOR GRADIENTS; STANDARD STARS; SPECTROSCOPY AB Narrow-band optical and near-IR images are used to study color gradients in elliptical and S0 galaxies. Over 90% of the 23 sample galaxies display gradients in the optical of DELTA(v-y)/DELTA log r=-0.15+/-0.08 (which corresponds to DELTA(B-R)/DELTA log r=-0.09, in agreement with previous broadband studies) and in the near-IR of DELTA(V-K)/DELTA log r=-0.27+/-0.14 and DELTA(J-K)/DELTA log r=-0.15+/-0.12. Using an empirical calibration from the optical colors v-y to Mg2 produces a mean Mg gradient for the sample equivalent to DELTAMg2/DELTA log r=-0.036+/-0.016 or DELTAMg2/DELTAmu(V)=-0.013+/-0.007. Near-IR colors imply DELTA[Fe/H]/DELTA log r=-0.48 and core [Fe/H] values between -0.5 and +0.1 versus halo values near -1.3. A discrepancy exists between optical colors, influenced by light element abundances (particularly CN), and J-K, which is dominated by the true metallicity as reflected in the mean giant branch temperature, supporting the hypothesis that the [Mg/Fe] ratio in early-type galaxies differs from other galaxies due to an enhanced Type II SN component at the initial phase of star formation [Worthey et al., ApJ, 393, 611 (1992) ]. Gradients in our continuum color, b-y, signals a blue horizontal branch population contribution in the integrated light and warns that finer knowledge of the color evolutionary history of early-type galaxies will require substantial improvements in our Spectroenergy distribution models in order to predict behavior from the far-UV to the near-IR. C1 UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV VIENNA,INST ASTRON,A-1180 VIENNA,AUSTRIA. RP SCHOMBERT, JM (reprint author), CALTECH,JET PROPULS LAB,CTR INFRARED PROC & ANAL,MS100-22,PASADENA,CA 91125, USA. NR 65 TC 25 Z9 25 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1993 VL 106 IS 3 BP 923 EP 938 DI 10.1086/116694 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU943 UT WOS:A1993LU94300007 ER PT J AU ARMANDROFF, TE DACOSTA, GS CALDWELL, N SEITZER, P AF ARMANDROFF, TE DACOSTA, GS CALDWELL, N SEITZER, P TI THE DWARF SPHEROIDAL COMPANIONS TO M31 - A COLOR MAGNITUDE DIAGRAM FOR AND III SO ASTRONOMICAL JOURNAL LA English DT Article ID GLOBULAR-CLUSTERS; GIANT BRANCH; LEO-I; GALAXY; PHOTOMETRY; SYSTEM; METALLICITY; LUMINOSITY; ANDROMEDA; FIELD AB The prime focus CCD camera of the KPNO 4 m telescope has been used to image Andromeda III, a dwarf spheroidal galaxy companion to M31, in the V and I bands. The resulting color-magnitude diagram shows a well defined giant branch whose tip luminosity corresponds to that expected for an old metal-poor population at the distance of M31. By comparing these data with the giant branches of Galactic globular clusters, we determine that the abundance of And III is [Fe/H] = -2.0 +/- 0.15; with this abundance And III lies on the luminosity-abundance relation defined by the Galactic dwarf spheroidal galaxies. There is some evidence for a small (0.16 < sigma ([Fe/H]) < 0.24) intrinsic abundance dispersion within And III, but we are unable to unambiguously establish its presence. A study of the And III I-band luminosity function yields a distance modulus (m-M)0 of 24.4 +/- 0.2 for this galaxy, and indicates that the fraction of intermediate-age (3 to 10 Gyr) population in And III is approximately 10 +/- 10 percent. In all these aspects And III, like And I, is similar to the Galactic dwarf spheroidal systems, indicating that M31 and the Galaxy provided similar conditions for the evolution of such galaxies. C1 ANGLO AUSTRALIAN OBSERV,EPPING,NSW 2121,AUSTRALIA. SMITHSONIAN INST,F L WHIPPLE OBSERV,AMADO,AZ 85645. UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. RP ARMANDROFF, TE (reprint author), NATL OPT ASTRON OBSERV,KITT PEAK NATL OBSERV,POB 26732,TUCSON,AZ 85726, USA. NR 46 TC 53 Z9 53 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1993 VL 106 IS 3 BP 986 EP 998 DI 10.1086/116698 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU943 UT WOS:A1993LU94300011 ER PT J AU HAZEN, ML AF HAZEN, ML TI THE VARIABLE-STARS IN THE FIELD OF THE GLOBULAR-CLUSTER NGC-6544 SO ASTRONOMICAL JOURNAL LA English DT Article AB A search for variable stars in the neighborhood of the galactic globular cluster NGC 6544 has located two variables within the tidal radius of the cluster and two outside. A star of large proper motion was also detected. One of the variables within the tidal radius is possibly an eclipsing binary; the other is a RR Lyrae type ab star that may be a cluster member. The two field variables are RR Lyrae type ab stars. RP HAZEN, ML (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 6 TC 4 Z9 4 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1993 VL 106 IS 3 BP 1055 EP 1058 DI 10.1086/116703 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU943 UT WOS:A1993LU94300016 ER PT J AU SODERBLOM, DR JONES, BF BALACHANDRAN, S STAUFFER, JR DUNCAN, DK FEDELE, SB HUDON, JD AF SODERBLOM, DR JONES, BF BALACHANDRAN, S STAUFFER, JR DUNCAN, DK FEDELE, SB HUDON, JD TI THE EVOLUTION OF THE LITHIUM ABUNDANCES OF SOLAR-TYPE STARS .3. THE PLEIADES SO ASTRONOMICAL JOURNAL LA English DT Article ID LOW-MASS STARS; MAIN-SEQUENCE STARS; ALPHA-PERSEI CLUSTER; ROTATIONAL VELOCITIES; F-DWARFS; HYADES; PRAESEPE; TAURI; TEMPERATURES; ELEMENTS AB We report new measurements of lithium in more than 100 Pleiades F, G, and K dwarfs. Abundances were determined from spectrum synthesis fits to the data as well as from use of new curves of growth for the Li 6708 angstrom feature (presented in an Appendix). We confirm the intrinsic spread in lithium abundance within the Pleiades seen by Duncan & Jones [ApJ, 271, 663 (1983)], but we establish more observational constraints on Li in this cluster: First, for stars near 1.0 M. [about 0.60 to 0.75 in (B-V)0], the scatter in the relation between log N(Li)(= N(Li) and T(eff) is consistent with our observational uncertainty. That means that most late-F and early-G dwarfs in the Pleiades are consistent with the tight N(Li) versus mass relation seen in the Hyades in the same mass range. Second, at (B-V)0 almost-equal-to 0.8 (M almost-equal-to 0.9 M.), large and real star-to-star differences in N(Li) appear. The range in N(Li) at (B-V)0 almost-equal-to 0.8 is about 1 dex, and grows to as much as 1.5 dex for less massive stars Third, the most Li-rich stars have abundances at or near the primordial level for Population I (N(Li) almost-equal-to 3.2), and none exceed that level by a significant amount. Fourth, at any given color the stars that rotate fastest have the most Li and have the strongest chromospheric activity. We consider the ways in which an apparent spread in N(Li) could arise from an intrinsically tight N(Li)-mass relation and conclude that the spread is probably real and is not an artifact of line formation conditions or inhomogeneous atmospheres on the stars. It is possible to produce large apparent changes in N(Li) by covering a significant fraction of a star's surface with cooler regions (''spots''), but doing so has other ramifications that conflict with the observations. Some current models lead to a spread in N(Li) in which the fastest rotators (those that have lost the least angular momentum) have the most Li, and that mechanism may account for what is seen. A comparison of the Pleiades to the alpha Persei cluster shows that most a Persei stars have Li abundances comparable to their Pleiades counterparts, but there is a significant fraction (about 30%) of alpha Persei stars that lie below the Pleiades in N(Li) by 1 dex or more. Some of these anomalous stars have even less Li than Hyades stars of the same T(eff). If these stars are bona fide alpha Persei members (and they probably are), their Li abundances strain our understanding of Li depletion. The Pleiades, considered together with alpha Persei and the Hyades, shows that stars with [Fe/H]greater-than-or-equal-to 0.0 and which are more massive than about 1.25 M. do not deplete Li prior to reaching the main sequence. Moreover, solar-abundance stars ([Fe/H] = 0.0) with M greater than or similar to 1.1 M. do not experience pre-main-sequence depletion either. Pleiades dwarfs near T(eff) = 6700 K show evidence of being depleted in Li, indicating that an incipient Li ''chasm'' is present even at an age of 70 Myr. C1 UNIV CALIF SANTA CRUZ,LICK OBSERV,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. UNIV N CAROLINA,DEPT PHYS & ASTRON,CHAPEL HILL,NC 27599. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CHICAGO,DEPT ASTRON & ASTROPHYS,CHICAGO,IL 60637. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. UNIV TORONTO,DEPT ASTRON,TORONTO M5S 1A7,ONTARIO,CANADA. RP SODERBLOM, DR (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 80 TC 437 Z9 439 U1 1 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1993 VL 106 IS 3 BP 1059 EP 1079 DI 10.1086/116704 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU943 UT WOS:A1993LU94300017 ER PT J AU SODERBLOM, DR FEDELE, SB JONES, BF STAUFFER, JR PROSSER, CF AF SODERBLOM, DR FEDELE, SB JONES, BF STAUFFER, JR PROSSER, CF TI THE EVOLUTION OF THE LITHIUM ABUNDANCES OF SOLAR-TYPE STARS .4. PRAESEPE SO ASTRONOMICAL JOURNAL LA English DT Article ID LOW-MASS STARS; ALPHA-PERSEI CLUSTER; ROTATIONAL VELOCITIES; COLOR ANOMALIES; BINARY STARS; HYADES; PLEIADES; DWARFS AB Echelle observations are presented of lithium in 63 F and G dwarfs of the Praesepe cluster. For stars earlier than about GOV, Praesepe follows the same trends seen in the Hyades, which has approximately the same age and composition. Stars in Praesepe later than about G5V have more Li than their Hyades counterparts, possibly because Praesepe is slightly younger than the Hyades or has slightly lower metallicity. Significant differences in the abundance of Li are seen among stars of the same color, and, as in the Hyades, there is a tendency for the deviant stars to be binaries to the extent that duplicity in Praesepe is known. There are also stars with much less Li than most cluster members yet which appear to be true members of Praesepe. The close binary KW 181 has a normal Li abundance, despite the fact that similar close binaries in the Hyades are Li rich. C1 UNIV CALIF OBSERV,LICK OBSERV,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP SODERBLOM, DR (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 43 TC 79 Z9 79 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1993 VL 106 IS 3 BP 1080 EP 1086 DI 10.1086/116705 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU943 UT WOS:A1993LU94300018 ER PT J AU MARSCHALL, LA SEEDS, MA DAVIS, RJ AF MARSCHALL, LA SEEDS, MA DAVIS, RJ TI RADIAL-VELOCITY AND LIGHT VARIATIONS OF IR CEPHEI SO ASTRONOMICAL JOURNAL LA English DT Article AB Radical-velocity observations of the short-period Cepheid, IR Cephei, have been used to derive a complete radial-velocity versus phase curve for the variable, to investigate the presence of a possible binary companion, and to address the question of its membership in the Cepheus OB2 association. The observations are consistent with the absence of a close binary companion and shed doubt on its membership in the association. Photoelectric observations made with the Phoenix 10 Automated Photometric Telescope confirm the single nature of the star. We present simulations to show the effects of an equiluminous companion on the light curve of a Cepheid, concluding that the light curve of IR Cephei, whether or not it is corrected for a possible companion, exhibits the low-amplitude, sinusoidal variations characteristic of an s-type Cepheid. C1 FRANKLIN & MARSHALL COLL,DEPT PHYS & ASTRON,LANCASTER,PA 17604. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MARSCHALL, LA (reprint author), GETTYSBURG COLL,DEPT PHYS,GETTYSBURG,PA 17325, USA. NR 29 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 1993 VL 106 IS 3 BP 1123 EP 1132 DI 10.1086/116711 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU943 UT WOS:A1993LU94300024 ER PT J AU SCHMITT, JHMM KAHABKA, P STAUFFER, J PITERS, AJM AF SCHMITT, JHMM KAHABKA, P STAUFFER, J PITERS, AJM TI ROSAT ALL-SKY X-RAY SURVEY OF THE CORE REGION OF THE PLEIADES CLUSTER SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-RAYS, STARS; STARS, CORONAE; OPEN CLUSTERS, INDIVIDUAL, PLEIADES; STARS, FLARE; SURVEYS ID COEVAL STAR SAMPLES; CORONAE AB We present the ROSAT all-sky survey observations of the core region of the Pleiades cluster. A total of 24 X-ray sources are detected and identified with known Pleiades members; 20 X-ray sources had already previously been detected as X-ray emitters with the Einstein Observatory, 3 objects represent new detections, the status of one object is unclear. We show that the Pleiades when viewed as a statistical ensemble of X-ray sources look identical in both the Einstein and ROSAT observations. However, inspection of the activity levels of individual stars shows that changes of more than one order of magnitude have occurred in some stars over a time scale of ten years; we present a statistical method to properly construct the distribution function for the data set consisting of the measured Einstein IPC and ROSAT PSPC count rate ratios, which contains detections and upper and lower limits simultaneously. We argue that the observed large-scale variations in X-ray flux are in general not due to rotational modulation or flare events, but may be signatures of cyclic activity. We also report the detection of an X-ray super flare on the rapidly rotating Pleiades star HII2034. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. ASTRON INST ANTON PANNEKOEK, AMSTERDAM, NETHERLANDS. RP SCHMITT, JHMM (reprint author), MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. NR 18 TC 32 Z9 32 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 1993 VL 277 IS 1 BP 114 EP 122 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY306 UT WOS:A1993LY30600014 ER PT J AU MOROSSI, C FRANCHINI, M MALAGNINI, ML KURUCZ, RL BUSER, R AF MOROSSI, C FRANCHINI, M MALAGNINI, ML KURUCZ, RL BUSER, R TI COOL STARS - SPECTRAL ENERGY-DISTRIBUTIONS AND MODEL ATMOSPHERE FLUXES SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE STARS, LATE TYPE; STARS, ATMOSPHERES; ULTRAVIOLET, STARS ID EXTINCTION; CATALOG AB The main results of a program of systematic comparison between observed and computed spectral energy distributions of late G and K type solar chemical composition stars are illustrated. We built the observed energy distributions of eleven representative stars, from the ultraviolet to the infrared, starting from IUE archive data, supplemented by our own IUE observations, and data from the literature. Broad-band Johnson and DDO color indices, together with suitable calibrations, were used for estimating the basic stellar atmospheric parameters, i.e., effective temperature and surface gravity. Theoretical fluxes were computed for the appropriate parameters of each star, starting from a recent grid of atmosphere models. While very good consistency between data and model predictions has been obtained in the optical and infrared, significant discrepancies were found in the ultraviolet. We present semi-empirical models, based on the minimum temperature concept, obtained by modifying the temperature (versus optical depth) structure so as to mimic the effect of non-radiative heating in the upper photospheres of cool stars. The fluxes predicted by these models provide a fairly good description of the data not only in the visible and IR regions, but also in the ultraviolet region. Our results indicate that different values for the T(min)/T(eff) ratio, ranging from 0.76 (as in the Sun) up to 0.85 (theta Boo), are required to reproduce the observed ultraviolet fluxes of different stars. C1 UNIV TRIESTE, DIPARTIMENTO ASTRON, I-34131 TRIESTE, ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV BASEL, INST ASTRON, CH-4051 BASEL, SWITZERLAND. RP MOROSSI, C (reprint author), OSSERV ASTRON TRIESTE, VIA GB TIEPOLO 11, I-34131 TRIESTE, ITALY. NR 36 TC 23 Z9 23 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 1993 VL 277 IS 1 BP 173 EP 183 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY306 UT WOS:A1993LY30600020 ER PT J AU ALBERDI, A LARA, L MARCAIDE, JM ELOSEGUI, P SHAPIRO, II COTTON, WD DIAMOND, PJ ROMNEY, JD PRESTON, RA AF ALBERDI, A LARA, L MARCAIDE, JM ELOSEGUI, P SHAPIRO, II COTTON, WD DIAMOND, PJ ROMNEY, JD PRESTON, RA TI VLBA IMAGE OF SGR-A-ASTERISK AT LAMBDA=1.35-CM SO ASTRONOMY & ASTROPHYSICS LA English DT Letter DE RADIO SOURCES, SGR-A-ASTERISK; THE GALACTIC CENTER; INTERFEROMETRY, VLBI ID COMPACT RADIO-SOURCE; GALACTIC-CENTER; SIZE AB The compact non-thermal radio source at the Galactic Center, Sgr A*, has been imaged, at lambda=1.35 cm, for the first time with VLBI techniques. We observed Sgr A*, on 1991 June 23, with an array formed by 5 of the VLBA telescopes and the phased-VLA. The maximum angular resolution corresponded to a fringe spacing of 6.0x2.8 milliarcseconds in position angle 3-degrees (measured east from north). The observed surface brightness distribution of Sgr A* is best modelled by an elliptically shaped gaussian component with parameter values: flux density 1.07 +/- 0.15 Jy, major axis of FWHM = 2.58 0.08 milliarcseconds in position angle = 79-degrees +/- 6-degrees, and axial ratio = 0.5 +/- 0.2. The angular size of this model agrees well with the expected scattering size of Sgr A*. There is no clear evidence of any change in the source structure between our two sets of lambda=1.35 cm VLBI observations on Sgr A* which were separated by 6 years. C1 UNIV VALENCIA, E-46100 BURJASSOT, SPAIN. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NATL RADIO ASTRON OBSERV, CHARLOTTESVILLE, VA 22901 USA. NATL RADIO ASTRON OBSERV, SOCORRO, NM 87801 USA. JET PROP LAB, PASADENA, CA 91109 USA. RP ALBERDI, A (reprint author), CSIC, INST ASTROFIS ANDALUCIA, APDO 3004, E-18080 GRANADA, SPAIN. NR 22 TC 17 Z9 17 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 1993 VL 277 IS 1 BP L1 EP L4 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY306 UT WOS:A1993LY30600001 ER PT J AU RAGA, AC CANTO, J CALVET, N RODRIGUEZ, LF TORRELLES, JM AF RAGA, AC CANTO, J CALVET, N RODRIGUEZ, LF TORRELLES, JM TI A UNIFIED STELLAR JET MOLECULAR OUTFLOW MODEL SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE HYDRODYNAMICS; TURBULENCE; INTERSTELLAR MEDIUM, JETS AND OUTFLOWS; INTERSTELLAR MEDIUM, MOLECULES ID HERBIG-HARO OBJECTS; CO LINE FORMATION; MACH NUMBER JET; RILEY-I JETS; SURFACE BRIGHTNESS; THEORETICAL-MODEL; NH3 OBSERVATIONS; STAR FORMATION; BIPOLAR FLOWS; TURBULENT AB We present a coupled stellar jet/molecular outflow model. In this model, the stellar jet is assumed to have a large number of ''internal working surfaces'' that intercept material from the jet beam and eject it sideways into the near environment. This sideways ejection of mass and momentum leads to the formation of a ''turbulent envelope'' in which the jet material is mixed with entrained environmental gas. Under the assumption that the jet has a large number of internal working surfaces (which would probably be the case for an evolved outflow), we derive a simple theoretical framework for describing this flow. We then use this model to obtain predictions of intensity maps and position-velocity diagrams which can be directly compared with observations of molecular outflows. We also discuss the general characteristics predicted from our model, which apparently show a good qualitative agreement with observations of molecular outflows. However, our model appears to predict a somewhat too high degree of collimation for the molecular outflows. This discrepancy could be a result of the simple parametrization that we have adopted for the description of the turbulent flow. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV LEEDS, SCH MATH, LEEDS LS2 9JT, W YORKSHIRE, ENGLAND. Univ Nacl Autonoma Mexico, INST ASTRON, MEXICO CITY 04510, DF, MEXICO. CTR INVEST ASTRON, MERIDA 5101A, VENEZUELA. CSIC, INST ASTROFIS ANDALUCIA, E-18080 GRANADA, SPAIN. RP RAGA, AC (reprint author), UNIV MANCHESTER, INST SCI & TECHNOL, DEPT MATH, POB 88, MANCHESTER M60 1QD, LANCS, ENGLAND. NR 37 TC 76 Z9 76 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 1993 VL 276 IS 2 BP 539 EP 548 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LW895 UT WOS:A1993LW89500024 ER PT J AU PRESS, WH RYBICKI, GB SCHNEIDER, DP AF PRESS, WH RYBICKI, GB SCHNEIDER, DP TI PROPERTIES OF HIGH-REDSHIFT LYMAN-ALPHA CLOUDS .1. STATISTICAL-ANALYSIS OF THE SCHNEIDER-SCHMIDT-GUNN QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE INTERGALACTIC MEDIUM; QUASARS, ABSORPTION LINES ID FOREST; ABSORPTION; RESOLUTION; SPECTROPHOTOMETRY; CONTINUUM; SPECTRUM; QSOS AB Techniques for statistical analysis of the Lyman-alpha forest in high-redshift quasars are developed, and applied to the low-resolution (25 angstrom) spectra of 29 of the 33 quasars in the Schneider-Schmidt-Gunn (SSG) sample. We extrapolate each quasar's continuum shortward of Lyman-alpha emission, then consider each spectral bin of each quasar to be an (approximately) independent measurement of the absorption due to the Lyman-alpha clouds. With several thousand such measurements thus available, we can obtain good determinations of some interesting properties of clouds in the redshift range 2.5 < z < 4.3 without actually resolving any single cloud. We find that the mean absorption increases with z approximately as a power law (1 + z)gamma+1 with gamma = 2.46 +/- 0.37. The mean ratio of Lyman-alpha to Lyman-beta absorption in the clouds is 0.476 +/- 0.054. We also detect, and obtain ratios, for Lyman-gamma, delta, and possibly epsilon. We are also able to quantify the fluctuations of the absorption around its mean, and find that these are comparable to, or perhaps slightly larger than, that expected from an uncorrelated distribution of clouds. The techniques in this paper, which include the use of bootstrap resampling of the quasar sample to obtain estimated errors and error covariances, and a mathematical treatment of absorption from a (possibly nonuniform) stochastic distribution of lines, should be applicable to future, more extensive, data sets. C1 INST ADV STUDY,PRINCETON,NJ 08540. RP PRESS, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 33 TC 107 Z9 108 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1993 VL 414 IS 1 BP 64 EP 81 DI 10.1086/173057 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU114 UT WOS:A1993LU11400007 ER PT J AU ROSSI, P BODO, G MASSAGLIA, S FERRARI, A AF ROSSI, P BODO, G MASSAGLIA, S FERRARI, A TI RADIATIVE INSTABILITY IN SYNCHROTRON-EMITTING PLASMAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, JETS; INSTABILITIES; RADIATION MECHANISMS, CYCLOTRON AND SYNCHROTRON ID THERMAL INSTABILITIES; RADIO-SOURCES; CYGNUS-A; FILAMENTS; JET; EVOLUTION; M87 AB We present a linear study of the radiative instability driven by synchrotron emission in astrophysical plasmas. The novelty in this work is to consider the case of a non-Maxwellian distribution function and follow its time evolution consistently. We find unstable filamentation modes for any value of the spectral index, with increasing growth rate going from steep to flat spectra, provided that the plasma beta is larger than unity. We discuss our results in the context of the formation of the filamentary structures observed in jets and lobes of extended radio sources. C1 OSSERV ASTRON TORINO,I-10025 PINO TORINESE,ITALY. UNIV TURIN,IST FIS GEN,I-10125 TURIN,ITALY. UNIV TURIN,IST FIS MATEMAT,I-10123 TURIN,ITALY. RP ROSSI, P (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. RI Bodo, Gianluigi/F-9223-2012; ROSSI, PAOLA/I-7031-2015; OI Bodo, Gianluigi/0000-0002-9265-4081; ROSSI, PAOLA/0000-0002-0840-4726; massaglia, silvano/0000-0003-1779-7426 NR 22 TC 7 Z9 7 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1993 VL 414 IS 1 BP 112 EP 119 DI 10.1086/173061 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU114 UT WOS:A1993LU11400011 ER PT J AU HWANG, U HUGHES, JP CANIZARES, CR MARKERT, TH AF HWANG, U HUGHES, JP CANIZARES, CR MARKERT, TH TI HIGH-RESOLUTION X-RAY SPECTROSCOPY OF THE SUPERNOVA REMNANT N132D SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (LMC-N132D); MAGELLANIC CLOUDS; SUPERNOVA REMNANTS; X-RAYS, INTERSTELLAR ID NOVA REMNANTS; LINE EMISSION; ABUNDANCES; SPECTRA; RATIOS; MODELS AB We present a joint nonequilibrium ionization analysis of spectral data from the Einstein Observatory of the supernova remnant N132D in the Large Magellanic Cloud. We use high spectral resolution data from the Focal Plane Crystal Spectrometer (FPCS) and the Solid State Spectrometer (SSS), and lower spectral resolution data from the Imaging Proportional Counter (IPC) and Monitor Proportional Counter (MPC). Our updated analysis uses new calibrations for the FPCS and SSS efficiencies and a single-temperature, single-ionization time-scale model for the plasma. The FPCS detected individual emission lines of O VII, O VIII, Ne IX, Ne X, Fe XVII, and possibly Fe XX. Measured line widths for the oxygen lines suggest Doppler broadening that is roughly consistent with optically measured expansion velocities of 2250 km s-1. Constraints on temperature and ionization age from measured FPCS line flux ratios are consistent with results of spectral fits to the SSS and IPC data, which give a temperature of 8.4 (+0.8; -0.6) x 10(6) K and an ionization age of 6.1 (+5.0; -2.6) x 10(3) cm-3 yr. At the SSS/IPC temperature, FPCS flux ratios constrain the O/Fe abundance to be at least 1.9 times its solar value and the O/Ne abundance to be 0.2-1.0 times its solar value. The SSS/IPC fits provide constraints of 1.0-4.0 times solar for O/Fe and 0.5-1.5 times solar for O/Ne which are consistent with the FPCS results. We are puzzled to find that the SSS/IPC fits indicate abundances of oxygen and other heavy elements relative to the light elements that are below both their solar values and their mean values for the LMC. We therefore compare abundance ratios to calculations for the composition of ejecta from Type II supernovae including a contribution from swept-up interstellar material with elemental abundances appropriate for the LMC. Models for remnants with progenitor masses of 20 and 25 M. are completely consistent with the data, while remnants With progenitor masses of 13 and 15 M. can be made consistent if the progenitors are required to eject a large fraction of their iron cores. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP HWANG, U (reprint author), MIT,CTR SPACE RES,70 VASSAR ST,CAMBRIDGE,MA 02139, USA. NR 40 TC 30 Z9 30 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1993 VL 414 IS 1 BP 219 EP 229 DI 10.1086/173070 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU114 UT WOS:A1993LU11400020 ER PT J AU GOMEZ, JF TORRELLES, JM HO, PTP RODRIGUEZ, LF CANTO, J AF GOMEZ, JF TORRELLES, JM HO, PTP RODRIGUEZ, LF CANTO, J TI UPPER LIMITS TO THE DETECTION OF AMMONIA FROM PROTOPLANETARY DISKS AROUND HL TAURI AND L1551-IRS 5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; STARS, INDIVIDUAL (HL TAURI, L1551 IRS 5); STARS, PRE-MAIN-SEQUENCE ID YOUNG STELLAR OBJECTS; CIRCUMSTELLAR DISKS; ACCRETION DISK; STARS; OUTFLOWS; SPECTRA; IRS-5; GAS AB We present NH3(1, 1) and (2, 2) observations of the young stellar sources HL Tau and L1551-IRS 5 using the VLA in its B-configuration, which provides an angular resolution of approximately 0.4'' (approximately 50 AU at 140 pc) at 1.3 cm wavelength. Our goal was to detect and resolve circumstellar molecular disks with radius of the order of 100 AU around these two sources. No ammonia emission was detected toward either of them. The 3 sigma levels were 2.7 mJy beam-1 and 3.9 mJy beam-1 for HL Tau and L1551-IRS 5, respectively, with a velocity resolution of approximately 5 km s-1. With this nondetection, we estimate upper limits to the mass of the proposed protoplanetary molecular disks (within a radius of 10 AU from the central stars) on the order of 0.02 (X(NH3)/10(-8))-1 M. for HL Tau and 0.1 (X(NH3)/10(-8))-1 M. for L1551-IRS 5. C1 CSIC,INST ASTROFIS ANDALUCIA,E-18080 GRANADA,SPAIN. NATL AUTONOMOUS UNIV MEXICO,INST ASTRON,MEXICO CITY 04510,DF,MEXICO. RP GOMEZ, JF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 NR 33 TC 6 Z9 6 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1993 VL 414 IS 1 BP 333 EP 336 DI 10.1086/173079 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU114 UT WOS:A1993LU11400029 ER PT J AU LITES, BW RUTTEN, RJ KALKOFEN, W AF LITES, BW RUTTEN, RJ KALKOFEN, W TI DYNAMICS OF THE SOLAR CHROMOSPHERE .1. LONG-PERIOD NETWORK OSCILLATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE SUN, CHROMOSPHERE; SUN, OSCILLATIONS ID HIGH-RESOLUTION SPECTROSCOPY; CA-II LINES; DISK CHROMOSPHERE; VERTICAL PROPAGATION; SUNS CHROMOSPHERE; WAVE-PROPAGATION; FINE-STRUCTURE; PHASE DELAYS; K-EMISSION; ATMOSPHERE AB We analyze differences in solar oscillations between the chromospheric network and internetwork regions from a 1 hr sequence of spectrograms of a quiet region near disk center. The spectrograms contain Ca II H, Ca I 422.7 nm, and various Fe I blends in the Ca II H wing. They permit vertical tracing of oscillations throughout the photosphere and into the low chromosphere. We find that the rms amplitude of Ca II H line center Doppler fluctuations is approximately 1.5 km s-1 for both network and internetwork, but that the character of the oscillations differs markedly in these two regions. Within internetwork areas the chromospheric velocity power spectrum is dominated by oscillations with frequencies at and above the acoustic cutoff frequency. They are well correlated with the oscillations in the underlying photosphere, but they are much reduced in the network. In contrast, the network Ca II H line center velocity and intensity power spectra are dominated by low-frequency oscillations with periods of 5-20 minutes. Their signature is much clearer in our Ca II H line center measurements than in previously used diagnostics which are contaminated by signals from deeper layers. We find that these long-period oscillations are not correlated with underlying photospheric disturbances, and we discuss their nature. C1 STERREKUNDIG INST,3508 TA UTRECHT,NETHERLANDS. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP LITES, BW (reprint author), NATL CTR ATMOSPHER RES,HIGH ALTITUDE OBSERV,POB 3000,BOULDER,CO 80307, USA. NR 70 TC 183 Z9 184 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1993 VL 414 IS 1 BP 345 EP 356 DI 10.1086/173081 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU114 UT WOS:A1993LU11400031 ER PT J AU SOON, WH BALIUNAS, SL ZHANG, Q AF SOON, WH BALIUNAS, SL ZHANG, Q TI AN INTERPRETATION OF CYCLE PERIODS OF STELLAR CHROMOSPHERIC ACTIVITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, ACTIVITY; STARS, CHROMOSPHERES; STARS, LATE-TYPE; STARS, MAGNETIC FIELDS; STARS, ROTATION ID MAIN-SEQUENCE STARS; CA-II H; K-EMISSION; MAGNETIC-STRUCTURE; COOL STARS; ROTATION; DYNAMO; FIELD; CONVECTION; WAVES AB We propose (P(cyc)/P(rot))2, the square of the ratio of the characteristic oscillatory timescales of stellar chromospheric activity to the rotation period, as a useful parameterization of the stellar activity cycle and as the observational equivalent of the theoretical dynamo number, N(D). (P(cyc)/P(rot))2 can be obtained observationally from 25 yr activity records of stellar Ca II H and K chromospheric emission fluxes of the Mount Wilson Observatory HK Project. Using that parameterization, we study the relationships between the period of the activity cycle and mass or age (estimated from the average level of chromospheric emission, [R(HK)'], and its calibration with age). The quantity (P(cyc)/P(rot))2 increases as B-V decreases, in qualitative agreement with the expectation that as the fractional depth of convective zone decreases (i.e., toward higher mass stars), ND increases (i.e., the variability of stellar activity tends to be more irregular). (P(cyc)/p(rot))2 seems independent on age for young stars but has a well-defined dependence on age for the older stars. The difference in the behavior of (P(cyc)/P(rot))2 with age is another aspect of chromospheric activity that changes as a star ages; the time of the transition depends on mass but occurs roughly near stellar age of approximately 1-3 billion years. C1 TENNESSEE STATE UNIV,CTR EXCELLENCE INFORMAT SYST,NASHVILLE,TN 37203. RP SOON, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Zhang, Qizhou/0000-0003-2384-6589 NR 32 TC 34 Z9 34 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 1993 VL 414 IS 1 BP L33 EP L36 DI 10.1086/186989 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU108 UT WOS:A1993LU10800009 ER PT J AU GREENHOUSE, MA FELDMAN, U SMITH, HA KLAPISCH, M BHATIA, AK BARSHALOM, A AF GREENHOUSE, MA FELDMAN, U SMITH, HA KLAPISCH, M BHATIA, AK BARSHALOM, A TI INFRARED CORONAL EMISSION-LINES AND THE POSSIBILITY OF THEIR LASER-EMISSION IN SEYFERT NUCLEI SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ATOMIC PROCESSES; GALAXIES, NUCLEI; GALAXIES, SEYFERT; INFRARED, GALAXIES; LINE, FORMATION; MASERS ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRUM; CLASSICAL NOVAE; FORBIDDEN LINES; IONIZATION; GALAXIES; PROFILES; ELEMENTS; NGC-1068; PROGRAM AB Infrared coronal emission lines are providing a new window for observation and analysis of highly ionized gas in such Galactic and extragalactic sources as Seyfert nuclei and classical novae shells. These lines are expected to be primary coolants in colliding galaxies, galaxy cluster cooling flows, cometary-compact H II regions, and supernova remnants. In this paper, we compile a complete list of infrared (lambda > 1 mum) lines due to transitions within the ground configurations 2s(2)2p(k) and 3s(2)3p(k) (k = 1-5) or the first excited configurations 2s2p and 3s3p of highly ionized (chi greater-than-or-equal-to 100 eV) astrophysically abundant [n(X)/n(H) greater-than-or-equal-to 10(-6)]elements. Included are approximately 74 lines in ions of O, Ne, Na, Mg, Al, Si, S, Ar, Ca, Fe, and Ni spanning a wavelength range of approximately 1-280 mum. We present results from detailed balance calculations, critical densities for collisional deexcitation, intrinsic photon rates, branching ratios, and excitation temperatures for the majority of the compiled transitions. The temperature and density parameter space for dominant cooling via infrared coronal lines is presented, and the relationship of infrared and optical coronal lines is discussed. We find that under physical conditions found in Seyfert nuclei, 14 of 70 transitions examined have significant population inversions in levels that give rise to infrared coronal lines. Laser gain lengths and corresponding column densities are calculated for dense [10(6) less-than-or-equal-to n(e) (cm-3) less-than-or-equal-to 10(9)] collisionally ionized plasmas. Application of these results to cooler plasmas photoionized by power-law continuum radiation fields is also discussed. We find that several infrared coronal line transitions have laser gain lengths that correspond to column densities of 10(24-25) cm-2 which are modeled to exist in Seyfert nuclei. Observations that can reveal inverted level populations and laser gain in infrared coronal lines are also suggested. C1 NUCL RES CTR NEGEV,BEER SHEVA,ISRAEL. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. USN,RES LAB,SOLAR TERR RELAT BRANCH,WASHINGTON,DC 20375. USN,RES LAB,ARTEP INC,WASHINGTON,DC 20375. RP GREENHOUSE, MA (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560, USA. NR 63 TC 35 Z9 35 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD SEP PY 1993 VL 88 IS 1 BP 23 EP 48 DI 10.1086/191813 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LU110 UT WOS:A1993LU11000002 ER PT J AU GARCIA, MN SMITH, AP AF GARCIA, MN SMITH, AP TI FILTER USEFUL FOR SIMULATING THE LIGHT QUALITY OF UNDERSTORIES SO BIOTROPICA LA Spanish DT Note ID RADIATION; PHYTOCHROME; GROWTH; PLANTS RP GARCIA, MN (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 17 TC 2 Z9 2 U1 0 U2 0 PU ASSN TROP BIOL PI ST LOUIS PA MISSOURI BOTANICAL GARDEN 2345 TOWER GROVE AVE, ST LOUIS, MO 63110 SN 0006-3606 J9 BIOTROPICA JI Biotropica PD SEP PY 1993 VL 25 IS 3 BP 356 EP 358 PG 3 WC Ecology SC Environmental Sciences & Ecology GA MB694 UT WOS:A1993MB69400015 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI PLANNING IN THE UNIVERSITY-LIBRARY - BIDDLE,SF SO INFORMATION PROCESSING & MANAGEMENT LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0306-4573 J9 INFORM PROCESS MANAG JI Inf. Process. Manage. PD SEP-OCT PY 1993 VL 29 IS 5 BP 675 EP 676 DI 10.1016/0306-4573(93)90091-Q PG 2 WC Computer Science, Information Systems; Information Science & Library Science SC Computer Science; Information Science & Library Science GA LZ017 UT WOS:A1993LZ01700014 ER PT J AU COOKSY, AL ELROD, MJ SAYKALLY, RJ KLEMPERER, W AF COOKSY, AL ELROD, MJ SAYKALLY, RJ KLEMPERER, W TI DIPOLE-MOMENT ANALYSIS OF EXCITED VAN-DER-WAALS VIBRATIONAL-STATES OF ARH35CL SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID INFRARED-LASER SPECTROSCOPY; AR-HCL; INTERMOLECULAR FORCES; STARK SPECTROSCOPY; BENDING VIBRATION; SIGMA-BEND; ARHCL; SPECTRUM; RESONANCE; BONDS AB The far-infrared laser electric resonance spectra of the prototypical 'atom-diatom complex (ArHCl)-Cl-35 are analyzed using improved zero-field molecular constants, yielding accurate permanent and transition dipole moments for the three lowest excited van der Waals vibrational states. The constants are obtained from a multistate fit to previous microwave, far-infrared laser electric resonance, and far-infrared tunable laser spectra, as well as new far-infrared measurements of the SIGMA-stretch state, which are reported here. The signs of the dipole moments and Coriolis coefficients establish the relative orientations of the HCl subunit in these states. The fit is found to converge only if these signs correspond to the HCl pointing in opposite directions along the a inertial axis in the SIGMA-stretch and SIGMA-bend states. A weak preference, near the experimental error limit, is found for the Ar-Cl-H average angle in the PI-bend state to be greater than 90-degrees, contrary to expectation. For the best fit, we obtain the a-axis dipole moment components -0.5413(11) D (SIGMA bend), -0.26345(29) D (PI bend), and 0.6754(36) D (SIGMA-stretch); and the b-axis components 0.365(12) D (PI and SIGMA-bend) and -0.0465(43) D (PI and SIGMA stretches), where the signs of the Coriolis coefficients and mu(a) for the SIGMA stretch have been arbitrarily fixed positive. For the expected PI-bend configuration, with the Ar-Cl-H angle less than 90-degrees, the magnitudes along the a axis change only slightly, but the b-axis components become 0.149(12) and -0.1403(64) D for the H-SIGMA-bend and PI-SIGMA-stretch interactions, respectively. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALIF BERKELEY,DEPT CHEM,BERKELEY,CA 94720. RP COOKSY, AL (reprint author), HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138, USA. NR 17 TC 4 Z9 4 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD SEP 1 PY 1993 VL 99 IS 5 BP 3200 EP 3204 DI 10.1063/1.465128 PG 5 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA LU722 UT WOS:A1993LU72200006 ER PT J AU MORENO, SH AF MORENO, SH TI IMPACT OF DEVELOPMENT ON THE PANAMA CANAL ENVIRONMENT SO JOURNAL OF INTERAMERICAN STUDIES AND WORLD AFFAIRS LA English DT Article RP MORENO, SH (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 23 TC 2 Z9 3 U1 0 U2 3 PU UNIV MIAMI PI CORAL GABLES PA J INTERAMER STUD WORLD AFF PO BOX 248134, CORAL GABLES, FL 33124 SN 0022-1937 J9 J INTERAM STUD WORLD JI J. Interam. Stud. World Aff. PD FAL PY 1993 VL 35 IS 3 BP 129 EP 149 DI 10.2307/165971 PG 21 WC Area Studies; International Relations; Political Science SC Area Studies; International Relations; Government & Law GA MF053 UT WOS:A1993MF05300006 ER PT J AU COOPER, GA LEE, DE AF COOPER, GA LEE, DE TI CALLORIA, A REPLACEMENT NAME FOR THE RECENT BRACHIOPOD GENUS WALTONIA FROM NEW-ZEALAND SO JOURNAL OF THE ROYAL SOCIETY OF NEW ZEALAND LA English DT Article DE TEREBRATULIDA; RECENT, TAXONOMIC REVISION, WALTONIA, MAGASELLA, CALLORIA NEW GENUS AB The new generic name Calloria is proposed as a replacement for Waltonia Davidson, 1850, the type species of which is the common smooth red endemic terebratulide brachiopod of New Zealand seas. Waltonia was based on a juvenile, imperfect specimen of a ribbed brachiopod belonging to an existing genus, and was abandoned by Davidson in 1861. The complex later nomenclatural history of Waltonia and Magasella Dall is described in detail. A type is selected for Terebratula inconspicua Sowerby, 1846, the type species of Calloria n. gen. C1 SMITHSONIAN INST,DEPT PALEOBIOL,WASHINGTON,DC 20560. NR 45 TC 4 Z9 4 U1 0 U2 0 PU SIR PUBLISHING PI WELLINGTON PA PO BOX 399, WELLINGTON, NEW ZEALAND SN 0303-6758 J9 J ROY SOC NEW ZEAL JI J. R. Soc. N.Z. PD SEP PY 1993 VL 23 IS 3 BP 257 EP 270 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA MJ282 UT WOS:A1993MJ28200003 ER PT J AU COOPER, GA DOHERTY, PJ AF COOPER, GA DOHERTY, PJ TI CALLORIA-VARIEGATA, A NEW RECENT SPECIES OF BRACHIOPOD (ARTICULATA, TEREBRATULIDA) FROM NORTHERN NEW-ZEALAND SO JOURNAL OF THE ROYAL SOCIETY OF NEW ZEALAND LA English DT Article DE TEREBRATULIDA; RECENT; CALLORIA-VARIEGATA; ECOLOGY; DISTRIBUTION; LOOP DEVELOPMENT AB A new species of terebratellid brachiopod, Calloria variegata, is described from rocky, subtidal habitats in the Hauraki Gulf, northern New Zealand. The distribution and ecology of C. variegata are compared with the closely related C. inconspicua, and a detailed description of the new species, including loop development, is provided. C1 SMITHSONIAN INST,DEPT PALEOBIOL,WASHINGTON,DC 20560. UNIV AUCKLAND,DEPT ZOOL,AUCKLAND,NEW ZEALAND. NR 9 TC 4 Z9 4 U1 0 U2 0 PU SIR PUBLISHING PI WELLINGTON PA PO BOX 399, WELLINGTON, NEW ZEALAND SN 0303-6758 J9 J ROY SOC NEW ZEAL JI J. R. Soc. N.Z. PD SEP PY 1993 VL 23 IS 3 BP 271 EP 281 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA MJ282 UT WOS:A1993MJ28200004 ER PT J AU BALLOU, JD AF BALLOU, JD TI ASSESSING THE RISKS OF INFECTIOUS-DISEASES IN CAPTIVE BREEDING AND REINTRODUCTION PROGRAMS SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE DISEASE RISK; POPULATION VIABILITY ANALYSES; METAPOPULATION; CAPTIVE BREEDING ID CALLITRICHID HEPATITIS; POPULATIONS AB Disease risks are an inherent part of captive breeding, translocation, and reintroduction Programs and of research involving contact between researchers and animals. Thus, quantitative assessment of the risks of disease should be an important part of developing conservation strategies. Population viability analysis (PVA) and the use of computer modeling allows conservation planners to examine the potential effects of both the catastrophic and subcatastrophic effects of disease on long-term population viability, measured as probability of extinction, and to explore strategies to mitigate unacceptably high risks. The effects of diseases on the demographic, environmental, and genetic aspects of a population should be examined. Metapopulation management strategies that establish geographically separate populations are likely to provide protection against total population extinction due to single disease epidemics. However, to offset the genetic costs of smaller population size, movement of animals (under quarantined supervision) may be required. RP BALLOU, JD (reprint author), SMITHSONIAN INST,DEPT ZOOL RES,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 49 TC 34 Z9 35 U1 2 U2 15 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD SEP PY 1993 VL 24 IS 3 BP 327 EP 335 PG 9 WC Veterinary Sciences SC Veterinary Sciences GA ME071 UT WOS:A1993ME07100013 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI NO PLACE LIKE UTOPIA - MODERN ARCHITECTURE AND THE COMPANY WE KEPT - BLAKE,P SO LIBRARY JOURNAL LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 1993 VL 118 IS 14 BP 178 EP 178 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA LW982 UT WOS:A1993LW98200034 ER PT J AU RUIZ, GM HINES, AH POSEY, MH AF RUIZ, GM HINES, AH POSEY, MH TI SHALLOW-WATER AS A REFUGE HABITAT FOR FISH AND CRUSTACEANS IN NONVEGETATED ESTUARIES - AN EXAMPLE FROM CHESAPEAKE BAY SO MARINE ECOLOGY PROGRESS SERIES LA English DT Review ID CRABS CALLINECTES-SAPIDUS; EELGRASS ZOSTERA-MARINA; SUBMERGED AQUATIC VEGETATION; PREDATOR-PREY INTERACTIONS; INTERTIDAL SALT-MARSH; BLUE CRABS; FUNDULUS-HETEROCLITUS; GRASS SHRIMP; MACROFAUNAL CRUSTACEANS; STRUCTURAL COMPONENTS AB Abundances and size-frequency distributions of common epibenthic fish and crustaceans were compared among 3 depth zones (1-35, 35-70, 71-95 cm) of the Rhode River, a subestuary of Chesapeake Bay, USA. In the absence of submerged aquatic vegetation (SAV), inter- and intraspecific size segregation occurred by depth from May to October, 1989-1992. Small species (Palaemonetes pugio, Crangon septemspinosa, Fundulus heteroclitus, F. majalis, Rhithropanopeus harrisii, Apeltes quadracus, Gobiosoma bosci) were most abundant at water depths < 70 cm. Furthermore, the proportion of small individuals decreased significantly with depth for 7 of 8 species, with C. septemspinosa being the exception, exhibiting no size change with increasing depth. These distributional patterns were related to depth-dependent predation risk. Large species (Callinectes sapidus, Leiostomus xanthurus, and Micropogonias undulatus), known predators of some of the small species, were often most abundant in deep water (> 70 cm). In field experiments, mortality of tethered P. pugio (30 to 35 mm), small F. heteroclitus (40 to 50 mm), and small C. sapidus (30 to 70 mm) increased significantly with depth. We hypothesize that predation risk was size-dependent, creating the observed intra- and interspecific size differences among depth zones. For C. septemspinosa, burial may modify this size-dependency and create the unusual absence of intraspecific size increase with depth. Historically, P. pugio and Fundulus spp, (and other small species) were not restricted to shallow (< 70 cm) waters and were abundant in deeper SAV beds, which provided a structural refuge from predators. Since the recent demise of SAV in Chesapeake Bay, our results indicate many small species have shifted their distributions and now utilize primarily shallow water as an alternate refuge habitat. C1 UNIV N CAROLINA, DEPT BIOL SCI, WILMINGTON, NC 28403 USA. RP RUIZ, GM (reprint author), SMITHSONIAN ENVIRONM RES CTR, POB 28, EDGEWATER, MD 21037 USA. OI Ruiz, Gregory/0000-0003-2499-441X NR 113 TC 224 Z9 230 U1 4 U2 43 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD SEP PY 1993 VL 99 IS 1-2 BP 1 EP 16 DI 10.3354/meps099001 PG 16 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA LY003 UT WOS:A1993LY00300001 ER PT J AU GRAYBEAL, A AF GRAYBEAL, A TI THE PHYLOGENETIC UTILITY OF CYTOCHROME-B - LESSONS FROM BUFONID FROGS SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article ID ANIMAL MITOCHONDRIAL-DNA; NUCLEOTIDE-SEQUENCE; GENE ORGANIZATION; EVOLUTIONARY BIOLOGY; GENOME; RATES; SUBSTITUTION; SYSTEMATICS; AMPHIBIA; VERTEBRATES C1 SMITHSONIAN INST, MUSEUM VERTEBRATE ZOOL, WASHINGTON, DC 20560 USA. UNIV CALIF BERKELEY, MOLEC SYSTEMAT LAB, BERKELEY, CA 94720 USA. UNIV CALIF BERKELEY, DEPT INTEGRAT BIOL, BERKELEY, CA 94720 USA. NR 99 TC 87 Z9 89 U1 0 U2 2 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD SEP PY 1993 VL 2 IS 3 BP 256 EP 269 DI 10.1006/mpev.1993.1024 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA MQ773 UT WOS:A1993MQ77300007 PM 8136925 ER PT J AU GOODWAY, M AF GOODWAY, M TI RECENT INFORMATION OVERLOOKED IN FORGING IRON SO MRS BULLETIN LA English DT Letter RP GOODWAY, M (reprint author), SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. NR 28 TC 0 Z9 0 U1 0 U2 0 PU MATERIALS RESEARCH SOCIETY PI PITTSBURGH PA 9800 MC KNIGHT ROAD SUITE 327, PITTSBURGH, PA 15237 SN 0883-7694 J9 MRS BULL JI MRS Bull. PD SEP PY 1993 VL 18 IS 9 BP 8 EP 10 PG 3 WC Materials Science, Multidisciplinary; Physics, Applied SC Materials Science; Physics GA LX554 UT WOS:A1993LX55400003 ER PT J AU RAND, AS DUDLEY, R AF RAND, AS DUDLEY, R TI FROGS IN HELIUM - THE ANURAN VOCAL SAC IS NOT A CAVITY RESONATOR SO PHYSIOLOGICAL ZOOLOGY LA English DT Article ID SOUND PRODUCTION; PHYSALAEMUS-PUSTULOSUS; MECHANISM; SELECTION; ENERGY; TRACT; BUFO AB A widely cited yet unproven function for anuran vocal sacs is that of cavity resonance and call tuning during vocalization. Because resonant frequency is influenced by the speed of sound within the cavity, we replaced a substantial proportion of the air in the anuran vocal tract with heliox (80% He/20% O2), a medium in which the speed of sound is approximately 75% faster than in a normal atmosphere. Such a manipulation will increase energy in higher call frequencies, provided that cavity resonance is present. In a heliox atmosphere, no consistent or predictable change in the frequency distribution of sound energy was observed in the advertisement calls of two hylids and one leptodactylid or in the release call of a bufonid. Therefore, the call characteristics of the anurans in this study do not arise from cavity resonance in the vocal sac or other supralaryngeal structures. The anuran vocal sac may have a variety of acoustic and nonacoustic functions, but that of cavity resonator can now be excluded in the species examined here and is unlikely to be found in other anurans. C1 UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712. RP RAND, AS (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,POB 2072,APO AA 34002-0948,BALBOA,PANAMA. NR 24 TC 27 Z9 28 U1 1 U2 10 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0031-935X J9 PHYSIOL ZOOL JI Physiol. Zool. PD SEP-OCT PY 1993 VL 66 IS 5 BP 793 EP 806 PG 14 WC Physiology; Zoology SC Physiology; Zoology GA MC859 UT WOS:A1993MC85900009 ER PT J AU TYREE, MT COCHARD, H CRUIZIAT, P SINCLAIR, B AMEGLIO, T AF TYREE, MT COCHARD, H CRUIZIAT, P SINCLAIR, B AMEGLIO, T TI DROUGHT-INDUCED LEAF SHEDDING IN WALNUT - EVIDENCE FOR VULNERABILITY SEGMENTATION SO PLANT CELL AND ENVIRONMENT LA English DT Article DE JUGLANS-REGIA; WALNUT; LEAF SHEDDING; DROUGHT; PLANT SEGMENTATION ID HEAT-BALANCE METHOD; HYDRAULIC ARCHITECTURE; WATER RELATIONS; SMALL TREES; SAP FLOW; EMBOLISM; STEM AB Trees of Juglans regia L. shed leaves when subjected to drought. Before shedding (when leaves are yellow), the petioles have lost 87% of their maximum hydraulic conductivity, but stems have lost only 14% of their conductivity. This is caused by the higher vulnerability of petioles than stems to water-stress induced cavitation. These data are discussed in the context of the plant segmentation hypothesis. C1 INRA,PHYSIOL INTEGREE ARBRE FRUITIER LAB,F-63039 CLERMONT FERRAND,FRANCE. INRA,ECOPHYSIOL FORESTIERE LAB,F-54280 CHAMPENOUX,FRANCE. SMITHSONIAN TROP RES INST,UNIT 0948,BALBOA,PANAMA. RP TYREE, MT (reprint author), US FOREST SERV,NE FOREST EXPT STN,POB 968,BURLINGTON,VT 05402, USA. RI AMEGLIO, THIERRY/E-1535-2011; Cochard, Herve/P-7406-2015 OI AMEGLIO, THIERRY/0000-0001-6919-3531; Cochard, Herve/0000-0002-2727-7072 NR 17 TC 146 Z9 158 U1 4 U2 28 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0140-7791 J9 PLANT CELL ENVIRON JI Plant Cell Environ. PD SEP PY 1993 VL 16 IS 7 BP 879 EP 882 DI 10.1111/j.1365-3040.1993.tb00511.x PG 4 WC Plant Sciences SC Plant Sciences GA LZ893 UT WOS:A1993LZ89300014 ER PT J AU STINE, JK AF STINE, JK TI THE UNITED-STATES-ARMY CORPS-OF-ENGINEERS RESPONSE TO THE EXXON-VALDEZ OIL-SPILL - MCDONNELL,JA SO PUBLIC HISTORIAN LA English DT Book Review RP STINE, JK (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD FAL PY 1993 VL 15 IS 4 BP 117 EP 119 PG 3 WC History SC History GA MH910 UT WOS:A1993MH91000032 ER PT J AU KUIJKEN, K AF KUIJKEN, K TI COUNTER-ROTATING POPULATIONS IN A DISK GALAXY SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article; Proceedings Paper CT 2ND HUBBLE FELLOWS SYMP CY NOV 09-11, 1992 CL SPACE TELESCOPE SCI INST, BALTIMORE, MD HO SPACE TELESCOPE SCI INST ID VELOCITY DISPERSIONS; STELLAR DISKS; NGC-4550; SPECTRA; WARPS AB Galactic absorption-line spectra can now yield valuable information about the internal kinematics beyond the classical measures of mean velocity and (Gaussian) velocity dispersion. An application of a new algorithm to the photometrically normal disk galaxy NGC 7217 has revealed that around 30% of the stars circulate in the opposite sense to the majority. The subtle, serendipitous nature of the discovery raises the possibility that this situation may not be uncommon. NGC 7217 and the previously discovered case of NGC 4550 (in which both directions of circulation are equally populated) point towards substantial secondary infall of material with variable angular momentum, and suggest a possible explanation of the decrease of bulge-to-disk ratio with strengthening spiral structure along the Hubble sequence. RP KUIJKEN, K (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 23 TC 6 Z9 6 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 1993 VL 105 IS 691 BP 1016 EP 1021 DI 10.1086/133275 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY652 UT WOS:A1993LY65200025 ER PT J AU FRANX, M AF FRANX, M TI CONSTRAINING GALAXY EVOLUTION AND COSMOLOGY FROM GALAXY KINEMATICS - 1ST OBSERVATIONS AT Z=0.18 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article; Proceedings Paper CT 2ND HUBBLE FELLOWS SYMP CY NOV 09-11, 1992 CL SPACE TELESCOPE SCI INST, BALTIMORE, MD HO SPACE TELESCOPE SCI INST ID ELLIPTICAL GALAXIES; CLUSTERS; PHOTOMETRY; SPECTROSCOPY; DISTANT AB There is significant evidence that galaxy evolution is a complex process, in which mass accretion, mergers, and star bursts play an important role. This complex evolution adds significant freedom to the modeling of observations of high-redshift galaxies. Additional constraints are necessary. Such constraints may come from measurements of circular velocities, or velocity dispersions of galaxies at intermediate redshift. The first observations of central velocity dispersions are presented for galaxies in the rich cluster Abell 665 at z=0.18. Full curves of radial velocity, and velocity dispersion of cluster members are presented. The measurements result in a well-defined Faber-Jackson relation for the red cluster members. A blue galaxy is lying 2.2 mag off the relation, and has an ''E+A'' spectrum. This ''Butcher-Oemler'' galaxy is rotating rapidly, which is indicative of a strong disk. The observations show that measurements of central velocity dispersions are possible with current telescope capabilities. Observations at higher redshifts will lead to new constraints on both galaxy evolution and cosmology. RP FRANX, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 34 TC 44 Z9 44 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD SEP PY 1993 VL 105 IS 691 BP 1058 EP 1062 DI 10.1086/133282 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY652 UT WOS:A1993LY65200032 ER PT J AU BERLIN, EA JARA, VM BERLIN, B BREEDLOVE, DE DUNCAN, TO LAUGHLIN, RM AF BERLIN, EA JARA, VM BERLIN, B BREEDLOVE, DE DUNCAN, TO LAUGHLIN, RM TI ME-WINIK - DISCOVERY OF THE BIOMEDICAL EQUIVALENCE FOR A MAYA ETHNOMEDICAL SYNDROME SO SOCIAL SCIENCE & MEDICINE LA English DT Article DE GALLBLADDER DISEASE; ETHNOMEDICINE; EPIDEMIOLOGY; CROSS-CULTURAL HEALTH CARE; NATIVE AMERICAN HEALTH; MAYA; MEXICO ID GALLBLADDER-DISEASE; AMERICAN-INDIANS; BILIARY-TRACT; CANCER; PREVALENCE; RISK; GALLSTONES; POPULATION; NATIVES AB Investigation of the correspondence of ethnomedical illness syndromes and biomedical disease classification has led to the identification of a high prevalence of gallbaldder disease among the Tzeltal and Tzotzil Maya populations of Highland Chiapas. This condition, known to demonstrate exceptionally high rates among North American Indians, has not previously been described among the Highland Maya. The failure to recognize this serious health problem has been due primarily to cultural differences in understanding the anatomy and difficulties arising from communication of symptomatology. A focus on the interface of ethnomedicine and biomedicine is shown to have significance from both theoretical and applied perspectives. C1 SMITHSONIAN INST,DEPT ANTHROPOL,WASHINGTON,DC 20560. UNIV CALIF BERKELEY,DEPT INTEGRAT BIOL,BERKELEY,CA 94720. CALIF ACAD SCI,DEPT BOT,SAN FRANCISCO,CA 94118. RP BERLIN, EA (reprint author), UNIV CALIF BERKELEY,DEPT ANTHROPOL,BERKELEY,CA 94720, USA. NR 45 TC 14 Z9 14 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0277-9536 J9 SOC SCI MED JI Soc. Sci. Med. PD SEP PY 1993 VL 37 IS 5 BP 671 EP 678 DI 10.1016/0277-9536(93)90106-E PG 8 WC Public, Environmental & Occupational Health; Social Sciences, Biomedical SC Public, Environmental & Occupational Health; Biomedical Social Sciences GA LQ010 UT WOS:A1993LQ01000012 PM 8211281 ER PT J AU BULL, JJ HUELSENBECK, JP CUNNINGHAM, CW SWOFFORD, DL WADDELL, PJ AF BULL, JJ HUELSENBECK, JP CUNNINGHAM, CW SWOFFORD, DL WADDELL, PJ TI PARTITIONING AND COMBINING DATA IN PHYLOGENETIC ANALYSIS SO SYSTEMATIC BIOLOGY LA English DT Editorial Material ID EVOLUTIONARY TREES; CLADISTIC-ANALYSIS; ESCHERICHIA-COLI; BRANCHING ORDER; MOLECULAR-DATA; CONGRUENCE; PARSIMONY; RATES; DNA; SUBSTITUTION C1 SMITHSONIAN INST, MOLEC SYSTEMAT LAB, WASHINGTON, DC 20560 USA. MASSEY UNIV, DEPT PLANT BIOL, PALMERSTON NORTH, NEW ZEALAND. RP BULL, JJ (reprint author), UNIV TEXAS, DEPT ZOOL, AUSTIN, TX 78712 USA. RI Cunningham, Clifford/B-9807-2014; Huelsenbeck, John/C-6398-2013; OI Cunningham, Clifford/0000-0002-5434-5122 NR 57 TC 218 Z9 222 U1 1 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1063-5157 EI 1076-836X J9 SYST BIOL JI Syst. Biol. PD SEP PY 1993 VL 42 IS 3 BP 384 EP 397 DI 10.2307/2992473 PG 14 WC Evolutionary Biology SC Evolutionary Biology GA LY704 UT WOS:A1993LY70400012 ER PT J AU TOON, O BROWELL, E GARY, B LAIT, L LIVINGSTON, J NEWMAN, P PUESCHEL, R RUSSELL, P SCHOEBERL, M TOON, G TRAUB, W VALERO, FPJ SELKIRK, H JORDAN, J AF TOON, O BROWELL, E GARY, B LAIT, L LIVINGSTON, J NEWMAN, P PUESCHEL, R RUSSELL, P SCHOEBERL, M TOON, G TRAUB, W VALERO, FPJ SELKIRK, H JORDAN, J TI HETEROGENEOUS REACTION PROBABILITIES, SOLUBILITIES, AND THE PHYSICAL STATE OF COLD VOLCANIC AEROSOLS SO SCIENCE LA English DT Article ID POLAR STRATOSPHERIC CLOUDS; ARCTIC WINTER STRATOSPHERE; SULFURIC-ACID; NITRIC-ACID; DROPLETS AB On 19 January 1992, heterogeneous loss of HNO3, ClNO3, and HCl was observed in part of the Mount Pinatubo volcanic cloud that had cooled as a result of forced ascent. Portions of the volcanic cloud froze near 191 kelvin. The reaction probability of ClNO3 and the solubility of HNO3 were close to laboratory measurements on liquid sulfuric acid. The magnitude of the observed loss of HCl suggests that it underwent a heterogeneous reaction. Such reactions could lead to substantial loss of HCl on background sulfuric acid particles and so be important for polar ozone loss. C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23665. JET PROP LAB,PASADENA,CA 91109. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. SRI INT,MENLO PK,CA 94025. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. STERLING SOFTWARE INC,PALO ALTO,CA 94303. RP TOON, O (reprint author), NASA,AMES RES CTR,MOFFETT FIELD,CA 94035, USA. RI Newman, Paul/D-6208-2012 OI Newman, Paul/0000-0003-1139-2508 NR 18 TC 35 Z9 35 U1 0 U2 1 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD AUG 27 PY 1993 VL 261 IS 5125 BP 1136 EP 1140 DI 10.1126/science.261.5125.1136 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LU586 UT WOS:A1993LU58600022 PM 17790346 ER PT J AU MOHR, JJ FABRICANT, DG GELLER, MJ AF MOHR, JJ FABRICANT, DG GELLER, MJ TI AN X-RAY-METHOD FOR DETECTING SUBSTRUCTURE IN GALAXY CLUSTERS - APPLICATION TO PERSEUS, A2256, CENTAURUS, COMA, AND SERSIC 40/6 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERING; X-RAYS, GALAXIES ID RICH CLUSTERS; INTRACLUSTER MEDIUM; ABELL CLUSTERS; DARK MATTER; EVOLUTION; EINSTEIN; MORPHOLOGY; DYNAMICS; FIELD AB We use the moments of the X-ray surface brightness distribution to constrain the dynamical state of a galaxy cluster. Using X-ray observations from the Einstein Observatory Imaging Proportional Counter (IPC), we measure the first moment M1(rBAR), the ellipsoidal orientation angle theta2(rBAR), and the axial ratio eta(rBAR) at a sequence of radii in the cluster. We argue that a significant variation in the image centroid M1(rBAR) as a function of radius is evidence for a nonequilibrium feature in the intracluster medium (ICM) density distribution. In simple terms, centroid shifts indicate that the center of mass of the ICM varies with radius. This variation is a tracer of continuing dynamical evolution. For each cluster, we evaluate the significance of variations in the centroid of the IPC image by computing the same statistics on an ensemble of simulated cluster images. In producing these simulated images we include X-ray point source emission, telescope vignetting, Poisson noise, and characteristics of the IPC. Application of this new method to five Abell clusters (A426 [Perseus], A2256, A3526 [Centaurus], A1656 [Coma], and A3266 [Sersic 40/6]) reveals that the core of each one has significant substructure. In addition, we find significant variations in the orientation angle theta2(rBAR) and the axial ratio eta(rBAR) for several of the clusters. RP MOHR, JJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS-10,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 38 TC 154 Z9 154 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1993 VL 413 IS 2 BP 492 EP 506 DI 10.1086/173019 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LT200 UT WOS:A1993LT20000005 ER PT J AU GARAY, G MORAN, JM RODRIGUEZ, LF AF GARAY, G MORAN, JM RODRIGUEZ, LF TI COMPACT AMMONIA SOURCES TOWARD THE G10.5+0.0 H-II REGION COMPLEX SO ASTROPHYSICAL JOURNAL LA English DT Article DE H-II REGIONS; ISM, INDIVIDUAL (G10.5+0.0); ISM, KINEMATICS AND DYNAMICS; ISM, MOLECULES ID MOLECULAR CLOUDS; CORE; G10.6-0.4; G34.3+0.2; COLLAPSE AB We present observations of the (2, 2) and (3, 3) inversion transitions of ammonia toward a group of compact H II regions near l = 10-degrees.5, b = 0-degrees.0, made at 4'' resolution using the VLA. We detected three distinct ammonia sources in a region of approximately 2' in diameter. The densest and hottest cloud, having a line center velocity of 66.9 +/- 0.2 km s-1, is associated with the G 10.47 + 0.03 cluster of ultracompact H II regions. It exhibits a core-halo structure, with a core of approximately 0.08 pc in size surrounded by an envelope of approximately 0.25 pc in diameter. The peak optical depth in the main line of the (2, 2) and (3, 3) transitions are 25 and 37, respectively. The rotational temperature of the ammonia gas rises from -25 K in the outer parts of the halo to -75 K at the center of the core. The ammonia column density rises from approximately 4 x 10(17) cm-2 in the envelope region to approximately 4 x 10(18) cm-2 in the central position. The NH3 emission from the core region is remarkably broad in velocity; the line widths of the (2, 2) and (3, 3) main lines are 12.2 +/- 1.2 and 11.6 +/- 0.5 km s-1, respectively. The observed velocity structure of the ammonia emission indicates that the halo is slowly rotating, with an angular velocity of 9.5 +/- 1.1 km s-1 pc-1, while the gas in the core is undergoing rapid motions. A second cloud, having an angular size of approximately 13', a line center velocity of 71.3 +/- 0.2 km s-1, and a line width of 3.5 km s-1, is found toward the G10.46 + 0.03 complex region of ionized gas. It has a rotational temperature of 48 +/- 6 K and an NH3 column density of approximately 1 X 10(16) cm-2. The velocity structure of the ammonia emission suggests that this cloud is probably expanding, with a velocity of approximately 2 km s-1. The third cloud, at l = 10-degrees-48, b = 0.03-degrees, has a size of approximately 9'', a line center velocity of 65.4 +/- 0.9 km s-1, and a line width of 3.5 km s-1, and is not associated with any known radio continuum emission. It may represent a molecular core undergoing gravitational collapse in a stage prior to the formation of a star. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP GARAY, G (reprint author), UNIV CHILE,DEPT ASTRON,CASILLA 36-D,SANTIAGO,CHILE. RI Garay, Guido/H-8840-2013 OI Garay, Guido/0000-0003-1649-7958 NR 19 TC 13 Z9 14 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1993 VL 413 IS 2 BP 582 EP 592 DI 10.1086/173027 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LT200 UT WOS:A1993LT20000013 ER PT J AU CECCHIPESTELLINI, C DALGARNO, A AF CECCHIPESTELLINI, C DALGARNO, A TI EMISSION OF HEH+ IN NEBULAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, ABUNDANCES; MOLECULAR PROCESSES; PLANETARY NEBULAE, INDIVIDUAL (NGC-7027) ID MOLECULAR-HYDROGEN; HIGH-RESOLUTION; EXCITATION; NGC-7027; DISSOCIATION; MODEL; DUST; H-2 AB The formation and destruction processes of HeH+ in nebulae are discussed, and calculations of the abundances of HeH+ are presented. It is shown that for effective temperatures of the ionizing source exceeding 50,000 K, the abundances are of the order of 10(12) cm-2, largely independent of the nebular parameters. The emission-line intensities increase approximately as the density of the nebula. Results are given for two detailed models of the planetary nebula NGC 7027. The predicted intensities exceed the observational upper limit. The emissions have sharply peaked distributions with maximum intensity reached in a narrow zone at the edge of the ionized region. The greater art of the emission may be outside the region observed. C1 UNIV FLORENCE,DIPARTIMENTO ASTRON & SCI SPAZIO,I-50125 FLORENCE,ITALY. RP CECCHIPESTELLINI, C (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. OI Cecchi Pestellini, Cesare/0000-0001-7480-0324 NR 31 TC 27 Z9 27 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1993 VL 413 IS 2 BP 611 EP 618 DI 10.1086/173030 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LT200 UT WOS:A1993LT20000016 ER PT J AU GREENHOUSE, MA FELDMAN, U SMITH, HA KLAPISCH, M BHATIA, AK BARSHALOM, A AF GREENHOUSE, MA FELDMAN, U SMITH, HA KLAPISCH, M BHATIA, AK BARSHALOM, A TI INFRARED CORONAL EMISSION-LINES AND THE POSSIBILITY OF THEIR LASER-EMISSION IN SEYFERT NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Meeting Abstract C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,WASHINGTON,DC 20560. USN,RES LAB,SOLAR TERR RELATIONSHIPS BRANCH,WASHINGTON,DC 20375. USN,RES LAB,ARTEP INC,WASHINGTON,DC 20375. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NUCL RES CTR NEGEV,IL-84190 BEER SHEVA,ISRAEL. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1993 VL 413 IS 2 BP 834 EP 835 PN 1 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LT200 UT WOS:A1993LT20000038 ER PT J AU FANG, Z KWONG, VHS PARKINSON, WH AF FANG, Z KWONG, VHS PARKINSON, WH TI RADIATIVE LIFETIMES OF THE 2S2P(2)(P-4) METASTABLE LEVELS OF N-III SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC DATA; ATOMIC PROCESSES ID OUTER ATMOSPHERIC STRUCTURE; GIANT STARS; CONSTRAINTS; LINES; IONS; IUE AB The radiative decay rates of N III 175 nm intersystem lines have been measured in the laboratory by recording the time dependence of photon intensities emitted as the 2s2p(4P) metastable term of N2+ ions decay to the 2s(2)2p(P-2(o)) ground term. A cylindrical radio frequency ion trap was used to store the electron impact-produced N2+ ions. The radiative decay signals were analyzed by multiexponential least-squares fits to the data. The measured radiative decay rates to the ground term are 1019(+/-64) s-1 for P-4(1/2), 74.5(+/-5.4) s-1 for P-4(3/2), and 308(+/-22) s-1 for P-4(5/2). Comparisons of the measured values with theoretical values are presented. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 01238. RP FANG, Z (reprint author), UNIV NEVADA,DEPT PHYS,LAS VEGAS,NV 89154, USA. NR 21 TC 25 Z9 26 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 1993 VL 413 IS 2 BP L141 EP L144 DI 10.1086/186979 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LT202 UT WOS:A1993LT20200022 ER PT J AU TOWE, KM AF TOWE, KM TI PHOTOCHEMISTRY IN THE PRIMITIVE SOLAR NEBULA SO SCIENCE LA English DT Article ID EARTHS EARLY ATMOSPHERE; IRON-FORMATION; OXYGEN; CARBON; METHANE RP TOWE, KM (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. NR 25 TC 1 Z9 1 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD AUG 20 PY 1993 VL 261 IS 5124 BP 1058 EP 1059 DI 10.1126/science.261.5124.1058-a PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LT747 UT WOS:A1993LT74700039 PM 17739626 ER PT J AU WILLIAMS, EH BUNKLEYWILLIAMS, L GRIZZLE, JM PETERS, EC LIGHTNER, DV HARSHBARGER, J ROSENFIELD, A REIMSCHUESSEL, R AF WILLIAMS, EH BUNKLEYWILLIAMS, L GRIZZLE, JM PETERS, EC LIGHTNER, DV HARSHBARGER, J ROSENFIELD, A REIMSCHUESSEL, R TI EPIDEMIC MISUSE SO NATURE LA English DT Letter ID MASS MORTALITY; DIADEMA-ANTILLARUM; DISEASE; VIRUS C1 AUBURN UNIV,DEPT FISHERIES & APPL AQUACULTURE,AUBURN,AL 36849. TETRA TECH INC,FAIRFAX,VA 22030. UNIV ARIZONA,DEPT VET SCI,TUCSON,AZ 85721. SMITHSONIAN INST,REGISTRY TUMORS LOWER ANIM,WASHINGTON,DC 20560. OXFORD LAB,NE FISHERIES CTR,OXFORD,MD 21654. UNIV MARYLAND,SCH MED,DEPT PATHOL,TEACHING FACIL,BALTIMORE,MD 21201. RP WILLIAMS, EH (reprint author), UNIV PUERTO RICO,DEPT MARINE SCI,MARINE ECOL DISTURBANCE INFORMAT CTR,POB 908,LAJAS,PR 00667, USA. NR 16 TC 4 Z9 4 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD AUG 19 PY 1993 VL 364 IS 6439 BP 664 EP 664 DI 10.1038/364664c0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LT677 UT WOS:A1993LT67700016 PM 8355774 ER PT J AU WIKRAMANAYAKE, ED DRYDEN, GL AF WIKRAMANAYAKE, ED DRYDEN, GL TI THERMAL ECOLOGY OF HABITAT AND MICROHABITAT USE BY SYMPATRIC VARANUS-BENGALENSIS AND V-SALVATOR IN SRI-LANKA SO COPEIA LA English DT Article ID TEMPERATURE REGULATION; AUSTRALIA; LIZARDS; BIOLOGY; DIET AB Habitat and microhabitat use by Varanus bengalensis and V, salvator differ considerably; V. bengalensis ranged further inland from aquatic habitats than the semiaquatic V. salvator, which was found mostly in riparian and aquatic habitats. When active, V. bengalensis used warm, open microhabitats, but inactive animals either took refuge in structures such as tree hollows, termite mounds, and burrows or remained in microhabitats which provided some cover but little protective refuge. The temperatures in refuges were stable but lower than day-time air temperatures, whereas the temperatures in the latter microhabitats were unstable. The habitats and microhabitats of V. salvator were, however, thermally stable and cooler than microhabitats of active V. bengalensis. Varanus salvator also used burrows for refuge. The body temperatures of the two species reflected their differential use of thermal habitats and microhabitats; active V. bengalensis, which used warm open microhabitats, had a high active body temperature, but inactive animals in refuges had low body temperatures. Varanus salvator, which used cooler microhabitats during activity and inactivity, maintained a stable but low body temperature. Its body temperature also approximated the ambient temperatures in the riparian and aquatic habitats. Thus, the two species had different thermoregulatory behaviors which required use of habitats and microhabitats with different thermal regimes. RP WIKRAMANAYAKE, ED (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT HERPETOL,WASHINGTON,DC 20008, USA. NR 21 TC 7 Z9 11 U1 2 U2 7 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS BUSINESS OFFICE PI CARBONDALE PA SOUTHERN ILLINOIS UNIV, DEPT ZOOLOGY, CARBONDALE, IL 62901-6501 SN 0045-8511 J9 COPEIA JI Copeia PD AUG 18 PY 1993 IS 3 BP 709 EP 714 PG 6 WC Zoology SC Zoology GA LU363 UT WOS:A1993LU36300013 ER PT J AU STARNES, WC SCHINDLER, I AF STARNES, WC SCHINDLER, I TI COMMENTS ON THE GENUS APAREIODON EIGENMANN (CHARACIFORMES, PARODONTIDAE) WITH THE DESCRIPTION OF A NEW SPECIES FROM THE GRAN SABANA REGION OF EASTERN VENEZUELA SO COPEIA LA English DT Article AB The genus Apareiodon is diagnosed based on several derived features of the jaws, and a new species plus 13 nominal parodontid species are assigned to it. The new species is described from the Rio Caroni system in the Gran Sabana region of eastern Venezuela, a region of apparent endemism in fishes. RP STARNES, WC (reprint author), SMITHSONIAN INST,DIV FISHES,NHB WG-12,WASHINGTON,DC 20560, USA. NR 33 TC 7 Z9 7 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS BUSINESS OFFICE PI CARBONDALE PA SOUTHERN ILLINOIS UNIV, DEPT ZOOLOGY, CARBONDALE, IL 62901-6501 SN 0045-8511 J9 COPEIA JI Copeia PD AUG 18 PY 1993 IS 3 BP 754 EP 762 PG 9 WC Zoology SC Zoology GA LU363 UT WOS:A1993LU36300020 ER PT J AU FORREY, RC HILL, RN AF FORREY, RC HILL, RN TI COMPUTATION OF BETHE LOGARITHMS AND OTHER MATRIX-ELEMENTS OF ANALYTIC-FUNCTIONS OF OPERATORS SO ANNALS OF PHYSICS LA English DT Article ID MEAN EXCITATION-ENERGIES; HELIUM; CONVERGENCE; HYDROGEN; RATES C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. RP FORREY, RC (reprint author), UNIV DELAWARE,DEPT PHYS & ASTRON,NEWARK,DE 19716, USA. NR 46 TC 10 Z9 10 U1 0 U2 2 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0003-4916 J9 ANN PHYS-NEW YORK JI Ann. Phys. PD AUG 15 PY 1993 VL 226 IS 1 BP 88 EP 157 DI 10.1006/aphy.1993.1064 PG 70 WC Physics, Multidisciplinary SC Physics GA LQ523 UT WOS:A1993LQ52300002 ER PT J AU SCOTT, TC BABB, JF DALGARNO, A MORGAN, JD AF SCOTT, TC BABB, JF DALGARNO, A MORGAN, JD TI THE CALCULATION OF EXCHANGE FORCES - GENERAL RESULTS AND SPECIFIC MODELS SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MOLECULAR INTERACTION ENERGIES; PERTURBATION-THEORY; CONVERGENCE PROPERTIES; RAYLEIGH-SCHRODINGER; EXPANSION; BEHAVIOR; H2+ AB In order to clarify questions about the calculation of the exchange energy of a homonuclear molecular ion, an analysis is carried out of a model problem consisting of the one-dimensional limit of H-2+. It is demonstrated that the use of the infinite polarization expansion for the localized wave function in the Holstein-Herring formula yields an approximate exchange energy which at large internuclear distances R has the correct leading behavior to O(e(-R)) and is close to but not equal to the exact exchange energy. The extension to the n-dimensional double-well problem is presented. C1 UNIV OXFORD,INST MATH,OXFORD OX1 3LB,ENGLAND. UNIV DELAWARE,DEPT PHYS & ASTRON,NEWARK,DE 19716. RP SCOTT, TC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Babb, James/0000-0002-3883-9501 NR 31 TC 38 Z9 39 U1 1 U2 10 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD AUG 15 PY 1993 VL 99 IS 4 BP 2841 EP 2854 DI 10.1063/1.465193 PG 14 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA LR056 UT WOS:A1993LR05600057 ER PT J AU PIRAN, T SHEMI, A NARAYAN, R AF PIRAN, T SHEMI, A NARAYAN, R TI HYDRODYNAMICS OF RELATIVISTIC FIREBALLS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE HYDRODYNAMICS; RELATIVITY; GAMMA-RAYS, BURSTS ID GAMMA-RAY BURSTS; COSMIC FIREBALLS; BLAST WAVES; STARS AB Many models of gamma-ray bursts involve a fireball, which is an optically thick concentration of radiation energy with a high ratio of energy density to rest mass. We examine analytically and numerically the evolution of a relativistic fireball. We show that, after an early rearrangement phase, most of the matter and energy in the fireball is concentrated within a narrow shell. The shell propagates at nearly the speed of light, with a frozen radial profile, and according to a simple set of scaling laws. The spectrum of the escaping radiation is harder at early times and softer later on. Depending on the initial energy-to-mass ratio, the final outcome of a fireball is either photons with roughly the initial temperature or ultrarelativistic baryons. In the latter case, the energy could be converted back to gamma-rays via interaction with surrounding material. C1 HEBREW UNIV JERUSALEM,RACAH INST PHYS,JERUSALEM,ISRAEL. TEL AVIV UNIV,DEPT PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. RP PIRAN, T (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 16 TC 142 Z9 144 U1 0 U2 2 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 15 PY 1993 VL 263 IS 4 BP 861 EP 867 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LR838 UT WOS:A1993LR83800007 ER PT J AU PERIVOLAROPOULOS, L AF PERIVOLAROPOULOS, L TI STATISTICS OF MICROWAVE BACKGROUND FLUCTUATIONS INDUCED BY TOPOLOGICAL DEFECTS SO PHYSICAL REVIEW D LA English DT Article ID COLD-DARK-MATTER; LARGE-SCALE STRUCTURE; COSMIC-STRING EVOLUTION; GLOBAL TEXTURE; DENSITY PERTURBATIONS; GALAXY FORMATION; COBE; INFLATION; SIMULATIONS; ANISOTROPY AB We use the analytical model recently introduced by the author to investigate the statistics of temperature fluctuations on the cosmic microwave background induced by topological defects. The cases of cosmic strings and textures are studied. We derive analytically the characteristic function of the probability distribution for deltaT/T and use it to obtain the lowest twelve moments including the skewness and the kurtosis. The distribution function is also obtained and it is compared with the Gaussian distribution thus identifying long non-Gaussian tails. We show that for both cosmic strings and textures all odd moments (including skewness) vanish while the relative deviation from the Gaussian for even moments increases with the order of the moment. The non-Gaussian signatures of collapsing texture knots, derived from the distribution function and the moments, are found to be more prominent than the corresponding signatures for strings. We discuss the physical origin of this result. C1 BROWN UNIV,DEPT PHYS,PROVIDENCE,RI 02912. RP PERIVOLAROPOULOS, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,DIV THEORET ASTROPHYS,60 GADEN ST,CAMBRIDGE,MA 02138, USA. OI Perivolaropoulos, Leandros/0000-0001-9330-2371 NR 54 TC 44 Z9 44 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD AUG 15 PY 1993 VL 48 IS 4 BP 1530 EP 1538 DI 10.1103/PhysRevD.48.1530 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA LT880 UT WOS:A1993LT88000007 ER PT J AU SCHMIDT, BP KIRSHNER, RP EASTMAN, RG GRASHUIS, R DELLANTONIO, I CALDWELL, N FOLTZ, C HUCHRA, JP MILONE, AAE AF SCHMIDT, BP KIRSHNER, RP EASTMAN, RG GRASHUIS, R DELLANTONIO, I CALDWELL, N FOLTZ, C HUCHRA, JP MILONE, AAE TI THE UNUSUAL SUPERNOVA SN1993J IN THE GALAXY M81 SO NATURE LA English DT Article ID EXTRAGALACTIC DISTANCE SCALE; SN-1987A AB SUPERNOVA 1993J in the galaxy M81 is the second-brightest type II supernova observed this century, surpassed only by SN1987A in the Large Magellanic Cloud. Here we report the evolution of the photometric and spectral properties of SN1993J for the first 50 days following its discovery. The behaviour of this supernova is unusual, showing features typical of type II supernovae near the initial maximum, but with the strong helium lines characteristic of type Ib supernovae at later times. This implies that the progenitor star had an unusually thin hydrogen envelope (compared to normal type II progenitors), suggesting that significant mass loss had taken place before the explosion. Application of an expanding photosphere model1 to our data provides an estimate of the distance to the supernova of 2.6+/-0.4 Mpc, broadly consistent with the distance to M81 determined using Cepheid variable stars2. Supernova models that more closely match the atypical spectral features of SN1993J may change the inferred distance, and should provide better constraints on the structure of the progenitor. C1 UNIV CALIF SANTA CRUZ,LICK OBSERV,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. UNIV NEW MEXICO,INST ASTRON,ALBUQUERQUE,NM 87131. UNIV ARIZONA,STEWARD OBSERV,MMT OBSERV,TUCSON,AZ 85721. RP SCHMIDT, BP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 24 TC 64 Z9 65 U1 1 U2 2 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD AUG 12 PY 1993 VL 364 IS 6438 BP 600 EP 602 DI 10.1038/364600a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LR771 UT WOS:A1993LR77100043 ER PT J AU CURIR, A DIAFERIO, A DEFELICE, F AF CURIR, A DIAFERIO, A DEFELICE, F TI THE ANGULAR-MOMENTUM BEHAVIOR IN THE DISSIPATIONLESS COLLAPSE OF TRIAXIAL SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE CELESTIAL MECHANICS, STELLAR DYNAMICS; GALAXIES, ELLIPTIC AND LENTICULAR, CD; GALAXIES, FORMATION; GALAXIES, KINEMATICS AND DYNAMICS; METHODS, NUMERICAL ID MASSIVE BLACK-HOLES; INITIAL CONDITIONS; ELLIPTIC GALAXIES; SPHERICAL GALAXIES; HALOS; ROTATION; M31; NUCLEI; SHAPES AB We present N-body simulations of the collapse of six triaxial systems having the angular momentum aligned with one of their principal axes. Two different initial density distributions are chosen. The final relaxed states of the simulations show (1) a net outflow of angular momentum from the inner regions to the outer halo, consistent with the loss expected during the formation of elliptical galaxies; (2) a general misalignment of the average spin of the internal mass fractions with respect to that of the total system. Finally, some considerations are given concerning the occurrence of the necessary condition for the formation of a black hole at the center of these systems. C1 UNIV MILAN,DIPARTIMENTO FIS,I-20133 MILAN,ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV TURIN,IST FIS MATEMAT JL LAGRANGE,I-10123 TURIN,ITALY. RP CURIR, A (reprint author), OSSERV ASTRON TORINO,PINO TORINESE ITALY,STR OSSERV 20,I-10025 PINO,ITALY. OI Curir, Anna/0000-0002-2950-7097 NR 39 TC 20 Z9 20 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1993 VL 413 IS 1 BP 70 EP 78 DI 10.1086/172978 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LP771 UT WOS:A1993LP77100009 ER PT J AU HORA, JL DEUTSCH, LK HOFFMANN, WF FAZIO, GG SHIVANANDAN, K AF HORA, JL DEUTSCH, LK HOFFMANN, WF FAZIO, GG SHIVANANDAN, K TI NEAR-INFRARED AND MIDINFRARED IMAGING OF THE PLANETARY-NEBULAE BD +30-DEGREES-3639 AND IC-418 SO ASTROPHYSICAL JOURNAL LA English DT Article DE DUST, EXTINCTION; PLANETARY NEBULAE, INDIVIDUAL (BD + 30-DEGREES-3639, IC-418) ID POLYCYCLIC AROMATIC-HYDROCARBONS; EMISSION FEATURES; NEUTRAL HYDROGEN; SILICON-CARBIDE; DUST; CARBON; NGC-7027; GRAINS; STARS; SPECTROPHOTOMETRY AB We present near- and mid-infrared images of the planetary nebulae BD + 30-degrees-3639 and IC 418 with a unique combination of high spatial and spectral resolution. The mid-infrared images were obtained with MIRAC, a new IR array camera. For BD + 30-degrees-3639, the mid-IR images at 10.0, 11.2, 12.4, 12.8, and 13.2 mum have allowed us to separate the various spectral emission components such as the broad UIR features (perhaps from large molecular grains), the 12.8 mum [Ne II] emission feature, and continuum emission to determine the distribution of these components in the nebula. The derived temperature and opacity images show the detailed distribution of temperature and relative density of the dust. For IC 418, we have obtained high-resolution images in both the near- and mid-infrared. The images in the near-infrared at J, H, and K are important for determining the source of the IR excess; we have determined that one component of the excess is located near the central star and is possibly due to nonequilibrium heating of small grains. We have also imaged the halo emission at H and K, which has been detected in earlier studies, and have determined its spatial extent. The mid-IR images at 9.8 and 11.7 mum show continuum emission coincident with the ionized zone and suggest that silicon carbide emission originates from the region near the central star. C1 NASA,MOFFETT FIELD,CA 94035. UNIV CALIF BERKELEY,BERKELEY,CA 94720. STEWARD OBSERV,TUCSON,AZ 85721. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. GEN RES CORP,ARLINGTON,VA 22202. RP HORA, JL (reprint author), INST ASTRON,2680 WOODLAWN DR,HONOLULU,HI 96822, USA. OI Hora, Joseph/0000-0002-5599-4650 NR 51 TC 29 Z9 29 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1993 VL 413 IS 1 BP 304 EP 316 DI 10.1086/172998 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LP771 UT WOS:A1993LP77100029 ER PT J AU HABBAL, SR ESSER, R ARNDT, MB AF HABBAL, SR ESSER, R ARNDT, MB TI HOW RELIABLE ARE CORONAL HOLE TEMPERATURES DEDUCED FROM OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE SOLAR WIND; SUN, CORONA; SUN, UV RADIATION ID INNER SOLAR-WIND; SPECTRO-HELIOMETER; POLAR-REGION; ENERGY-FLOW; LINES; SUN; EMISSIVITIES; IONIZATION; MODEL; WAVES AB Given the importance of the temperature at the base of the corona for the modeling of the solar wind, we investigate the range of temperatures which have been deduced from remote measurements in coronal holes, within a heliocentric distance of 1.6 R(s), and the accuracy to which these temperatures have been inferred. We also present results of an analysis of extreme ultraviolet (EUV) observations made simultaneously in three spectral lines at the limb in a polar coronal hole, with very little contamination from quiet region emission along the line of sight. The values most commonly quoted for temperatures below 1.6 R(s) extend from 7 x 10(5) K to 1.6 x 10(6) K. However, by carefully reviewing the assumptions that enter into these inferences, we find that, within 1.6 R(s), the temperature in a coronal hole is at or below 1.3 x 10(6) K. Our own analysis yields a temperature range of 7.8-9.3 x 10(5) K, between 1.02 to 1.07 R(s) for the coronal hole, and a distinctly different temperature range of 9.4 x 10(5)-1.2 x 10(6) K for the quiet regions bordering it. Inhomogeneities within the coronal hole itself contribute to a 14% variation in its inferred temperature. Our results show that, from data currently available, temperatures in the inner corona cannot be derived with an accuracy better than 20%, even when neglecting many sources of uncertainty such as instrument calibration, line of sight effects, departure from ionization balance, and inaccuracies of the atomic data. We also show in this study that the elemental abundance, which is one of the parameters that influence the temperature inference, can in turn be significantly constrained when intensity ratios from three spectral lines are used. We find that, within the wide range of values quoted so far in the literature, the larger values of the abundance of O[log (A(O)) = 8.96], Ne[log (A(Ne)) = 8.2], and Mg[log (A(Mg)) = 7.65] [relative to hydrogen when log (A(H)) = 12], yield a self-consistent temperature. RP HABBAL, SR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 49 TC 66 Z9 66 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1993 VL 413 IS 1 BP 435 EP 444 DI 10.1086/173011 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LP771 UT WOS:A1993LP77100042 ER PT J AU MYERS, PC LADD, EF AF MYERS, PC LADD, EF TI BOLOMETRIC TEMPERATURES OF YOUNG STELLAR OBJECTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; HERTZSPRUNG-RUSSELL DIAGRAM; STARS, EVOLUTION ID MAIN-SEQUENCE STARS; T-TAURI STARS; AURIGA DARK CLOUDS; MOLECULAR CLOUD; PROTOSTARS; EVOLUTION; CORES AB We propose the '' bolometric temperature '' T(bol) as a measure of the circumstellar obscuration and evolutionary development of a young stellar object (YSO). T(bol) is the temperature of a blackbody having the same mean frequency as the observed continuum spectrum. A log-log plot of bolometric luminosity L(bol) versus T(bol) has the same main sequence as the Hertzsprung-Russell diagram, but for YSOs T(bol) can have much lower values (approximately 30 K) than can the photospheric temperature T(eff) (approximately 2800 K). We present three indications that a YSO evolves toward the main sequence from low to high T(bol) as a YSO clears its natal circumstellar dust: (1) For 129 YSOs in Taurus-Auriga, T(bol) ranges continuously from 60 to 5250 K, from '' protostars '' to '' classical '' T Tauri stars (CTTs) to '' weak-line '' T Tauri stars (WTTs), and a plot of L(bol) versus T(bol) terminates abruptly at the main sequence. (2) In T(eff) CTTs and WTTs are indistinguishable, with T(eff) approximately 4200 K, but in T(bol) WTTs are distinctly hotter (3600 K) than CTTs (2100 K). These temperatures indicate that circumstellar matter intercepts a larger fraction of the stellar luminosity for CTTs (0.5) than for WTTs (0.2). (3) In stellar groups, YSOs with low T(bol) are fewer and more concentrated, while YSOs with high T(bol) are more numerous and widespread. As T(bol) increases, an increasing fraction of YSOs lie outside a fiducial contour of (CO)-C-13 line emission: more than half the YSOs are excluded when T(bol) > 2500 K. Thus colder YSOs are probably younger, and hotter YSOs older, than the dispersal time for gas traced by the (CO)-C-13 line, estimated to be 1-3 Myr. C1 UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. RP MYERS, PC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 40 TC 149 Z9 149 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 1993 VL 413 IS 1 BP L47 EP L50 DI 10.1086/186956 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LP774 UT WOS:A1993LP77400012 ER PT J AU WAGNER, RH AF WAGNER, RH TI THE PURSUIT OF EXTRA-PAIR COPULATIONS BY FEMALE BIRDS - A NEW HYPOTHESIS OF COLONY FORMATION SO JOURNAL OF THEORETICAL BIOLOGY LA English DT Article ID SNIPE GALLINAGO-MEDIA; MIXED REPRODUCTIVE STRATEGY; GUILLEMOT URIA-AALGE; INFORMATION-CENTERS; SEXUAL SELECTION; TAENIOPYGIA-GUTTATA; PATERNITY ASSURANCE; NORTHERN FULMAR; MATING SYSTEMS; RAZORBILLS RP WAGNER, RH (reprint author), SMITHSONIAN INST,DEPT ZOOL RES,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 90 TC 87 Z9 88 U1 2 U2 15 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0022-5193 J9 J THEOR BIOL JI J. Theor. Biol. PD AUG 7 PY 1993 VL 163 IS 3 BP 333 EP 346 DI 10.1006/jtbi.1993.1123 PG 14 WC Biology; Mathematical & Computational Biology SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational Biology GA LZ936 UT WOS:A1993LZ93600003 ER PT J AU MARTIN, A AF MARTIN, A TI HAMMERHEAD SHARK ORIGINS SO NATURE LA English DT Letter RP MARTIN, A (reprint author), SMITHSONIAN TROP RES INST,NAOS MARINE LAB,POB 2072,BALBOA,PANAMA. NR 4 TC 19 Z9 19 U1 3 U2 13 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD AUG 5 PY 1993 VL 364 IS 6437 BP 494 EP 494 DI 10.1038/364494a0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LQ667 UT WOS:A1993LQ66700036 ER PT J AU KAEPPLER, AL AF KAEPPLER, AL TI POETICS AND POLITICS OF TONGAN LAMENTS AND EULOGIES SO AMERICAN ETHNOLOGIST LA English DT Article DE POETICS; POLITICS; AESTHETICS; ORATORY; SOCIAL STRUCTURE; LAMENT; EULOGY; TONGA; POLYNESIA ID RANK AB The aesthetic and political importance of oratory in Tongan laments and eulogies is the focus of this article. A series of historic poetic texts are presented as frames for an interpretation of the politics of prestige and power. These socially realized cultural constructions of emotion illustrate how written texts that are essentially oratorical are interpreted and explained in the oral tradition; how they impose knowledge about social order through an aesthetic medium that helps to create the shared values of the society; and how this essentially aristocratic art form serves as a mechanism for social distancing and control and the elevation of selected chiefly lineages. Spatial, temporal, and sound boundaries are related to social hierarchy, and poetic metaphor is shown to foreground and background the political importance of individuals and society. RP KAEPPLER, AL (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 33 TC 15 Z9 15 U1 0 U2 1 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0094-0496 J9 AM ETHNOL JI Am. Ethnol. PD AUG PY 1993 VL 20 IS 3 BP 474 EP 501 DI 10.1525/ae.1993.20.3.02a00020 PG 28 WC Anthropology SC Anthropology GA LW198 UT WOS:A1993LW19800002 ER PT J AU SAYRE, EV YENER, KA JOEL, EC AF SAYRE, EV YENER, KA JOEL, EC TI EVALUATING LEAD-ISOTOPE DATA - FURTHER OBSERVATIONS - COMMENTS .1. SO ARCHAEOMETRY LA English DT Note ID STATISTICAL EVALUATION; SURROUNDING REGIONS; ANATOLIA RP SAYRE, EV (reprint author), SMITHSONIAN INST,CTR MUSEUM SUPPORT,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. NR 4 TC 3 Z9 3 U1 0 U2 1 PU OXFORD UNIV PI OXFORD PA RES LAB ARCHAEOL HIST ART 6 KEBLE RD, OXFORD, ENGLAND OX1 3QJ SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD AUG PY 1993 VL 35 BP 247 EP 252 DI 10.1111/j.1475-4754.1993.tb01039.x PN 2 PG 6 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA PE885 UT WOS:A1993PE88500007 ER PT J AU VANDIVER, PB KAYLOR, R FEATHERS, J GOTTFRIED, M YENER, KA HORNYAK, WF FRANKLIN, A AF VANDIVER, PB KAYLOR, R FEATHERS, J GOTTFRIED, M YENER, KA HORNYAK, WF FRANKLIN, A TI THERMOLUMINESCENCE DATING OF A CRUCIBLE FRAGMENT FROM AN EARLY TIN PROCESSING SITE IN TURKEY SO ARCHAEOMETRY LA English DT Article DE TURKEY; THERMOLUMINESCENCE DATING; BRONZE; EARLY TIN MINING ID LEAD ISOTOPE; ANATOLIA; ORE AB Archaeological exploration in the Taurus mountains at Goltepe in south-central Turkey has uncovered a site indicating the presence of extensive tin ore mining and smelting operations. The most recent find of smelting crucible fragments allowed for a thermoluminescence-based age determination spanning a late fifth to early third millennium BC date. This result is consistent with a number of radiocarbon dates derived for charcoal also found at the site. The importance of this site relates to the possible tin production and subsequent trade with south-western Asia which would have provided this otherwise scarce ingredient to bronze technology in that area. This date is directly for crucible material and thus confirms the antiquity of tin smelting at Goltepe. C1 SMITHSONIAN INST,CTR MUSEUM SUPPORT,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560. RP VANDIVER, PB (reprint author), UNIV MARYLAND,DEPT PHYS,COLLEGE PK,MD 20742, USA. NR 9 TC 0 Z9 0 U1 0 U2 5 PU OXFORD UNIV PI OXFORD PA RES LAB ARCHAEOL HIST ART 6 KEBLE RD, OXFORD, ENGLAND OX1 3QJ SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD AUG PY 1993 VL 35 BP 295 EP 298 DI 10.1111/j.1475-4754.1993.tb01044.x PN 2 PG 4 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA PE885 UT WOS:A1993PE88500013 ER PT J AU CALDWELL, N ROSE, JA SHARPLES, RM ELLIS, RS BOWER, RG AF CALDWELL, N ROSE, JA SHARPLES, RM ELLIS, RS BOWER, RG TI STAR-FORMATION IN EARLY-TYPE GALAXIES IN THE COMA CLUSTER SO ASTRONOMICAL JOURNAL LA English DT Article ID EMISSION-LINE SPECTRA; MORPHOLOGICAL TYPES; RICH CLUSTERS; SPECTROSCOPY; PHOTOMETRY; EVOLUTION; REDSHIFT; POPULATIONS; PARAMETERS; MAGNITUDES AB We have obtained multifiber spectra of 125 early-type galaxies in the Coma cluster of galaxies, using the Hydra bench spectrograph on the 4 m telescope at Kitt Peak. The sample selection was based on both color and morphology, care being taken to exclude intermediate and late-type spirals. Surprisingly, a large fraction (about 1/3) of all galaxies in a field located approximately 40' SW of the center of the cluster exhibits enhanced Balmer absorption lines or emission lines, indicative of recent star formation or nuclear activity. In contrast, very few such galaxies are found in the central field of the cluster. Those galaxies with abnormal spectra cover a range in luminosity down to B almost-equal-to 19 (M(B) almost-equal-to -15). Furthermore, the bulk of the abnormal-spectrum galaxies are located near a secondary peak in the cluster x-ray emission found by Briel et al. [A&A, 259, L31 (1992)] and by Watt et al. [MNRAS, 258, 738 (1992)]. We argue by detailed comparisons with Kennicutt's [ApJS, 79, 255 (1992a)] sequence of normal spiral galaxy spectra that the anomalous spectral features cannot arise from morphological misindentifications. Specifically, the abnormal spectra are fundamentally different, with [O II] emission lines too weak for the enhanced Balmer absorption. The spectra are, however, remarkably similar to the red Hdelta-strong galaxies studied by Couch & Sharples [MNRAS, 229, 423 (1987)] in clusters at redshift z almost-equal-to 0.3 Hence it appears that an environmental process similar to that frequently found in clusters at moderate redshift is occurring at the present epoch in the outskirts of the Coma cluster. C1 SMITHSONIAN INST,FL WHIPPLE OBSERV,AMADO,AZ 85645. UNIV N CAROLINA,DEPT PHYS & ASTRON,CHAPEL HILL,NC 27599. UNIV DURHAM,DEPT PHYS,DURHAM DH1 3LE,ENGLAND. MAX PLANCK INST EXTRATERR PHYS,W-8046 GARCHING,GERMANY. NR 40 TC 166 Z9 166 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1993 VL 106 IS 2 BP 473 EP & DI 10.1086/116656 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LN790 UT WOS:A1993LN79000006 ER PT J AU EIROA, C LENZEN, R MIRANDA, LF TORRELLES, JM ANGLADA, G ESTALELLA, R AF EIROA, C LENZEN, R MIRANDA, LF TORRELLES, JM ANGLADA, G ESTALELLA, R TI OPTICAL AND NEAR-INFRARED OBSERVATIONS OF S-140N SO ASTRONOMICAL JOURNAL LA English DT Article ID HERBIG-HARO OBJECTS; OUTFLOW SOURCES AB Optical CCD images and polarimetry as well as near-IR observations of the molecular core S 140N are presented. The images reveal a reflection nebulosity associated with the young IRAS source 22178+6317. Two pointlike sources are embedded in the reflection nebulosity. The near-IR colors indicate an IR excess characteristic of PMS objects. The CO outflow detected in the region is likely to be driven by these young objects. Four Herbig-Haro objects are detected in our images. This is the first detection of these kinds of objects in the S 140 molecular cloud. The HH objects are aligned in a scale of almost-equal-to 2.5' (almost-equal-to 0.7 pc) and point to a faint star, located at the northern end of the brighter HH object This star is therefore a suitable candidate to excite the HH objects and is likely to be a T Tauri-like star. In addition, the star is centered on a previously detected ammonia core and likely heats the high density gas. Finally, these data show that not only high-mass stars, but also low-mass stars have recently formed in the S 140 molecular cloud. C1 MAX PLANCK INST ASTRON,W-6900 HEIDELBERG,GERMANY. UNIV COMPLUTENSE MADRID,FAC CIENCIAS FIS,DEPT ASTROFIS,E-28040 MADRID,SPAIN. INST ASTROFIS ANDALUCIA,E-18080 GRANADA,SPAIN. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV BARCELONA,DEPT ASTRON & METEOROL,E-08028 BARCELONA,SPAIN. RP EIROA, C (reprint author), UNIV AUTONOMA MADRID,FAC CIENCIAS,DEPT FIS TEOR,CANTOBLANCO,E-28049 MADRID,SPAIN. OI Torrelles, Jose Maria/0000-0002-6896-6085 NR 14 TC 7 Z9 7 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1993 VL 106 IS 2 BP 613 EP & DI 10.1086/116665 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LN790 UT WOS:A1993LN79000015 ER PT J AU ALONSO, MV DACOSTA, LN PELLEGRINI, PS KURTZ, MJ AF ALONSO, MV DACOSTA, LN PELLEGRINI, PS KURTZ, MJ TI CCD CALIBRATION OF THE MAGNITUDE SCALE FOR THE SOUTHERN SKY REDSHIFT SURVEY EXTENSION GALAXY SAMPLE SO ASTRONOMICAL JOURNAL LA English DT Article ID SURFACE PHOTOMETRY; REDUCTION AB In this paper we use new CCD observations to examine the accuracy of the magnitude system we have adopted to define the galaxy sample being used to conduct the Southern Sky Redshift Survey Extension hereafter referred to as (SSRS2). The magnitude scale of the SSRS2 is based on the instrumental magnitudes of the nonstellar objects listed in the ST ScI Guide Star Catalog, converted to the B(0) (Zwicky) system. This was done using a linear relation derived from the comparison of objects in common with the photometric catalogue of Lauberts & Valentijn [The Surface Photometry Catalogue of the ESO-Uppsala Galaxies (European Southern Observatory, Munchen) (1989)]. Using the results of new independent CCD observations we find: (1) the magnitudes derived by Lauberts & Valentijn are in excellent agreement with the CCD measurements, with isophotal magnitudes showing a dispersion of almost-equal-to 0.13 mag, although an offset 0.15 mag in zero point may be present; (2) the magnitudes M(SSRS2) derived from the ST ScI instrumental magnitudes correspond well to a blue magnitude measured within B=26 mag/arcsec2 isophote. These magnitudes have an intrinsic dispersion of about 0.34 mag, comparable to that estimated for the Zwicky system, and a relatively small plate-to-plate variation of the zero point. These results indicate that the ST ScI objects may provide an invaluable source for the construction of a uniform magnitude-limited sample of galaxies in the southern hemisphere. C1 OBSERV ASTRON,CORDOBA,ARGENTINA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP ALONSO, MV (reprint author), OBSERV NACL,RIO JANEIRO,BRAZIL. RI KURTZ, Michael /B-3890-2009; OI Kurtz, Michael/0000-0002-6949-0090 NR 18 TC 20 Z9 20 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 1993 VL 106 IS 2 BP 676 EP 686 DI 10.1086/116674 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LN790 UT WOS:A1993LN79000024 ER PT J AU LECACHEUX, A ROSOLEN, C DAVIS, M BOOKBINDER, J BASTIAN, TS DULK, GA AF LECACHEUX, A ROSOLEN, C DAVIS, M BOOKBINDER, J BASTIAN, TS DULK, GA TI DYNAMIC SPECTRA OF RADIO-SOURCES FROM 4.5 TO 5.0 GHZ SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE INSTRUMENTATION, SPECTROGRAPHS; SUN, RADIO RADIATION; AD LEO; STARS, FLARE; INTERPLANETARY MEDIUM; RADIO CONTINUUM, STARS ID AD-LEONIS; FLARES; BURSTS; SPIKES AB We report on the first observations of astronomical sources made with the mini-Gregorian feed of the 305 m Arecibo telescope together with an acousto-optic spectrometer (AOS). Both the mini-Gregorian and the AOS have a bandwidth of 500 MHz, permitting wide bandwidth dynamic spectra of both celestial and solar sources to be obtained. In the examples reported herein, we used the 5 GHz receiver, operating between 4.5 and 5.0 GHz with a spectral resolution of 1 MHz and temporal resolution of 20 ms. We represent observations of the flare star AD Leo, of the Sun, and of interplanetary scintillations of the quasar 0735 + 178 which, at the time it was observed, was about 8-degrees from the Sun. C1 NATL ASTRON & IONOSPHERE CTR, ARECIBO, PR 00613 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NATL RADIO ASTRON OBSERV, SOCORRO, NM 87801 USA. UNIV COLORADO, DEPT ASTROPHYS PLANETARY & ATMOSPHER SCI, BOULDER, CO 80309 USA. RP LECACHEUX, A (reprint author), OBSERV PARIS, RADIOASTRON DECAMETR GRP, F-92195 MEUDON, FRANCE. NR 14 TC 5 Z9 5 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 1993 VL 275 IS 2 BP 670 EP 678 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LT459 UT WOS:A1993LT45900036 ER PT J AU DAVID, LP SLYZ, A JONES, C FORMAN, W VRTILEK, SD ARNAUD, KA AF DAVID, LP SLYZ, A JONES, C FORMAN, W VRTILEK, SD ARNAUD, KA TI A CATALOG OF INTRACLUSTER GAS TEMPERATURES SO ASTROPHYSICAL JOURNAL LA English DT Article DE CATALOGS; GALAXIES, CLUSTERING; INTERGALACTIC MEDIUM; X-RAYS, GALAXIES ID X-RAY DATA; MEDIUM-SENSITIVITY SURVEY; LARGE-SCALE STRUCTURE; COLD DARK MATTER; GALAXY FORMATION; CLUSTERS; EVOLUTION; SAMPLE; MASS; EFFICIENCY AB We have searched the Einstein Monitor Proportional Counter (MPC) data base for observations of clusters of galaxies. The MPC was a nonfocal plane instrument on board the Einstein Observatory and accumulated data during all pointed observations with the four focal plane instruments. By co-adding the MPC spectra obtained during all pointed observations of clusters with IPC count rates greater than 0.1 counts per second, we have obtained sufficient photon statistics to estimate the X-ray temperature of 84 clusters. Combining the MPC results with EXOSAT and Ginga results reported in the literature yields a combined sample of 104 clusters with known X-ray temperatures. This is approximately twice as large as any previously published sample. One of the best studied X-ray correlations between clusters is that between their X-ray luminosity and gas temperature. We show that the best-fit power-law relation for our combined cluster sample can be explained by the observed increase in the gas-to-stellar mass ratio between low- and high-temperature clusters. There have been several recent reports in the literature concerning the evolution of X-ray luminous clusters at fairly low redshifts. The statistical significance of any evolution in our combined X-ray sample has been examined and compared with the statistical properties of clusters culled from optical catalogs. We find that there is strong evidence for a decrease in the X-ray luminosity of optically rich clusters beyond z almost-equal-to 0.06. This result is used to estimate the normalization of the primordial power spectrum of density fluctuations. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. UNIV MARYLAND,DEPT ASTRON,COLL PK,MD 20742. RP DAVID, LP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 48 TC 451 Z9 452 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1993 VL 412 IS 2 BP 479 EP 488 DI 10.1086/172936 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LN831 UT WOS:A1993LN83100003 ER PT J AU SCHACHTER, JF STOCKE, JT PERLMAN, E ELVIS, M REMILLARD, R GRANADOS, A LUU, J HUCHRA, JP HUMPHREYS, R URRY, CM WALLIN, J AF SCHACHTER, JF STOCKE, JT PERLMAN, E ELVIS, M REMILLARD, R GRANADOS, A LUU, J HUCHRA, JP HUMPHREYS, R URRY, CM WALLIN, J TI 10 NEW BL LACERTAE OBJECTS DISCOVERED BY AN EFFICIENT X-RAY RADIO OPTICAL TECHNIQUE SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL LACERTAE OBJECTS, GENERAL; GALAXIES, ACTIVE; GALAXIES, NUCLEI; METHODS, OBSERVATIONAL; X-RAYS, GALAXIES; SURVEYS ID LUMINOSITY FUNCTION; SKY SURVEY AB We report the recent discovery of 10 BL Lac objects in the Einstein IPC Slew Survey by means of X-ray/radio versus X-ray/optical color-color diagrams and confirming optical spectroscopy. These 10 BL Lac objects were discovered using a technique proposed by Stocke et al. which exploits the characteristic broad-band spectra of BL Lac objects. New VLA detections provide accurate fluxes [limiting f(6 cm) approximately 0.5 mJy] and approximately 1'' positions, facilitating the determination of an optical counterpart. All 10 new BL Lac objects show essentially featureless optical spectra and lie within the range of radio/X-ray/optical colors of known X-ray-selected BL Lac objects, when approximately 1 mag optical variability is included. We expect approximately 50 new BL Lac objects in total, from complete optical follow-up of our now completed VLA work and recent Australia Telescope observations, yielding a complete Slew Survey sample of approximately 90 BL Lac objects. C1 UNIV COLORADO,DEPT APAS,BOULDER,CO 80309. RP SCHACHTER, JF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS 4,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Urry, Claudia/G-7381-2011; OI Urry, Claudia/0000-0002-0745-9792; Perlman, Eric/0000-0002-3099-1664 NR 26 TC 93 Z9 94 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1993 VL 412 IS 2 BP 541 EP 549 DI 10.1086/172942 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LN831 UT WOS:A1993LN83100009 ER PT J AU BIRKINSHAW, M WORRALL, DM AF BIRKINSHAW, M WORRALL, DM TI THE X-RAY STRUCTURE AND SPECTRUM OF NGC-6251 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (NGC-6251); GALAXIES, JETS; GALAXIES, NUCLEI; RADIATION MECHANISMS, MISCELLANEOUS; X-RAYS, GALAXIES ID EARLY-TYPE GALAXIES; EXTRAGALACTIC RADIO-SOURCES; ELLIPTICAL GALAXIES; HIGH-RESOLUTION; M87 JET; ENVIRONMENTS; MORPHOLOGY; EMISSION; NUCLEUS; DENSITY AB NGC 6251 has been observed in low-energy X-rays with the Position Sensitive Proportional Counter on board ROSAT. No X-ray emission is seen from the 45 long radio jet of this galaxy, suggesting that the electron spectrum is cut off for electron energies greater than E(max) almost-equal-to 10(12) eV, but a bright X-ray source is coincident with the center of the galaxy. Most of the counts in this source are in a component of small angular size, FWHM < 4'', corresponding to a linear size less than 3 kpc, although there is evidence for the presence of a low surface brightness halo with FWHM approximately 3'. If this halo is thermal bremsstrahlung of gas near NGC 6251, this gas cannot confine the arcminute-scale radio jet by simple (static) gas pressure. The spectrum of the X-ray core source in NGC 6251 is a bad match to a single-component thermal model and, when fitted by a simple power-law model, requires the presence of an absorbing column far in excess of the Galactic or intrinsic columns. The nuclear spectrum can be well fitted by a composite model with two (or more) different components: a plausible decomposition consists of a flat-spectrum (energy index alpha(x) almost-equal-to 0.27) power-law component from a mini-active galactic nucleus (AGN) plus an 0.5 keV thermal component. The power-law spectral index is close to the high-frequency radio spectral index of the VLBI core, supporting a synchro-self-Compton model for this component of the X-ray emission. The temperature of the thermal component is characteristic of the temperatures of gas found in other elliptical galaxies, and the ps must be in a cooling flow. The infall of material into the nucleus is sufficiently rapid to power the mini-AGN component, if the mass of the central black hole exceeds 5 x 10(4) M.. Unification schemes that relate BL Lac objects and radio galaxies (e.g., Padovani & Urry 1990) require a component of unbeamed X-ray emission: it is possible that the type of thermal gas that we find in NGC 6251 may produce the necessary unbeamed X-ray com ponent. RP BIRKINSHAW, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 51 TC 76 Z9 76 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1993 VL 412 IS 2 BP 568 EP 585 DI 10.1086/172944 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LN831 UT WOS:A1993LN83100011 ER PT J AU CHRISTODOULOU, DM AF CHRISTODOULOU, DM TI THE STABILITY OF ACCRETION TORI .5. UNSTABLE MODES AND AVOIDED CROSSINGS IN EXTENDED, SELF-GRAVITATING ANNULI SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; HYDRODYNAMICS; INSTABILITIES; STARS, FORMATION ID DIFFERENTIALLY ROTATING-DISKS; NON-LINEAR EVOLUTION; DYNAMICAL STABILITY; NONAXISYMMETRIC INSTABILITIES; 3-DIMENSIONAL SIMULATIONS; ANGULAR-MOMENTUM; VERSATILE METHOD; T-TAURI; FRAGMENTATION; SLENDER AB We continue a study of the dynamical evolution of two-dimensional, differentially rotating, self-gravitating annuli by investigating systems having arbitrarily large radial thickness and orbiting around a central mass. Such extended annuli are idealized models of thick, pressure-supported accretion disks. The initial axisymmetric equilibria are cylindrical with well-defined inner and outer edges, compressible with polytropic index n = 1, and have constant specific anagular momentum. Linear growth rates and eigenfunction characteristics of the different modes are calculated through a solution of the linearized fluid and Poisson equations. Some model evolutions have also been carried into the nonlinear regime using a two-dimensional, Eulerian hydro code that is second-order-accurate in both space and time. As we abandon the quasi-Cartesian, slender-annulus approximation, several new features are revealed by the stability analysis, most of which were unexpected. (1) In contrast to the results obtained for slender annuli, the I mode instability survives in purely self-gravitating extended annuli without a central mass. Furthermore, this mode is not symmetric across the pressure maximum but has corotation only in the vicinity of the outer edge. These results are in agreement with previous three-dimensional calculations of self-gravitating tori. (2) Neutral acoustic modes and neutral gravity modes undergo deflections called ''avoided crossings'' right outside the outer edge. This type of mode interaction has been previously identified in solar/stellar oscillation theory. (3) Such deflected modes enter the fluid where they intersect with acoustic modes and produce sequences of short, weakly unstable branches different in character from ''conventional'' edge modes and rather similar to the I modes. Because of the presence of a strong I mode with m = 1 (which distorts these extended systems), the weakly unstable modes are not expected to be dominant. (4) Besides the I mode, the P and J modes also exist in these systems. As is already known, the P and J modes dominate for low and high degrees of self-gravity, respectively. In addition, J modes appear only in radially slender systems. (5) As soon as the P mode disappears with self-gravity, ''conventional'' edge modes become dominant before the I mode appears. In contrast to the I and J modes of slender systems, these edge modes as well as the P modes do not appear capable of breaking the annulus. Instead, they only stir up the fluid and result in the appearance of distinct inhomogeneities (edge modes) or spiral shocks (P mode). (6) Surprisingly, all annuli are stable against infinitesimal axisymmetric perturbations. Consequently, cylindrical annuli do not obey Toomre's local stability criterion derived for differentially rotating sheets. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 51 TC 9 Z9 9 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1993 VL 412 IS 2 BP 696 EP 719 DI 10.1086/172955 PN 1 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LN831 UT WOS:A1993LN83100022 ER PT J AU EASTMAN, RG PINTO, PA AF EASTMAN, RG PINTO, PA TI SPECTRUM FORMATION IN SUPERNOVAE - NUMERICAL TECHNIQUES SO ASTROPHYSICAL JOURNAL LA English DT Article DE LINE, FORMATION; METHODS, NUMERICAL; RADIATIVE TRANSFER; SUPERNOVAE, GENERAL ID MULTILEVEL RADIATIVE-TRANSFER; APPROXIMATE LAMBDA-OPERATORS; LINE FORMATION; QUADRATURE PERTURBATIONS; SOBOLEV APPROXIMATION; ITERATION METHOD; COMOVING-FRAME; ATMOSPHERES; SCATTERING; CONTINUUM AB We have combined several novel techniques for spectrum simulation in the computer program EDDINGTON which solves the comoving frame equation of transfer coupled with the statistical and radiative equilibrium equations. The first of these is a generalization of the accelerated lambda iteration (ALI) scheme to include an approximate frequency-derivative operator. This greatly enhances the convergence rate of ALI in optically thick, high-velocity shear flows. The next is a partial linearization technique which is capable of efficiently solving a very large (approximately 10(4)) number of rate equations on a moderately sized computer; part of its efficiency derives from a '' fixed-excitation '' iteration which allows this technique to handle simulations with a large number of (intrinsically) overlapping lines and continua. Finally, we derive an expansion opacity and emissivity approximation which allows us to determine the effect on the transfer and statistical equilibrium of a very large number of lines not explicitly represented in the frequency grid and additionally to treat line-blanketing from species not explicitly included in the rate equations. We illustrate the utility of these techniques with models of two supernovae. The first is a typical Type II supernova 45 days past explosion which illustrates the power of the ALI scheme for optically thick problems in rapidly moving flows. The second is a Type la supernova 250 days past explosion which demonstrates the ability of partial linearization and the expansion opacity/emissivity approximation to treat a problem with 727 atomic energy levels coupled by all continua and 4447 lines. For each we discuss rates of convergence and the effect of various convergence-accelerating techniques. Detailed models of various supernovae and the microphysics (e.g., energy deposition and atomic data) we employ will be discussed in future publications. C1 UNIV CALIF SANTA CRUZ,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP EASTMAN, RG (reprint author), UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064, USA. NR 56 TC 81 Z9 81 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 1993 VL 412 IS 2 BP 731 EP 751 DI 10.1086/172957 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LN831 UT WOS:A1993LN83100024 ER PT J AU BALSER, EJ RUPPERT, EE JAECKLE, WB AF BALSER, EJ RUPPERT, EE JAECKLE, WB TI ULTRASTRUCTURE OF THE COELOMS OF AURICULARIA LARVAE (HOLOTHUROIDEA, ECHINODERMATA) - EVIDENCE FOR THE PRESENCE OF AN AXOCOEL SO BIOLOGICAL BULLETIN LA English DT Article ID NEPHRIDIA AB A hallmark feature of echinoderm larvae is the development of the left anterior coelom. This coelom, called the axohydrocoel, consists of the morphologically distinct, but undivided, left axocoel and hydrocoel. The axocoelic portion forms a duct that opens to the exterior via a pore on the dorsal surface of the animal. Holothuroid larvae are thought to lack an axocoel, but develop an.anterior coelom, duct, and pore that are regarded as parts of the hydrocoel. New ultrastructural data, however, show that holothuroid auricularia larvae possess an axocoel and hydrocoel united together into an axohydrocoel. During development the anterior coelom consists of an interconnected left somatocoel, hydrocoel, and axocoel. The left somatocoel separates from the axohydrocoel and subdivides into left and right somatocoels. The somatocoels and hydrocoel region of the axohydrocoel are lined by a monociliated mesothelium having characteristics of transporting epithelia. The axocoel epithelium, like that of asteroid larvae, is composed of mesothelial podocytes. A duct connects the axocoel directly to the open dorsal pore and is lined with a columnar transporting epithelium. The occurrence of a specialized podocyte-lined cavity between the surface pore and the hydrocoel in echinoderm larvae is indicative of an axocoel. That similar structures occur in auricularia larvae supports the identification of an axocoel in holothuroids. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. RP BALSER, EJ (reprint author), CLEMSON UNIV,DEPT BIOL SCI,132 LONG HALL,CLEMSON,SC 29634, USA. NR 19 TC 13 Z9 14 U1 0 U2 2 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA BIOLOGICAL BULL MBL STREET, WOODS HOLE, MA 02543 SN 0006-3185 J9 BIOL BULL JI Biol. Bull. PD AUG PY 1993 VL 185 IS 1 BP 86 EP 96 DI 10.2307/1542132 PG 11 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA LT687 UT WOS:A1993LT68700008 ER PT J AU TOWE, KM AF TOWE, KM TI ENVIRONMENTAL-IMPACT SO GEOTIMES LA English DT Letter RP TOWE, KM (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER GEOLOGICAL INST PI ALEXANDRIA PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 SN 0016-8556 J9 GEOTIMES JI Geotimes PD AUG PY 1993 VL 38 IS 8 BP 3 EP 3 PG 1 WC Geosciences, Multidisciplinary SC Geology GA LQ875 UT WOS:A1993LQ87500003 ER PT J AU ROBINSON, MS MOUGINISMARK, PJ ZIMBELMAN, JR WU, SSC ABLIN, KK HOWINGTONKRAUS, AE AF ROBINSON, MS MOUGINISMARK, PJ ZIMBELMAN, JR WU, SSC ABLIN, KK HOWINGTONKRAUS, AE TI CHRONOLOGY, ERUPTION DURATION, AND ATMOSPHERIC CONTRIBUTION OF THE MARTIAN VOLCANO APOLLINARIS-PATERA SO ICARUS LA English DT Article ID OLYMPUS MONS; ALBA-PATERA; MARS; EVOLUTION; ELYSIUM; TOPOGRAPHY; DEPOSITS; WATER; ICE C1 SMITHSONIAN INST,CEPS,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560. US GEOL SURVEY,ASTROGEOL BRANCH,FLAGSTAFF,AZ 86001. RP ROBINSON, MS (reprint author), UNIV HAWAII,SOEST,DEPT GEOL & GEOPHYS,2525 CORREA RD,HONOLULU,HI 96822, USA. NR 75 TC 46 Z9 46 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD AUG PY 1993 VL 104 IS 2 BP 301 EP 323 DI 10.1006/icar.1993.1103 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LY532 UT WOS:A1993LY53200012 ER PT J AU JOHNSTON, PF ROBINSON, DS AF JOHNSTON, PF ROBINSON, DS TI THE WRECK OF THE 1848 PROPELLER INDIANA - INTERIM-REPORT SO INTERNATIONAL JOURNAL OF NAUTICAL ARCHAEOLOGY LA English DT Article C1 TEXAS A&M UNIV,NAUT ARCHAEOL PROGRAM,COLL STN,TX 77843. RP JOHNSTON, PF (reprint author), SMITHSONIAN INST,NMAH-5010,MRC 628,WASHINGTON,DC 20560, USA. NR 18 TC 4 Z9 4 U1 0 U2 0 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0305-7445 J9 INT J NAUT ARCHAEOL JI Int. J. Naut. Archaeol. PD AUG PY 1993 VL 22 IS 3 BP 219 EP & DI 10.1006/ijna.1993.1005 PG 0 WC Archaeology SC Archaeology GA MX997 UT WOS:A1993MX99700006 ER PT J AU SUN, Y DALGARNO, A AF SUN, Y DALGARNO, A TI EXCITATION OF 2 O((1)D) ATOMS IN THE COLLISION OF GROUND-STATE OXYGEN-ATOMS SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ENERGETIC O+ PRECIPITATION; RYDBERG STATE; PREDISSOCIATION; ATMOSPHERE; O2 AB The collisional process (O(P))-P-3 + (O(P))-P-3 --> O(1D) + O(1D) is investigated. It is found that the excitation cross section is comparable to that of the single-excitation process (O(P))-P-3 + (O(P))-P-3 --> (O(P))-P-3 + O(1D). The process enhances the intensity of the 6300-angstrom red line emission arising from the deposition into the atmosphere of energetic O+ ions which undergo charge transfer to produce fast oxygen atoms. RP SUN, Y (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 11 TC 1 Z9 1 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES JI J. Geophys. Res-Space Phys. PD AUG 1 PY 1993 VL 98 IS A8 BP 13715 EP 13716 DI 10.1029/93JA01031 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LR054 UT WOS:A1993LR05400046 ER PT J AU RILEY, S AF RILEY, S TI THE DISSOLUTION OF DEE,NICHOLAS - HIS RESEARCHES - STADLER,M SO LIBRARY JOURNAL LA English DT Book Review RP RILEY, S (reprint author), SMITHSONIAN INST LIBS,WASHINGTON,DC, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU BOWKER MAGAZINE GROUP CAHNERS MAGAZINE DIVISION PI NEW YORK PA 249 W 17TH ST, NEW YORK, NY 10011 SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 1993 VL 118 IS 13 BP 156 EP 156 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA LT263 UT WOS:A1993LT26300335 ER PT J AU MESSIER, P VITALE, T AF MESSIER, P VITALE, T TI CRACKING IN ALBUMIN PHOTOGRAPHS - AN ESEM INVESTIGATION SO MICROSCOPY RESEARCH AND TECHNIQUE LA English DT Article DE CONSERVATION; WATER; RELATIVE HUMIDITY; CRACKING AB The preservation of nineteenth-century albumen prints is of great concern to collection managers and to conservators of photographic materials. In the field of art conservation, preservation techniques incorporating aqueous treatments are often used to enhance the long- and short-term stability of historical artifacts or art objects. In a study of the interaction of water with albumen photographs, experiments were carried out in the ESEM to follow the real time effects of water on the prints. The experiments were designed to observe the effects of a range of relative humidities and liquid water on samples of expendable historic albumen prints, utilizing the advantages of imaging in the presence of water vapor. All albumen photographs exhibit a fine network of cracks in the albumen protein layer. Average crack width is approximately 10 mum. As observed in the ESEM, a 4.25-fold increase in the width of a single crack (at 50% RH), viewed normal to the surface, resulted from a single controlled excursion to high relative humidity and immersion. In an extraordinary series of images, a print viewed in cross-section exhibited a 22% swelling and shrinkage in thickness, and a 5% and 9% swelling and shrinkage along the width of a fragment of the albumen/image layer when the sample was immersed in water and dried. The visual information gained through the use of the ESEM helped to focus a materials investigation and served as a foundation for a study which shows that aqueous treatment causes increased cracking of both unsupported albumen and the albumen/image layer in prints. (C) 1993 Wiley-Liss, Inc. C1 SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560. RP MESSIER, P (reprint author), ROCKY MT CONSERVAT CTR,2420 S UNIV BLVD,DENVER,CO 80203, USA. NR 11 TC 20 Z9 20 U1 1 U2 4 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 1059-910X J9 MICROSC RES TECHNIQ JI Microsc. Res. Tech. PD AUG PY 1993 VL 25 IS 5-6 BP 374 EP 383 DI 10.1002/jemt.1070250505 PG 10 WC Anatomy & Morphology; Biology; Microscopy SC Anatomy & Morphology; Life Sciences & Biomedicine - Other Topics; Microscopy GA LN846 UT WOS:A1993LN84600004 PM 8400428 ER PT J AU FRYE, BL BECHTOLD, J MOUSTAKAS, LA DOBRZYCKI, A AF FRYE, BL BECHTOLD, J MOUSTAKAS, LA DOBRZYCKI, A TI ABSORPTION-SPECTRA OF Q-0000-263 AND 1442+101 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE INTERGALACTIC MEDIUM; QUASARS ABSORPTION LINES; QUASARS INDIVIDUAL 0000-263; QUASARS INDIVIDUAL 1442+101 ID LYMAN-ALPHA-FOREST; REDSHIFT EVOLUTION; CLOUDS; LINES; QSOS; RESOLUTION; SYSTEMS; ABUNDANCES AB We present a new analysis of the Ly alpha forest for the high-redshift QSOs 1442 + 101 (z = 3.544) and 0000 - 263 (z = 4.11 1). We have performed detailed profile fitting to spectra of moderate resolution and high signal-to-noise ratio. The results are compared to a more conventionally derived line list. As a result, we provide a high-redshift extension to the previously reported Ly a forest samples of Bajtlik, Duncan & Ostriker, Lu, Wolfe & Turnshek and Rauch et al. If the evolution of the number of lines per unit redshift has the functional form (1 + z) gamma then we find a best-fitting value of gamma = 2.5 9 +/- 0.49 for an equivalent width completeness limit of W(thr) = 0.21 angstrom. If the equivalent widths are distributed as exp(- W/W*), we determine a characteristic equivalent width W* = 0.084 +/-0.008 for the new data. Relating this to a column density distribution of the form p(N(H1) is-proportional-to N(H1)-beta we find that beta almost-equal-to 1.9. The new data combined with the Rauch et al. sample give W* = 0. 1 79 +/- 0.0 1 0, which corresponds to beta almost-equal-to 1.7. Our values for W* and beta imply that the new data are not consistent with the typical intermediate-resolution sample. The larger values that we have determined for beta are, however, consistent with high-resolution spectra. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,HARVARD OBSERV,CAMBRIDGE,MA 02138. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. NICHOLAS COPERNICUS ASTRON CTR,WARSAW,POLAND. RP FRYE, BL (reprint author), UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721, USA. NR 26 TC 9 Z9 9 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 1993 VL 263 IS 3 BP 575 EP 588 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LP311 UT WOS:A1993LP31100008 ER PT J AU DALPINO, EMD OPHER, R AF DALPINO, EMD OPHER, R TI ARE THE FILAMENTS FORMED BY SYNCHROTRON THERMAL-INSTABILITY BRIGHT SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE HYDRODYNAMICS; INSTABILITIES; RADIATION MECHANISMS MISCELLANEOUS; GALAXIES JETS ID CENTAURUS-A; RADIO-SOURCES; HIGH-RESOLUTION; JET; ORIGIN; M87; EMISSION; KNOTS AB Previous analyses of the formation of filaments by the synchrotron-inverse-Compton thermal instability (STI) have assumed a relativistic Maxwellian distribution of electrons, rather than a power-law distribution as observed. In these analyses, the hypothesis of a monoenergetic spectrum does not permit determination of the true evolution of the volume emissivity as a function of the spectral luminosity in the filament. It is thus not possible to conclude whether the filaments formed by STI, such as in supernova remnants and extragalactic radio lobes and jets, are effectively bright or dark compared to the adjacent ambient region when observed at a given frequency. Since this question of the brightness of the synchrotron thermal filaments relative to the ambient medium has caused some controversy in the literature, we here abandon the assumption of a monoenergetic electron distribution and study STI by considering a power-law electron distribution obtained from the observed spectral luminosity. As an example, the data of luminosity (versus frequency), pressure and density of the inner 40-arcsec Centaurus jet are used. Curves of volume emissivity versus frequency indicate that filaments formed by STI are brighter than the adjacent unperturbed regions for almost the entire frequency range, in agreement with observations. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP DALPINO, EMD (reprint author), UNIV SAO PAULO,INST ASTRON & GEOFIS,AV MIGUEL STEFANO 4200,BR-04301 SAO PAULO,BRAZIL. RI de Gouveia Dal Pino, Elisabete/H-9560-2013 OI de Gouveia Dal Pino, Elisabete/0000-0001-8058-4752 NR 24 TC 5 Z9 5 U1 0 U2 1 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 1993 VL 263 IS 3 BP 687 EP 694 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LP311 UT WOS:A1993LP31100018 ER PT J AU MAZEH, T KRYMOLOWSKI, Y LATHAM, DW AF MAZEH, T KRYMOLOWSKI, Y LATHAM, DW TI STUDIES OF MULTIPLE STELLAR-SYSTEMS .1. THE HALO STAR G38-13 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE CELESTIAL MECHANICS, STELLAR DYNAMICS; BINARIES SPECTROSCOPIC; STARS INDIVIDUAL G38-13 ID PROPER-MOTION STARS; 40 SPECTROSCOPIC BINARIES; TIME-SERIES ANALYSIS; PLANETARY SYSTEM; 3RD STAR; ORBITS; PSR1257+12; TRIPLE AB We report the discovery of the spectroscopic triple system G38-13. Its outer orbit has one of the shortest known periods, 645 d, for a late-type triple system. The shortness of the outer period, and the small ratio of the periods of the outer and the inner orbits, 28: 1, make this system very interesting for the study of long-term modulations of the orbital elements of triple systems. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MAZEH, T (reprint author), TEL AVIV UNIV,SCH PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. NR 28 TC 15 Z9 15 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG 1 PY 1993 VL 263 IS 3 BP 775 EP 780 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LP311 UT WOS:A1993LP31100026 ER PT J AU FANG, Z KWONG, VHS WANG, JB PARKINSON, WH AF FANG, Z KWONG, VHS WANG, JB PARKINSON, WH TI MEASUREMENTS OF RADIATIVE-DECAY RATES OF THE 2S(2)2P(P-2(0))-2S2P(2)(P-4) INTERSYSTEM TRANSITIONS OF C-II SO PHYSICAL REVIEW A LA English DT Article ID OUTER ATMOSPHERIC STRUCTURE; GIANT STARS; IONS; CONSTRAINTS; SPECTRUM; LINES; IUE AB The radiative-decay rates of the 2s(2)2p(P-2degrees)-2s2p2(4P) intersystem transitions of C+ ions have been measured by recording the time dependence of the approximately 233-nm emission. A cylindrical radio-frequency ion trap was used to store electron-impact-produced C+ ions. The time-dependent signals were analyzed by multiexponential least-squares fits to the data. The measured radiative-decay rates to the ground term are 146.4(+8.3,-9.2) s-1 for P-4(1/2), 11.6(+0.8,-1.7) s-1 for P-4(3/2), and 51.2(+2.6,-3.5) s-1 for P-4(5/2). Comparison of the measured values with theoretical values is presented. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP FANG, Z (reprint author), UNIV NEVADA,DEPT PHYS,LAS VEGAS,NV 89154, USA. NR 27 TC 34 Z9 34 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD AUG PY 1993 VL 48 IS 2 BP 1114 EP 1122 DI 10.1103/PhysRevA.48.1114 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LQ990 UT WOS:A1993LQ99000033 ER PT J AU ZOTZ, G WINTER, K AF ZOTZ, G WINTER, K TI SHORT-TERM PHOTOSYNTHESIS MEASUREMENTS PREDICT LEAF CARBON BALANCE IN TROPICAL RAIN-FOREST CANOPY PLANTS SO PLANTA LA English DT Article DE CARBON DIOXIDE ASSIMILATION; PHOTOSYNTHESIS (CANOPY); TROPICAL RAIN FOREST ID WATER AB Diel (24 h) courses of net CO2 exchange of leaves were determined in eight species of tropical rain-forest plants on Barro Colorado Island, Panama, during 1990 and 1991. The species included three canopy trees, one liana, two epiphytes and one hemiepiphyte. One of the species studied was growing in a rain-forest gap. Daily carbon gain varied considerably across species, leaf age, and season. The analysis of data for all plants from 64 complete day/night cycles revealed a linear relationship between the diurnal carbon gain and the maximum rate of net CO2 uptake, A(max). Nocturnal net carbon loss was about 10% of diurnal carbon gain and was positively related to A(max). We conclude that short-term measurements of light-saturated photosynthesis, performed at periodic intervals throughout the season, allow the annual leaf carbon balance in these rain-forest plants to be predicted. C1 SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. NR 16 TC 32 Z9 34 U1 0 U2 3 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0032-0935 J9 PLANTA JI Planta PD AUG PY 1993 VL 191 IS 3 BP 409 EP 412 PG 4 WC Plant Sciences SC Plant Sciences GA ME166 UT WOS:A1993ME16600016 ER PT J AU CLAYTON, GC WHITNEY, BA MATTEI, JA AF CLAYTON, GC WHITNEY, BA MATTEI, JA TI LONG-TERM VARIATIONS IN DUST PRODUCTION IN R-CORONAE-BOREALIS SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID STARS; FADINGS AB Several searches for periodicities in the historical visible light curves of RCB stars have found that the intervals between declines are random. This paper reexamines 70 declines of R Coronae Borealis since 1853 using one homogeneous data set, the AAVSO light curve. In this data set, pairs of consecutive declines also show a random distribution of intervals. However, if the sequence of declines is examined, there are semiperiodic variations between times of high- and low-decline activity on a time scale of a few years. Near-IR photometry of RCB stars indicates that there are large semiperiodic variations in the amount of dust being produced which have similar time scales. Possible interpretations of a semiperiodic variation in dust formation rates in RCB stars are as follows: (i) A magnetic activity cycle resulting in ''spots'' on the star over which dust formation takes place. Such a magnetic activity cycle is similar to the solar cycle; (ii) changes in the period and amplitude of the pulsations over several years affecting the efficiency of dust production. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. AMER ASSOC VARIABLE STAR OBSERVERS,CAMBRIDGE,MA 02138. RP CLAYTON, GC (reprint author), UNIV COLORADO,CTR ASTROPHYS & SPACE ASTRON,CAMPUS BOX 389,BOULDER,CO 80309, USA. NR 35 TC 11 Z9 11 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD AUG PY 1993 VL 105 IS 690 BP 832 EP 835 DI 10.1086/133240 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LW251 UT WOS:A1993LW25100004 ER PT J AU KUMAR, M STELBOVICS, AT WILLIAMS, JF AF KUMAR, M STELBOVICS, AT WILLIAMS, JF TI CIRCULAR-POLARIZATION OF THE 3D STATE OF ATOMIC-HYDROGEN EXCITED BY ELECTRONS SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID ANGULAR-CORRELATION MEASUREMENTS; PHOTON COINCIDENCE EVENTS; IMPACT EXCITATION; 32DJ STATES; RADIATION; HELIUM; COLLISIONS; REGION AB The theory of the circular polarization from the 3(2)D state is analysed and angular correlation formulae are derived for the scattered n = 3 electron and the cascade Lyman-alpha radiation. The formulae include allowance for the polarization of the intermediate-state 2p electron from the LS coupling in the time evolution of the decay of the collisionally excited n = 3(2)D states. The effect of a finite coincidence time window is also examined. The predictions of the model are compared with the model which assumes that the intermediate-state 2p electron is unpolarized. New experimental data at an incident electron kinetic energy of 54.4 eV are reported and indicate the circular polarization of the Lyman-alpha radiation has small negative values from 10-degrees to 120-degrees. The theoretical predictions of the correlation are illustrated in a six-state close-coupling model which gives a minimum at forward angles but does not agree quantitatively with the experimental data. C1 UNIV WESTERN AUSTRALIA,CTR ATOM MOLEC & SURFACE PHYS,DEPT PHYS,PERTH 6009,AUSTRALIA. HARVARD SMITHSONIAN CTR ASTROPHYS,ITAMP,CAMBRIDGE,MA 02138. RP KUMAR, M (reprint author), MURDOCH UNIV,SCH MATH & PHYS SCI,CTR ATOM MOLEC & SURFACE PHYS,PERTH 6150,AUSTRALIA. NR 26 TC 11 Z9 11 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD JUL 28 PY 1993 VL 26 IS 14 BP 2165 EP 2177 DI 10.1088/0953-4075/26/14/016 PG 13 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LR830 UT WOS:A1993LR83000016 ER PT J AU RAYMOND, JC AF RAYMOND, JC TI A MODEL OF AN X-RAY ILLUMINATED ACCRETION DISK AND CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; BINARIES, CLOSE; RADIATION MECHANISM, MISCELLANEOUS; X-RAYS, STARS ID COMPTON HEATED WINDS; SCORPIUS X-1; CROSS-SECTIONS; MULTIWAVELENGTH CAMPAIGN; ULTRAVIOLET-SPECTRUM; CYGNUS X-2; IUE; IONIZATION; EMISSION; SHELL AB The X-ray-illuminated surface of the accretion disk in a low-mass X-ray Binary (LMXRB) and the X-ray-heated corona above the disk produce optical, UV, and soft X-ray emission lines. This paper presents one-dimensional models of the emission line spectra and the vertical temperature and density structures at different radii. The models include a detailed treatment of the important atomic processes and an escape probability treatment of radiative transfer. A companion paper (Soker & Raymond) uses the density structure predicted by these models for a two-dimensional Monte Carlo simulation of the photon scattering in the accretion disk corona (ADC) to examine the effects of the ADC on the angular distribution of X-rays and the flux of X-rays incident on the outer disk. This paper concentrates on the emission line fluxes for various elemental abundances and disk parameters. The UV lines of the classic LMXRBs are consistent with the model predictions. Some CNO processing is necessary to account for the nitrogen and helium abundances in Sco X-1 and other LMXRBs. Comparison of the models with observed spectra also points to a soft X-ray component with luminosity comparable to the hard X-rays. The models predict a substantial luminosity in the group of highly ionized iron lines near 100 angstrom. They also predict a significant zone where cooling by atomic processes dominates Compton heating and cooling, and the temperature is a fraction of the Compton temperature. RP RAYMOND, JC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 55 TC 94 Z9 94 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1993 VL 412 IS 1 BP 267 EP 277 DI 10.1086/172917 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LM214 UT WOS:A1993LM21400022 ER PT J AU STRACHAN, L KOHL, JL WEISER, H WITHBROE, GL MUNRO, RH AF STRACHAN, L KOHL, JL WEISER, H WITHBROE, GL MUNRO, RH TI A DOPPLER DIMMING DETERMINATION OF CORONAL OUTFLOW VELOCITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE SOLAR WIND; SUN, CORONA; SUN, PARTICLE EMISSION; SUN, UV RADIATION ID ALPHA FLUX; POLARIZATION; LINE; HOLE AB Outflow velocities in a polar coronal hole are derived from observations made during a 1982 sounding rocket flight. The velocity results are derived from a Doppler dimming analysis of resonantly scattered H I Lyalpha. This analysis indicates radial outflow velocities of 217 km s-1 at 2 R. from Sun-center with an uncertainty range of 153 to 251 km s-1 at a confidence level of 67%. These results are best characterized as strong evidence for supersonic outflow within 2 R. of Sun-center in a polar coronal hole. Several means for obtaining improved accuracy in future observations are discussed. C1 BALL AEROSP SYST GRP,BOULDER,CO 80306. RP STRACHAN, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 25 TC 51 Z9 51 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 1993 VL 412 IS 1 BP 410 EP 420 DI 10.1086/172930 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LM214 UT WOS:A1993LM21400035 ER PT J AU MOLLAAGHABABA, R GOTTLIEB, CA VRTILEK, JM THADDEUS, P AF MOLLAAGHABABA, R GOTTLIEB, CA VRTILEK, JM THADDEUS, P TI MILLIMETER-WAVE SPECTRUM OF VIBRATIONALLY EXCITED CYCLOPROPENYLIDENE, C-C3H2 SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID MOLECULAR LINE SURVEY; SAGITTARIUS B2; ORION-A; C3H2; SPECTROSCOPY; GHZ; IDENTIFICATION; RING AB The millimeter-wave rotational spectrum of c-C3H2 in four vibrationally excited states was measured and the rotational and quartic centrifugal distortion constants determined. Of the vibrational states observed here, only nu3 has been previously detected in the infrared. Assignment of the three new states to nu6, nu5, and nu2 was based on relative intensities, comparison of calculated and measured inertial defects, and symmetry considerations. The spectroscopic constants determined will guide future infrared investigation of c-C3H2, needed for a complete elucidation of the vibrational structure of this molecule. The experimental values of the vibration-rotation coupling constants will allow comparison with theoretical calculations that have recently become feasible for molecules of similar size as c-C3H2. Detection in space of rotational lines from the lowest vibrationally excited states may be possible. C1 HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MOLLAAGHABABA, R (reprint author), HARVARD UNIV,DEPT PHYS,CAMBRIDGE,MA 02138, USA. NR 36 TC 10 Z9 10 U1 3 U2 4 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 15 PY 1993 VL 99 IS 2 BP 890 EP 896 DI 10.1063/1.465353 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA LM894 UT WOS:A1993LM89400013 ER PT J AU CHEUNG, ASC MOK, DKW JAMIESON, MJ FINCH, M YOSHINO, K DALGARNO, A PARKINSON, WH AF CHEUNG, ASC MOK, DKW JAMIESON, MJ FINCH, M YOSHINO, K DALGARNO, A PARKINSON, WH TI ROTATIONAL DEPENDENCE OF THE PREDISSOCIATION LINEWIDTHS OF THE SCHUMANN-RUNGE BANDS OF O2 SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ISOTOPIC OXYGEN MOLECULES; ABSORPTION-BANDS; O-16 O-18; NM AB The predissociation linewidths of vibrational levels nu = 0 - 12 for O-16(2), O-16O-18, and O-18(2) molecules in the B2SIGMA(u)- state with rotational quantum numbers N less-than-or-equal-to 20 have been calculated taking into account the spin-orbit interactions of the B3SIGMA(u)- state with the 5PI(u), 3SIGMA(u)+, 3PI(u), and 1PI(u) states, and the rotational coupling with the 3PI(u) state. The predissociation linewidths exhibit systematic variations with rotational quantum number for different vibrational levels. Good agreement between most of the calculated and experimental linewidths has been obtained for all three isotopic molecules, with the exception of the set of linewidths of O-16(2) for nu = 0 and 2. The agreement can be improved by adjustment of the 1PI(u) potential and the strength of the spin-orbit interaction between the B3SIGMA(u)- and 1PI(u) states. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. GEORGIA INST TECHNOL,DEPT COMP SCI,ATLANTA,GA 30332. RP CHEUNG, ASC (reprint author), UNIV HONG KONG,DEPT CHEM,HONG KONG,HONG KONG. RI Mok, Daniel Kam-Wah/K-5826-2013 OI Mok, Daniel Kam-Wah/0000-0002-6677-2949 NR 24 TC 16 Z9 16 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 15 PY 1993 VL 99 IS 2 BP 1086 EP 1092 DI 10.1063/1.466204 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA LM894 UT WOS:A1993LM89400034 ER PT J AU YI, I VISHNIAC, ET AF YI, I VISHNIAC, ET TI SIMPLE ESTIMATE OF THE STATISTICS OF LARGE-SCALE STRUCTURE SO PHYSICAL REVIEW D LA English DT Note ID INFLATIONARY UNIVERSE; FLUCTUATIONS AB We examine the low order moments of inflationary density fluctuations in simple scalar field inflationary models. Using observational constraints on the average amplitude of cosmological density fluctuations we constrain the size of any possible non-Gaussian effects. We find that they are small (with a skewness less than approximately 10(-6) and a kurtosis less than approximately 10(-12)). We show that these results are consistent with previous work based on a stochastic model for the evolution of the inflaton field distribution. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP YI, I (reprint author), UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712, USA. OI Vishniac, Ethan/0000-0002-2307-3857 NR 23 TC 3 Z9 3 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD JUL 15 PY 1993 VL 48 IS 2 BP 950 EP 953 DI 10.1103/PhysRevD.48.950 PG 4 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA LN084 UT WOS:A1993LN08400059 ER PT J AU MARVIN, UB AF MARVIN, UB TI TO A ROCKY MOON - A GEOLOGISTS HISTORY OF LUNAR EXPLORATION - WILHELMS,DE SO SCIENCE LA English DT Book Review RP MARVIN, UB (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD JUL 9 PY 1993 VL 261 IS 5118 BP 231 EP 234 DI 10.1126/science.261.5118.231 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LL596 UT WOS:A1993LL59600045 PM 17829280 ER PT J AU DALGARNO, A AF DALGARNO, A TI THE CHEMISTRY OF ASTRONOMICAL ENVIRONMENTS SO JOURNAL OF THE CHEMICAL SOCIETY-FARADAY TRANSACTIONS LA English DT Article; Proceedings Paper CT 28TH FARADAY SYMP ON CHEMISTRY IN THE INTERSTELLAR MEDIUM CY DEC 16-18, 1992 CL UNIV BIRMINGHAM, BIRMINGHAM, ENGLAND HO UNIV BIRMINGHAM ID DENSE INTERSTELLAR CLOUDS; CANDIDATE IRAS F10214+4724; TIME-DEPENDENT CHEMISTRY; INTER-STELLAR SHOCKS; GAS-PHASE PRODUCTION; MOLECULAR CLOUDS; INFRARED-SPECTRUM; CARBON-MONOXIDE; PHOTODISSOCIATION REGIONS; ULTRAVIOLET-RADIATION AB Beginning with the chemistry of the early Universe, a review is presented of the chemistry of astronomical environments beyond the solar system with a particular emphasis on the interstellar medium. The ion-molecule chemistry of a quiescent interstellar cloud is summarized and modifications arising from intense radiation fields and shocks associated with star formation are discussed. The influence of grain chemistry is noted. The formation of molecules in the ejecta of Supernova 1987A is described. The fundamental role of chemistry in stellar and galactic formation and evolution is emphasized. RP DALGARNO, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 106 TC 39 Z9 39 U1 0 U2 3 PU ROYAL SOC CHEMISTRY PI CAMBRIDGE PA THOMAS GRAHAM HOUSE, SCIENCE PARK MILTON ROAD, CAMBRIDGE, CAMBS, ENGLAND CB4 4WF SN 0956-5000 J9 J CHEM SOC FARADAY T JI J. Chem. Soc.-Faraday Trans. PD JUL 7 PY 1993 VL 89 IS 13 BP 2111 EP 2117 DI 10.1039/ft9938902111 PG 7 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA LM947 UT WOS:A1993LM94700001 ER PT J AU RAVENHILL, PL AF RAVENHILL, PL TI 'MINING THE MUSEUM' SO AFRICAN ARTS LA English DT Art Exhibit Review RP RAVENHILL, PL (reprint author), SMITHSONIAN INST,NATL MUSEUM AFRIC ART,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD JUL PY 1993 VL 26 IS 3 BP 72 EP 73 DI 10.2307/3337154 PG 2 WC Art SC Art GA LR800 UT WOS:A1993LR80000010 ER PT J AU STAPLES, AJ AF STAPLES, AJ TI 'IN AND OUT OF AFRICA' - BARBASH,I, TAYLOR,L SO AFRICAN ARTS LA English DT Film Review RP STAPLES, AJ (reprint author), SMITHSONIAN INST,NATL MUSEUM AFRIC ART,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD JUL PY 1993 VL 26 IS 3 BP 75 EP & DI 10.2307/3337157 PG 0 WC Art SC Art GA LR800 UT WOS:A1993LR80000013 ER PT J AU ROMOLI, M WEISER, H GARDNER, LD KOHL, JL AF ROMOLI, M WEISER, H GARDNER, LD KOHL, JL TI STRAY-LIGHT SUPPRESSION IN A REFLECTING WHITE-LIGHT CORONAGRAPH SO APPLIED OPTICS LA English DT Article DE CORONAGRAPH; POLARIMETER; STRAY LIGHT ID POLARIZATION AB An analysis of stray-light suppression in the white-light channel of the Ultraviolet Coronagraph Spectrometer experiment for the Solar and Heliospheric Observatory is reported. The white-light channel consists of a reflecting telescope with external and internal occultation and a polarimeter section. Laboratory tests and analytical methods are used to perform the analysis. The various stray-light contributions are classified in two main categories: the contribution from sunlight that passes directly through the entrance aperture and the contribution of sunlight that is diffracted by the edges of the entrance aperture. Values of the stray-light contributions from various sources and the total stray-light level for observations at heliocentric heights from 1.4 to 5 solar radii are derived. Anticipated signal-to-stray-light ratios are presented together with the effective stray-light rejection by the polarimeter, demonstrating the efficacy of the stray-light suppression design. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP ROMOLI, M (reprint author), UNIV FLORENCE, DIPARTIMENTO ASTRON & SCI SPAZIO, LARGO FERMI 5, I-50125 FLORENCE, ITALY. RI Romoli, Marco/H-6859-2012 NR 25 TC 21 Z9 21 U1 0 U2 2 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0003-6935 J9 APPL OPTICS JI Appl. Optics PD JUL 1 PY 1993 VL 32 IS 19 BP 3559 EP 3569 PG 11 WC Optics SC Optics GA LK405 UT WOS:A1993LK40500031 PM 20829981 ER PT J AU SPINRAD, H FILIPPENKO, AV YEE, HKC ELLINGSON, E BLADES, JC BAHCALL, JN JANNUZI, BT BECHTOLD, J DOBRZYCKI, A AF SPINRAD, H FILIPPENKO, AV YEE, HKC ELLINGSON, E BLADES, JC BAHCALL, JN JANNUZI, BT BECHTOLD, J DOBRZYCKI, A TI HYDROGEN AND METAL ABSORPTION-LINES IN PKS 0405-123 FROM THE HALOS OF LOW-REDSHIFT GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article ID SYSTEM AB Hubble Space Telescope ultraviolet spectra and ground-based optical spectra of the bright quasar PKS 0405-123 are used to identify two absorption-line systems probably produced by the halos of foreground galaxies. The quasar lies in a rich galaxy field. Loose groups of galaxies are present in the field at [z1] = 0.1669 and [z2] = 0.3519. Ly alpha, C IV lambda1549, and probably Mg II lambda2798 resonance lines are detected in an absorption system at z = 0.1670. An absorption system consisting of only Ly alpha is observed at z = 0.3516. We cannot be completely certain which foreground galaxy is responsible for the metal line absorption system at z1. A likely candidate is a large, luminous, early-type spiral 40'' (projected distance 78h-1 kpc) to the east of the quasar. However, the origin of the z1 system could possibly be a small, undetected galaxy more precisely aligned along our line of sight to PKS 0405 - 123, or a very faint galaxy whose redshift has not yet been measured. C1 UNIV TORONTO,DEPT ASTRON,TORONTO M5S 1A7,ONTARIO,CANADA. UNIV COLORADO,CASA,BOULDER,CO 80309. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. INST ADV STUDY,SCH NAT SCI,PRINCETON,NJ 08540. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP SPINRAD, H (reprint author), UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720, USA. NR 20 TC 33 Z9 33 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 1993 VL 106 IS 1 BP 1 EP 5 DI 10.1086/116614 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LJ882 UT WOS:A1993LJ88200001 ER PT J AU STAUFFER, JR PROSSER, CF GIAMPAPA, MS SODERBLOM, DR SIMON, T AF STAUFFER, JR PROSSER, CF GIAMPAPA, MS SODERBLOM, DR SIMON, T TI LITHIUM AND CHROMOSPHERIC ACTIVITY IN THE ALPHA-PERSEI CLUSTER SO ASTRONOMICAL JOURNAL LA English DT Article ID LOWER-MAIN-SEQUENCE; SOLAR-TYPE STARS; LOW-MASS STARS; HYADES; EMISSION; ROTATION; EVOLUTION AB We have obtained high resolution spectra of a set of proposed members of the Alpha Persei open cluster which had previously been shown to have anomalously low lithium abundances. We have used the new spectra to derive Ca II emission strengths, radial velocities, and reddening estimates in order to assess whether these stars truly are members of the Alpha Per cluster. We conclude that most of the weak lithium stars are indeed bonafide cluster members, and thus the problem of explaining their anomalous lithium abundances remains. We have also obtained spectra for another sample of stars for which the previous membership data were relatively limited. Most of these stars do not appear to be members of the cluster. C1 NATL OPT ASTRON OBSERV,NATL SOLAR OBSERV,TUCSON,AZ 85726. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. RP STAUFFER, JR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 21 TC 19 Z9 19 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 1993 VL 106 IS 1 BP 229 EP 235 DI 10.1086/116630 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LJ882 UT WOS:A1993LJ88200017 ER PT J AU DOBRZYCKA, D KENYON, SJ MIKOLAJEWSKA, J AF DOBRZYCKA, D KENYON, SJ MIKOLAJEWSKA, J TI SPECTROSCOPIC OBSERVATIONS OF V443 HERCULIS - A SYMBIOTIC BINARY WITH A LOW-MASS WHITE-DWARF SO ASTRONOMICAL JOURNAL LA English DT Article ID INHOMOGENEOUS-MEDIUM; STELLAR EVOLUTION; COOL COMPONENTS; PLANETARY-NEBULAE; ANGULAR-MOMENTUM; M-GIANTS; STARS; ACCRETION; GALAXY; S0-GALAXIES AB We present an analysis of new and existing photometric and spectroscopic observations of the symbiotic binary V443 Herculis. This binary system consists of a normal M5 giant (M(g) approximately 2.5M.) and a hot, compact star (M(h) approximately 0.4M.). These two objects have comparable luminosities: L(g) approximately 1500 L. and L(h) approximately 1000L. for an adopted distance of 2 kpc. We identify three nebular regions in this binary: a small, highly ionized volume surrounding the hot component, a modestly ionized shell close to the red giant photosphere, and a less dense region of intermediate ionization encompassing both binary components. The system parameters for V443 Her suggest the hot component currently declines from a symbiotic nova eruption. C1 COPERNICUS ASTRON CTR,PL-00176 WARSAW,POLAND. RP DOBRZYCKA, D (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 89 TC 24 Z9 24 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 1993 VL 106 IS 1 BP 284 EP 297 DI 10.1086/116636 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LJ882 UT WOS:A1993LJ88200023 ER PT J AU GARAY, G RUBIO, M RAMIREZ, S JOHANSSON, LEB THADDEUS, P AF GARAY, G RUBIO, M RAMIREZ, S JOHANSSON, LEB THADDEUS, P TI MOLECULAR CLOUDS IN THE 30-DORADUS HALO SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE INTERSTELLAR MEDIUM, CLOUDS; INTERSTELLAR MEDIUM, MOLECULES; INTERSTELLAR MEDIUM, 30-DOR (LMC); GALAXIES, MAGELLANIC CLOUDS; GALAXIES, ISM; RADIO LINES, GALAXIES ID LARGE MAGELLANIC CLOUD; 30 DORADUS NEBULA; H-II REGIONS; STAR FORMATION; SUPERNOVA-REMNANTS; LINE; EMISSION; GALAXIES; WIDTH; MASS AB Using the Columbia telescope we mapped with high sensitivity (0.02 K in radiation temperature) the CO(1 --> 0) line emission from a region of 1.0-degrees x 0.75-degrees in size, centered near the 30 Doradus Nebula of the Large Magellanic Cloud. Most of the emission arises from six well discernable molecular clouds, with radii between 60 and 160 pc and luminosities between 1 X 10(4) and 6 X 10(4) K km s-1 pc2. The CO brightness temperature and luminosity of these clouds are significantly weaker than those of Galactic molecular clouds with similar linear dimensions. The proportionality factor between the total column density of gas, N(H-2 + 2H), and the velocity integrated CO intensity for the 30 Doradus halo clouds is approximately 13 times larger than that for molecular complexes of similar size in the inner Galaxy, and approximately 2 times larger than the average value for clouds in the LMC. The strongest CO emission, although very weak compared with that of Galactic clouds, is associated with the 30 Doradus Nebula. The bulk of the molecular gas is at the heliocentric velocity of 265 km s-1, essentially equal to the mean velocity of both the stellar component and of the ionized gas in that region. This result, together with the low brightness temperature of the CO emission, suggests that the CO emission arises from small molecular clumps embedded in a region filled mainly by ionized gas and also possible by atomic gas where CO is photodissociated. Toward the Doradus Nebula there is also CO emission that is redshifted with respect to the main component, which we suggest arises from molecular gas that has been accelerated by the stellar winds from the many hot stars in that region. C1 ONSALA SPACE OBSERV, S-43992 ONSALA, SWEDEN. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP GARAY, G (reprint author), UNIV CHILE, DEPT ASTRON, CASILLA 36-D, SANTIAGO, CHILE. RI Garay, Guido/H-8840-2013 OI Garay, Guido/0000-0003-1649-7958 NR 35 TC 21 Z9 21 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 1993 VL 274 IS 3 BP 743 EP 751 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LP334 UT WOS:A1993LP33400009 ER PT J AU KRICHBAUM, TP ZENSUS, JA WITZEL, A MEZGER, PG STANDKE, KJ SCHALINSKI, CJ ALBERDI, A MARCAIDE, JM ZYLKA, R ROGERS, AEE BOOTH, RS RONNANG, BO COLOMER, F BARTEL, N SHAPIRO, II AF KRICHBAUM, TP ZENSUS, JA WITZEL, A MEZGER, PG STANDKE, KJ SCHALINSKI, CJ ALBERDI, A MARCAIDE, JM ZYLKA, R ROGERS, AEE BOOTH, RS RONNANG, BO COLOMER, F BARTEL, N SHAPIRO, II TI 1ST 43 GHZ VLBI DETECTION OF THE COMPACT SOURCE SGR-A-ASTERISK IN THE GALACTIC-CENTER SO ASTRONOMY & ASTROPHYSICS LA English DT Letter DE THE GALACTIC-CENTER INTERFEROMETRY JETS OF GALAXIES ID RADIO-SOURCE AB The Galactic Center radio source Sgr A* was detected for the first time with VLBI at 43 GHz. Observations made with four antennas of the Very Long Baseline Array suggest a size of the source exceeding that of a scatter-broadened unresolved object by a factor of 2-3. The data indicate that the structure is elongated along P.A. = -25 +/- 10-degrees. A first image was made, with an angular resolution of - 1 mas (corresponding to 8.5 AU at r0 = 8.5 kpc). C1 INST RADIOASTRON MILLIMETRIQUE, GRENOBLE, FRANCE. CSIC, INST ASTROFIS ANDALUCIA, GRANADA, SPAIN. NEROC, HAYSTACK OBSERV, WESTFORD, MA USA. ONSALA SPACE OBSERV, ONSALA, SWEDEN. YORK UNIV, N YORK, ON, CANADA. NATL RADIO ASTRON OBSERV, SOCORRO, NM 87801 USA. UNIV VALENCIA, VALENCIA, SPAIN. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP KRICHBAUM, TP (reprint author), MAX PLANCK INST RADIOASTRON, HUGEL 69, D-53121 BONN, GERMANY. NR 18 TC 39 Z9 39 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 1993 VL 274 IS 3 BP L37 EP L40 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LP334 UT WOS:A1993LP33400002 ER PT J AU JORGENSEN, I FRANX, M KJAERGAARD, P AF JORGENSEN, I FRANX, M KJAERGAARD, P TI SOURCES OF SCATTER IN THE FUNDAMENTAL PLANE AND THE DN-SIGMA RELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERING; GALAXIES, DISTANCES AND REDSHIFTS; GALAXIES, ELLIPTIC AND LENTICULAR, CD; GALAXIES, FUNDAMENTAL PARAMETERS; GALAXIES, PHOTOMETRY ID ELLIPTICAL GALAXIES; PHOTOMETRY; SPECTROSCOPY; PARAMETERS; CLUSTERS; MOTION AB On the basis of new photometric data for early-type galaxies in the Coma Cluster we have determined the relation log r(e) = a log sigma + b[mu]e + c known as the fundamental plane (FP). The scatter in the FP is equivalent to 11% uncertainty on distances. The residuals for the FP show no dependence on other available photometric and geometric parameters. Analysis of a nearby sample of ellipticals indicates that differences in dynamical structure for these galaxies may cause a scatter, in the FP equivalent to 10% uncertainty on the distances. Thus, it may be possible to decrease the scatter by using the mean velocity dispersion within half the effective radius instead of the central velocity dispersion. The scatter in the D(n)-sigma relation for the Coma Cluster galaxies is 17%, much higher than the 11% scatter for the FP. The residuals depend on the mean surface brightness. A similar result was obtained by Lucey, Bower, & Ellis, who used a linear fit in a restricted interval in [mu]e in order to incorporate the effect in the distance determination. The D(n)-sigma relation is an approximation to the FP, as first noted by Dressler et al. and Phillips. We find that the dependence on [mu]e can be understood (without restrictions in [mu]e) as originating from this approximation. The FP projects into a slightly tilted and bended surface in the log D(n) - log sigma - [mu]e space. The available data in literature support this interpretation. Under the assumption that the FP is linear and the galaxies follow a de Vaucouleurs r1/4 law, the D(n)-sigma relation can cause systematic errors of the order 10%-15% on distance determinations. It is possible that some existing discrepancies between distances determined from the D(n)-sigma relation and from the Tully-Fisher method or the surface brightness fluctuation method are caused by the systematic errors of the D(n)-sigma relation. There is no evidence that the large-scale motions in the universe derived by Lynden-Bell et al. on the basis of the D(n)-sigma relation are severely affected by the systematic errors. We conclude that the FP is to be preferred as a distance indicator. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP JORGENSEN, I (reprint author), COPENHAGEN UNIV OBSERV,OSTER VOLDGADE 3,DK-1350 COPENHAGEN,DENMARK. NR 20 TC 71 Z9 71 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1993 VL 411 IS 1 BP 34 EP 42 DI 10.1086/172805 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LH604 UT WOS:A1993LH60400004 ER PT J AU KWONG, VHS FANG, Z GIBBONS, TT PARKINSON, WH SMITH, PL AF KWONG, VHS FANG, Z GIBBONS, TT PARKINSON, WH SMITH, PL TI MEASUREMENT OF THE TRANSITION-PROBABILITY OF THE C-III 190.9 NANOMETER INTERSYSTEM LINE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC DATA; ATOMIC PROCESSES ID OSCILLATOR-STRENGTHS; CHARGED IONS; SI-III; LEVEL AB A radio-frequency ion trap has been used to store C2+ ions created by electron bombardment of CO. The transition probability for the 2s2p 3P1o-2s2 1S0 intersystem line of C III has been measured by recording the radiative decay at 190.9 nm. The measured A-value is 121. +/- 7 s-1 and agrees, within mutual uncertainty limits, with that of Laughlin, Constantinides, & Victor (1978), but is 20% larger than that of Nussbaumer & Storey (1978). The effective collision mixing rate coefficient among the fine structure levels of 3P(o) and the combined quenching and charge transfer rate coefficients out of the 3P1o level with the CO source gas have also been measured. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP KWONG, VHS (reprint author), UNIV NEVADA,DEPT PHYS,4505 MARYLAND PKWY,LAS VEGAS,NV 89154, USA. NR 26 TC 48 Z9 49 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1993 VL 411 IS 1 BP 431 EP 437 DI 10.1086/172845 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LH604 UT WOS:A1993LH60400044 ER PT J AU YUN, MS HO, PTP LO, KY AF YUN, MS HO, PTP LO, KY TI H-I STREAMERS AROUND M82 - TIDALLY DISRUPTED OUTER GAS DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (M81, M82); GALAXIES, INTERACTIONS; GALAXIES, IRREGULAR; GALAXIES, SPIRAL; GALAXIES, STARBURST ID NEUTRAL HYDROGEN; STARBURST NUCLEUS; MERGING GALAXIES; DYNAMICS; EMISSION; RADIO; KINEMATICS; MORPHOLOGY; CLOUDS AB Our new VLA observations of M82 reveals a triangular central concentration of neutral atomic gas (1.9 x 10(8) M.) and several greater than or similar to 10 kpc long tidal streamers originating from M82 itself. The coincidence of the beginning of the tidal streamer with the flaring of the optical disk as well as the smooth continuation of the disk velocity field into the H I streamer strongly suggest the tidal disruption of the disk of M82, contrary to the widely proposed scenario of tidal stripping and gas accretion from its neighbor M81. The velocity characteristics of H I within M82 are that of disk rotation as seen in CO. The gas kinematics appear complex because of large velocity dispersions that may be due to a tidally induced bar potential and the interaction between the disk gas and the nuclear wind. Closer to the nucleus, the H I features are associated with both optical filaments and dust lanes, and it is suggested that these H I clouds are the sites of reflection and scattering of the light originating from the nuclear region. The extinction characteristics of the dust associated with the H I gas are similar to the Galactic dust and argue against an intergalactic origin for this H I gas. C1 UNIV ILLINOIS,DEPT ASTRON,URBANA,IL 61801. RP YUN, MS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 41 TC 94 Z9 94 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 1993 VL 411 IS 1 BP L17 EP & DI 10.1086/186901 PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LH606 UT WOS:A1993LH60600005 ER PT J AU HOWARD, JG DONOGHUE, AM JOHNSTON, LA WILDT, DE AF HOWARD, JG DONOGHUE, AM JOHNSTON, LA WILDT, DE TI ZONA-PELLUCIDA FILTRATION OF STRUCTURALLY ABNORMAL SPERMATOZOA AND REDUCED FERTILIZATION IN TERATOSPERMIC CATS SO BIOLOGY OF REPRODUCTION LA English DT Article ID SALT-STORED HAMSTER; HEMIZONA ASSAY HZA; INVITRO FERTILIZATION; DOMESTIC CAT; FOLLICULAR OOCYTES; EMBRYO DEVELOPMENT; SPERM; BINDING; EGGS; CAPACITATION AB Zona pellucida (ZP) penetration, in vitro fertilization, embryo development, and the morphology of fertilizing sperm were examined through use of normospermic (> 60% structurally normal sperm/ejaculate) versus teratospermic (< 40% structurally normal sperm/ejaculate) ejaculates from domestic cats. In addition, the effect of swim-up processing on sperm-oocyte interaction was compared with that of simple sperm washing. Normospermic and teratospermic ejaculates were evaluated for sperm motility and morphology. Sperm were preincubated for 1 h, then coincubated with in vivo-matured follicular cat oocytes (n = 401 ) for 20 h and with ZP-intact, salt-stored oocytes (n = 202) for 6 h. In vivo-matured oocytes were assessed for percent cleavage and stage of embryo development over time. Salt-stored oocytes were assessed for percent ZP penetration (proportion of oocytes containing sperm within or through the inner ZP), mean (+/- SEM) number of inner ZP-penetrated sperm, and the morphology of all bound and penetrated sperm. The incidence of pleiomorphic sperm in raw ejaculates averaged 29% in normospermic versus 67% in teratospermic males, but all ejaculates contained high sperm motility ratings (> 60%). Swim-up processing increased (p < 0.05) the number of normal sperm recovered/teratospermic inseminate (66.5 +/- 2.3%) compared to recovery after simple washing (28.6 +/- 2.2% ). Percent sperm motility also increased (p < 0.05) in teratospermic males after swim-up (90.0 +/- 1.3%) as compared to sperm washing (64.2 +/- 3.7%). Cleavage rate in vitro was higher (p < 0.05) using sperm from normospermic (86.3% ) compared to teratospermic (50.3% ) males, but rates of embryo development to the morula/blastocyst stage were similar (p > 0.05). ZP penetration of salt-stored oocytes by normospermic ejaculates (73.7% ) was superior (p < 0.01) to that of teratospermic ejaculates (24. 1% ); the number of ZP-penetrated sperm/oocyte was 5-fold higher (p < 0.05) in the normospermic than in the teratospermic group. The proportion of structurally normal bound and ZP-penetrated sperm was similar (p > 0.05) between cat populations regardless of the morphologic forms in the inseminate. Structurally abnormal sperm from teratospermic males were capable of ZP binding (29% ) and initial penetration into the outer ZP ( 1 7% ). However, only 3% of the inner ZP sperm were pleiomorphic, and every sperm within the perivitelline space was morphologically normal. Although swim-up processing increased sperm motility and the number of structurally normal sperm in the teratospermic inseminates, no difference (p > 0.05) was observed in cleavage or ZP penetration. These results indicate that the ZP is an efficient filter for structurally abnormal sperm, but even normal sperm from teratospermic cats appear impaired in fertilizing ability. Although teratospermia compromises ZP penetration and fertilization, the few embryos produced via teratospermic ejaculates develop normally in vitro. RP HOWARD, JG (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. FU NCRR NIH HHS [RR00045]; NICHD NIH HHS [HD23853] NR 38 TC 67 Z9 68 U1 0 U2 2 PU SOC STUDY REPRODUCTION PI MADISON PA 1603 MONROE ST, MADISON, WI 53711-2021 SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD JUL PY 1993 VL 49 IS 1 BP 131 EP 139 DI 10.1095/biolreprod49.1.131 PG 9 WC Reproductive Biology SC Reproductive Biology GA LK124 UT WOS:A1993LK12400015 PM 8353179 ER PT J AU OFTEDAL, OT ALT, GL WIDDOWSON, EM JAKUBASZ, MR AF OFTEDAL, OT ALT, GL WIDDOWSON, EM JAKUBASZ, MR TI NUTRITION AND GROWTH OF SUCKLING BLACK BEARS (URSUS-AMERICANUS) DURING THEIR MOTHERS WINTER FAST SO BRITISH JOURNAL OF NUTRITION LA English DT Article DE NEONATAL NUTRITION; MILK INTAKE; BODY COMPOSITION; BLACK BEARS ID TOTAL-BODY WATER; TRITIATED-WATER; MILK; METABOLISM; LACTATION; ANIMALS; ORGANS; BIRTH; FAT; STARVATION AB In black bears the last 6-8 weeks of gestation and the first 10-12 weeks of lactation occur in winter while the mother is in a dormant state, and reportedly does not eat, drink, urinate or defaecate. Measurements were made of the body composition and organ weights of cubs, of the composition of milk, and of milk intake (by dilution of (H2O)-H-2), in the first 3 months after birth. Additional milk samples were collected until 10 months postpartum. Bear cubs were small at birth, only 3.7 g/kg maternal weight, and chemically immature, as indicated by the high concentration of water (840 g/kg) in their bodies. Organ weights at birth were similar to those of puppies. In the first month after birth cubs gained 22 g/d or 0.23 g/g milk consumed; the milk was high in fat (220 g/kg) and low in water (670 g/kg). About 30 % of the ingested energy and 51 % of the ingested N were retained in the body. Over the entire 12-week period bear cubs required about 11 kg milk, containing (kg) water 7, fat 2.5, protein 0.8 and total sugar 0.25, to achieve a 2.5 kg weight gain. The birth of immature young and the production of high-fat, low-carbohydrate milk seem to be maternal adaptations to limit the utilization of glucogenic substrates during a long fast. Isotope recycling indicates that mothers may also recover most of the water (and perhaps much of the N) exported in milk by ingesting the excreta of the cubs. Lactation represents another aspect of the profound metabolic economy of the fasting bear in its winter den. C1 PENN GAME COMMISSION,MOSCOW,PA 18444. UNIV CAMBRIDGE,DEPT MED,CAMBRIDGE,ENGLAND. RP OFTEDAL, OT (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 79 TC 49 Z9 51 U1 2 U2 19 PU C A B INTERNATIONAL PI WALLINGFORD PA WALLINGFORD, OXON, ENGLAND OX10 8DE SN 0007-1145 J9 BRIT J NUTR JI Br. J. Nutr. PD JUL PY 1993 VL 70 IS 1 BP 59 EP 79 DI 10.1079/BJN19930105 PG 21 WC Nutrition & Dietetics SC Nutrition & Dietetics GA LT689 UT WOS:A1993LT68900007 PM 8399119 ER PT J AU MITROVICA, JX PELTIER, WR AF MITROVICA, JX PELTIER, WR TI THE INFERENCE OF MANTLE VISCOSITY FROM AN INVERSION OF THE FENNOSCANDIAN RELAXATION SPECTRUM SO GEOPHYSICAL JOURNAL INTERNATIONAL LA English DT Article DE FENNOSCANDIA; INVERSION; MANTLE VISCOSITY; RELAXATION SPECTRUM ID ISOSTATIC ADJUSTMENT; EARTH AB A formal inverse theory for mantle viscosity is here applied to a relaxation spectrum derived from the post-glacial uplift of Fennoscandia. The spectrum represents the set of eigenfrequencies (or inverse decay times) for the fundamental mode of viscous gravitational relaxation between the spherical harmonic degrees 14 to 45 and 65 to 80. Theoretical predictions of the eigenfrequencies are based upon the determination of the zeroes of the secular determinant function derived for a spherically symmetric, self-gravitating, visco-elastic planet. Differential kernels relating shifts in the eigenfrequencies to arbitrary perturbations in the radial viscosity profile (i.e. Frechet kernels) are computed using the variational principle derived by Peltier (1976). The inversions are performed within the framework of non-linear Bayesian inference, and the problem has been parameterized in terms of the logarithm of viscosity. The inversions have yielded a set of robust constraints which all models for the radial viscosity profile below Fennoscandia must satisfy. The a posteriori estimates and variance reduction are found to be insensitive to the a priori variance ascribed to the model layers. The constraints have, furthermore, been summarized into a set of a posteriori estimates of the average model viscosity value in radial regions consistent with the resolving power of the data (which decreases from a radial length scale of approximately 120 km at the base of the lithosphere to 1200 km at 1000 km depth; the data provide essentially no information regarding the mantle rheology below 1200 km depth). For example, for Earth models with a lithospheric thickness (LT) of 100 km, the volumetric average logarithm of viscosity in regions in the depth ranges 1040-400 km, 670-210 km and 235-100 km is constrained to be, respectively, 21.03 +/- 0.09, 20.70 +/- 0.08 and 20.37 +/- 0.19. We have repeated the inversions for a number of assumed lithospheric thicknesses and have found that a relatively low-viscosity layer in the sublithospheric region (with respect to the underlying upper mantle) is required for LT less-than-or-equal-to 120 km. In this respect we have quantified the previously described trade-off between a decrease in the viscosity of this region and a decrease in LT (Cathles 1975). In forward analyses of the glacial isostatic adjustment data set it is common to use Earth models with isoviscous upper and lower mantle regions. To investigate this 'two-layer' case we have also performed inversions which assume perfect correlation amongst the model layers in the upper and, separately, the lower mantle. Under this strict model space limitation, the inversions yield models with upper and lower mantle viscosities in the range 3.7 x 10(20)-4.5 x 10(20) Pa s and 2.2 x 10(21)-1.9 x 10(21) Pa s, respectively. (The ranges are obtained from a suite of inversions using lithospheric thickness from 70 km to 145 km.) The a posteriori constraints generated from the Bayesian inversions are used together with a statistic based on the computed misfit to the Fennoscandian relaxation spectrum, to rule out a number of previously published viscosity models. The constraints have also been used to construct a set of models which illustrate the non-uniqueness inherent to the a posteriori model space. We show, for example, that a model with a weak asthenosphere (down to 400 km depth) overlying an isoviscous 10(21) Pa s deep mantle provides a good fit to the relaxation spectrum. This is also true of models with a thin sublithospheric low-viscosity zone overlying a two-layer deep mantle with a moderate (factor of about three) jump in viscosity across 670 km depth, and models (as described in the preceding paragraph) with a viscosity jump of between four and six across isoviscous upper and lower mantle regions. In a companion paper the a posteriori constraints derived herein are used as a priori constraints in the direct inversion of RSL observations from Fennoscandia in order to examine whether this imprecision in the inference is a manifestation of the non-uniqueness inherent to the totality of the Fennoscandian data. C1 UNIV TORONTO,DEPT PHYS,TORONTO M5S 1A7,ONTARIO,CANADA. RP MITROVICA, JX (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS-42,CAMBRIDGE,MA 02138, USA. RI Peltier, William/A-1102-2008 NR 37 TC 75 Z9 76 U1 0 U2 6 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0956-540X J9 GEOPHYS J INT JI Geophys. J. Int. PD JUL PY 1993 VL 114 IS 1 BP 45 EP 62 DI 10.1111/j.1365-246X.1993.tb01465.x PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA LM794 UT WOS:A1993LM79400005 ER PT J AU MONFORT, SL BROWN, JL WILDT, DE AF MONFORT, SL BROWN, JL WILDT, DE TI EPISODIC AND SEASONAL RHYTHMS OF CORTISOL SECRETION IN MALE ELDS DEER (CERVUS-ELDI-THAMIN) SO JOURNAL OF ENDOCRINOLOGY LA English DT Article ID WHITE-TAILED DEER; MONITORING OVARIAN-FUNCTION; CIRCADIAN-RHYTHMS; PLASMA-CORTISOL; RUSA DEER; TESTOSTERONE; PROLACTIN; ACTH; PATTERN; LH AB Episodic and seasonal rhythms of cortisol secretion were evaluated in six adult Eld's deer (Cervus eldi thamin) stags. Plasma cortisol was measured in serial blood samples collected via remote catheterization every 10 min for 10 h within 2 weeks of the summer solstice (21 June), autumn equinox (22 September), winter solstice (21 December) and spring equinox (20 March), and in weekly blood samples collected from sedated stags. Cortisol was secreted episodically at a rate of approximately 0.6 peaks/h. Based on quantitative peak detection analyses of each 10-h data series, no overall seasonal differences (P>0.05) were detected in the number of peaks (mean range, 5.7-6.2), maximal peak height (mean range, 30.1-40.8 nmol/l), mean peak height as per cent increase (mean range, 158-168%), mean interval between peaks (mean range, 80.1-88.6 min), mean peak width (mean range, 55.1-65.1 min) and mean peak area under the curve (mean range, 675-816 nmol/l min). Based on weekly blood sampling, spring cortisol concentrations were elevated (P < 0.05) compared with summer and autumn concentrations. However, when mean cortisol concentrations derived from the 10-h quarterly data sets were analysed, no seasonal differences (P>0.05) were detected. The present study represents the first detailed confirmation of episodic cortisol secretion in any cervid. Results (1) indicate that Eld's deer stags lack a distinct seasonal rhythm of cortisol secretion and (2) clearly illustrate the need for frequent blood sampling in fully conscious individuals to ensure accurate assessment of adrenal status in cervids. C1 SMITHSONIAN INST,DEPT ANIM HLTH,NATL ZOOL PK,FRONT ROYAL,VA 22630. GEORGE MASON UNIV,DEPT BIOL ENVIRONM BIOL & PUBL POLICY,FAIRFAX,VA 22039. RP MONFORT, SL (reprint author), SMITHSONIAN INST,CONSERVAT & RES CTR,NATL ZOOL PK,1500 REMOUNT RD,FRONT ROYAL,VA 22630, USA. FU NICHD NIH HHS [HD 00903] NR 29 TC 42 Z9 43 U1 1 U2 4 PU J ENDOCRINOLOGY LTD PI BRISTOL PA 17/18 THE COURTYARD, WOODLANDS, ALMONDSBURY, BRISTOL, ENGLAND BS12 4NQ SN 0022-0795 J9 J ENDOCRINOL JI J. Endocrinol. PD JUL PY 1993 VL 138 IS 1 BP 41 EP 49 DI 10.1677/joe.0.1380041 PG 9 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA LV067 UT WOS:A1993LV06700006 PM 7852891 ER PT J AU JORDAN, TE CORRELL, DL WELLER, DE AF JORDAN, TE CORRELL, DL WELLER, DE TI NUTRIENT INTERCEPTION BY A RIPARIAN FOREST RECEIVING INPUTS FROM ADJACENT CROPLAND SO JOURNAL OF ENVIRONMENTAL QUALITY LA English DT Article; Proceedings Paper CT 17TH SYMP OF THE USDA-ARS BELTSVILLE AGRICULTURAL RESEARCH CENTER - AGRICULTURAL WATER-QUALITY PRIORITIES : A TEAM APPROACH TO CONSERVING NATURAL RESOURCES CY MAY 04-08, 1992 CL BELTSVILLE, MD SP USDA ARS ID SLUG TEST; NITRATE; DENITRIFICATION; GROUNDWATER; DYNAMICS; LOSSES AB To investigate the ability of riparian forest to intercept nutrients leaving adjacent cropland, we examined changes in the chemistry of groundwater flowing from a corn (Zea mays L.) field through a riparian forest. This study provided a comparison to previous studies of a different forest. We sampled groundwater from a transect of wells, and used a Br- tracer to confirm that groundwater moved laterally along the transect through the forest. As groundwater flowed through the forest, NO3- concentrations decreased from about 8 mg/L at the edge of the corn field to <0.4 mg/L halfway through the forest. Dissolved organic N and NH4+ increased by less than 0.1 mg/L, and dissolved organic C did not change with distance. Sulfate remained constant with distance until midway through the forest, where it began to increase. Chloride concentration rose until midway through the forest, then fell. Values of pH increased from under 5 at the edge of the corn field to over 7 at the stream bank, perhaps as a result of the NO3- consumption. Most of the change in NO3- occurred abruptly at the edge of a floodplain within the forest. There the water table was closest to the surface and soil Eh below the water table was less than -90 mV. Such strongly reducing conditions may have promoted denitrification in the floodplain. In contrast, soil Eh on the adjacent hill slope was above 500 mV, too high to support denitrification. There were only slight seasonal changes in groundwater chemistry. We also studied the net annual accretion of sediment in the riparian forest by measuring changes in the elevation of the soil surface. There was little or no accretion in the forest, but along a path of overland storm now there was net erosion. Thus, nutrient retention by this forest, in contrast with the forest we previously studied, was entirely a below ground process. Functional differences within sections of this forest and among different riparian forests suggest a need for research on the factors that control nutrient retention. RP JORDAN, TE (reprint author), SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037, USA. OI Weller, Donald/0000-0002-7629-5437 NR 35 TC 209 Z9 212 U1 6 U2 31 PU AMER SOC AGRONOMY PI MADISON PA 677 S SEGOE RD, MADISON, WI 53711 SN 0047-2425 J9 J ENVIRON QUAL JI J. Environ. Qual. PD JUL-SEP PY 1993 VL 22 IS 3 BP 467 EP 473 PG 7 WC Environmental Sciences SC Environmental Sciences & Ecology GA LT892 UT WOS:A1993LT89200010 ER PT J AU BUZAS, MA AF BUZAS, MA TI COLONIZATION RATE OF FORAMINIFERA IN THE INDIAN RIVER, FLORIDA SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article AB A cage containing azoic sand was placed on the seabed (1 m water depth) at Link Port, Florida on 17 March 1988. Beginning one week after emplacement, four replicate cores were taken inside the cage and outside every week for six weeks. From each of the eight cores 5 ml of sediment was removed from each cm to a depth of three cm. The number of living (stained) individuals for Quinqueloculina, Ammonia, Elphidium and Ammobaculites were enumerated. These data were analyzed by two-way ANOVA testing for differences between time, cms and their interaction. Inside, all taxa had significantly lower densities at the first two sampling times and had significantly lower densities in the second and third cms. Outside, only Elphidium had a significant difference with time, the fifth sampling time had lower densities. Quinqueloculina had significantly higher densities in the first cm and Ammobaculites in the first two cms. These results indicate that colonization is rapid and occurs in the same rank order as the ambient fauna. Densities stabilize inside within about three weeks after emplacement. The top cm is colonized initially followed by the second and third cms. No density peak was observed after the initial colonization, nor was there any succession of species. RP BUZAS, MA (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,WASHINGTON,DC 20560, USA. NR 13 TC 18 Z9 20 U1 1 U2 2 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD JUL PY 1993 VL 23 IS 3 BP 156 EP 161 PG 6 WC Paleontology SC Paleontology GA LV976 UT WOS:A1993LV97600002 ER PT J AU LESSIOS, HA AF LESSIOS, HA TI DXY - A PROGRAM FOR JACKKNIFED COMPARISONS BETWEEN ESTIMATES OF NUCLEOTIDE DIVERGENCE FROM RESTRICTION SITES SO JOURNAL OF HEREDITY LA English DT Note ID SUBSTITUTIONS; POPULATIONS RP LESSIOS, HA (reprint author), SMITHSONIAN TROP RES INST,BOX 2072,BALBOA,PANAMA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 SN 0022-1503 J9 J HERED JI J. Hered. PD JUL-AUG PY 1993 VL 84 IS 4 BP 317 EP 317 PG 1 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA LR292 UT WOS:A1993LR29200016 ER PT J AU NEUFELD, MJ AF NEUFELD, MJ TI HITLER, THE V-2, AND THE BATTLE FOR PRIORITY, 1939-1943 SO JOURNAL OF MILITARY HISTORY LA English DT Article RP NEUFELD, MJ (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 64 TC 1 Z9 2 U1 0 U2 0 PU VIRGINIA MILITARY INST PI LEXINGTON PA LEXINGTON, VA 24450 SN 0899-3718 J9 J MILITARY HIST JI J. Mil. Hist. PD JUL PY 1993 VL 57 IS 3 BP 511 EP 538 DI 10.2307/2943990 PG 28 WC History SC History GA LM044 UT WOS:A1993LM04400005 ER PT J AU THOMAS, JD AF THOMAS, JD TI BIOLOGICAL MONITORING AND TROPICAL BIODIVERSITY IN MARINE ENVIRONMENTS - A CRITIQUE WITH RECOMMENDATIONS, AND COMMENTS ON THE USE OF AMPHIPODS AS BIOINDICATORS SO JOURNAL OF NATURAL HISTORY LA English DT Article DE AMPHIPODS; BIODIVERSITY; BIOLOGICAL CRITERIA; CORAL REEFS; INDEX OF BIOTIC INTEGRITY; MARINE MONITORING ID CONSERVATION; COMMUNITIES; DIVERSITY; GAMMARUS; CRISIS; OIL AB Preoccupations with regulatory and legal liability issues in marine environmental monitoring have led to programmes based on reductionist models that use non-biological parameters which are indirect measures of biotic condition. The ability to assess the effectiveness of current monitoring programmes to protect the marine environment at regional and national scales does not currently exist. Current monitoring programmes rarely serve the function for which they were intended: an accurate and sensitive source of information from which conditions and trends can be defined and recognized, and management decisions made. In addition, the natural variability of systems is problematic and must be documented in order to distinguish natural from anthropogenic changes in environmental conditions. Owing to their ecological importance, numerical abundance, and sensitivity to a variety of toxicants and pollutants, amphipod crustaceans have long been known as sensitive environmental indicators. However, application and use of amphipods in such programmes is limited to the few regions where ongoing comprehensive taxonomic and natural history investigations have been undertaken. Potential for amphipods as bioindicators exists in a wide variety of environments, especially in the tropics, but their incorporation into such programmes is dependent upon completion of taxonomic surveys and inventories. RP THOMAS, JD (reprint author), SMITHSONIAN INST,NHB STOP 163,WASHINGTON,DC 20560, USA. NR 55 TC 58 Z9 64 U1 0 U2 14 PU TAYLOR & FRANCIS LTD PI LONDON PA ONE GUNDPOWDER SQUARE, LONDON, ENGLAND EC4A 3DE SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PD JUL-AUG PY 1993 VL 27 IS 4 BP 795 EP 806 DI 10.1080/00222939300770481 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA LY830 UT WOS:A1993LY83000007 ER PT J AU BUZAS, MA CULVER, SJ AF BUZAS, MA CULVER, SJ TI PRESENTATION OF THE SCHUCHERT,CHARLES AWARD OF THE PALEONTOLOGICAL-SOCIETY TO CULVER,STEPHEN,J. SO JOURNAL OF PALEONTOLOGY LA English DT Item About an Individual RP BUZAS, MA (reprint author), SMITHSONIAN INST,DEPT PALEONTOL,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD JUL PY 1993 VL 67 IS 4 BP 690 EP 692 PG 3 WC Paleontology SC Paleontology GA LK833 UT WOS:A1993LK83300019 ER PT J AU MONFORT, SL BROWN, JL BUSH, M WOOD, TC WEMMER, C VARGAS, A WILLIAMSON, LR MONTALI, RJ WILDT, DE AF MONFORT, SL BROWN, JL BUSH, M WOOD, TC WEMMER, C VARGAS, A WILLIAMSON, LR MONTALI, RJ WILDT, DE TI CIRCANNUAL INTERRELATIONSHIPS AMONG REPRODUCTIVE HORMONES, GROSS MORPHOMETRY, BEHAVIOR, EJACULATE CHARACTERISTICS AND TESTICULAR HISTOLOGY IN ELDS DEER STAGS (CERVUS-ELDI-THAMIN) SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article ID WHITE-TAILED DEER; SEASONAL-VARIATION; TESTOSTERONE CONCENTRATIONS; PLASMA-CONCENTRATIONS; DOMESTICATED BREEDS; LUTEINIZING-HORMONE; SERUM TESTOSTERONE; SPERM PRODUCTION; RUSA-TIMORENSIS; ANTLER GROWTH AB Blood samples, morphometric measurements and behavioural data were collected weekly for 52 weeks from six adult Eld's deer stags exposed to natural fluctuations in photoperiod (38-degrees-N latitude). Mean (+/- SEM) serum LH concentrations reached peak values in the autumn (October), three months before FSH and testosterone concentrations reached peak values in early winter (January). Prolactin concentrations were inversely related (r = -0.733, P < 0.001) to LH and directly related to daylength, and maximal concentrations were observed during mid-summer (July) and minimal concentrations during early winter (January). The temporal pattern of circulating inhibin was positively correlated with FSH (r = 0.88, P < 0.001), but lagged behind the seasonal FSH increase by 1-3 weeks. Antler length, body weight and chest girth were maximal during pre-rut (December-January). Maximal scrotal circumference and combined testes volume were observed in mid-winter (February), whereas peak neck girth and behavioural aggression occurred 1-3 months later (March-May). On the basis of quarterly electroejaculation results, motile spermatozoa were produced in all seasons. However, the greatest number of motile spermatozoa per ejaculate was observed during the winter and spring, whereas the highest incidence of sperm pleiomorphisms (> 80%) was detected in the autumn. Histological assessments of the regressed testis (July) revealed fewer germ cells undergoing spermatogenesis and an increased incidence of degenerating and abnormal cell types. In summary, Eld's deer exhibit a circannual hypothalamic-pituitary-gonadal cycle with onset of pituitary activation occurring during the autumn and winter, whereas gonadal activity peaks during the winter and spring as daylengths are increasing. Marked circannual variations in circulating prolactin suggest that Eld's deer may use photoperiodic cues to modulate seasonal fertility; however, the existence of an endogenous seasonal rhythm operating independently of photoperiod cannot be excluded. C1 SMITHSONIAN INST,DEPT CONSERVAT & PATHOL,NATL ZOOL PK,FRONT ROYAL,VA 22630. GEORGE MASON UNIV,DEPT BIOL ENVIRONM BIOL & PUBL POLICY,FAIRFAX,VA 22039. RP MONFORT, SL (reprint author), SMITHSONIAN INST,DEPT ANIM HLTH,NATL ZOOL PK,FRONT ROYAL,VA 22630, USA. FU NICHD NIH HHS [HD 00903] NR 59 TC 62 Z9 64 U1 1 U2 2 PU J REPROD FERTIL INC PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE, ENGLAND CB5 8DT SN 0022-4251 J9 J REPROD FERTIL JI J. Reprod. Fertil. PD JUL PY 1993 VL 98 IS 2 BP 471 EP 480 PG 10 WC Reproductive Biology SC Reproductive Biology GA LW751 UT WOS:A1993LW75100021 PM 8410813 ER PT J AU MONFORT, SL BROWN, JL WOOD, TC WEMMER, C VARGAS, A WILLIAMSON, LR WILDT, DE AF MONFORT, SL BROWN, JL WOOD, TC WEMMER, C VARGAS, A WILLIAMSON, LR WILDT, DE TI SEASONAL PATTERNS OF BASAL AND GNRH-INDUCED LH, FSH AND TESTOSTERONE SECRETION IN ELDS DEER STAGS (CERVUS-ELDI-THAMIN) SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article ID WHITE-TAILED DEER; MALE FALLOW DEER; ELAPHUS STAGS; DAMA-DAMA; PLASMA-LH; ANTLER; RESPONSES; HORMONE; GROWTH AB Plasma LH, FSH and testosterone were measured in blood samples collected via remote catheterization from six adult Eld's deer stags every 10 min for 8 h before and 2 h after GnRH (1 mug kg-1, i.v.) administration. Blood samples were collected within 2 weeks of the summer solstice (21 June), autumn equinox (22 September), winter solstice (21 December) and spring equinox (20 March). Marked seasonal variations in basal LH, FSH and testosterone concentrations were observed. From autumn, well-defined LH pulses were temporally associated with small, but detectable pulses in testosterone. During the winter transition into the breeding season, episodic LH pulses were also temporally associated with corresponding testosterone surges that lasted 2-3 h. High amplitude, low frequency testosterone surges were also observed during the spring, but often in the absence of detectable LH pulses. Basal LH and testosterone concentrations decreased during the summer and, although LH pulses were detected, associated testosterone pulses were absent. Only 37% of LH pulses occurred coincidentally with FSH pulses, and FSH pulses were generally less prominent. The increases in LH and FSH above basal concentrations after GnRH treatment were significant (P < 0.05) for all seasons. Increases in testosterone after GnRH treatment were greatest during the winter and spring, but testosterone also increased to a lesser extent during the autumn (P < 0.05). In contrast, testosterone concentrations were not different before and after GnRH treatment during summer. The net LH increase after GnRH treatment was similar (P > 0.05) for all seasons, whereas the proportional increase in LH was greatest (P < 0.05) during the summer and autumn when basal concentrations were lowest. Although the net FSH increase after GnRH treatment ranged only from 20 to 40 ng ml-1 during all seasons, the proportional rise in FSH after GnRH treatment tended to be highest during the summer and autumn when basal concentrations were lowest. Basal testosterone secretion and the net increase in testosterone after GnRH treatments were greatest during the spring rut (P < 0.05). Thus, in Eld's deer, it appears that pituitary gonadotrophs seasonally adjust their basal secretory 'set point', but the capacity to respond above basal concentrations is constrained to a maximum net increase in both LH and FSH, regardless of season. Because both basal LH and the net releasable pool of LH remain relatively constant, increased testosterone secretion after GnRH treatment probably represents increased testicular sensitivity to LH. C1 SMITHSONIAN INST,DEPT CONSERVAT,NATL ZOOL PK,FRONT ROYAL,VA 22630. GEORGE MASON UNIV,DEPT BIOL ENVIRONM BIOL & PUBL POLICY,FAIRFAX,VA 22039. RP MONFORT, SL (reprint author), SMITHSONIAN INST,DEPT ANIM HLTH,NATL ZOOL PK,FRONT ROYAL,VA 22630, USA. FU NICHD NIH HHS [HD 00903] NR 18 TC 14 Z9 15 U1 0 U2 1 PU J REPROD FERTIL INC PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE, ENGLAND CB5 8DT SN 0022-4251 J9 J REPROD FERTIL JI J. Reprod. Fertil. PD JUL PY 1993 VL 98 IS 2 BP 481 EP 488 PG 8 WC Reproductive Biology SC Reproductive Biology GA LW751 UT WOS:A1993LW75100022 PM 8410814 ER PT J AU BANISH, LD SIMS, R SACK, D MONTALI, RJ PHILLIPS, L BUSH, M AF BANISH, LD SIMS, R SACK, D MONTALI, RJ PHILLIPS, L BUSH, M TI PREVALENCE OF SHIGELLOSIS AND OTHER ENTERIC PATHOGENS IN A ZOOLOGIC COLLECTION OF PRIMATES SO JOURNAL OF THE AMERICAN VETERINARY MEDICAL ASSOCIATION LA English DT Article ID FECAL LEUKOCYTES; RESISTANT AB An epidemiologic study of shigellosis was the preliminary step in the formulation of a plan for the control of devastating infectious diseases in nonhuman primates at the National Zoological Park. Data were collected from primate groups with enzootic shigellosis and included the following species: white-cheeked and siamang gibbons (Hylobates concolor and H syndactylies); lion-tailed, celebes, and Barbary macaques (Macaca silenus, M nigera, and M sylvanus); black and white colobus monkeys (Colobus guerzea); grey-cheeked mangabeys (Cerecocebus albigena); spider monkeys (Ateles susciceps robusuts); ruffed lemurs (Lemur varrigatus); lowland gorillas (Gorilla gorilla); and orangutans (pongo pygmaeus). Data included results of physical examination, proctoscopy with biopsy, fecal parasitologic and cytologic examinations, and bacteriologic culturing of swabbed specimens of rectum and gingiva. Repetitive fecal examinations were subsequently performed and included bacteriologic culturing of fecal specimens for enteropathogenic bacteria and parasites and cytologic examination of feces. Data were collected for a 1-year period from 82 primates, and 14 gibbons were studied intensively. White-cheeked and siamang gibbons shed Shigella flexneri sporadically, but persistently. All gibbons were affected with a mean point prevalence of 30.7% (range 0 to 71%). Shigella flexneri also was isolated from feces of lion-tailed macaques. Shigella sonnei was isolated from feces of grey-cheeked mangabeys, celebes macaques, and spider monkeys. Of 180 colonic mucosal biopsy specimens from 60 primates, 3 contained Shigella spp. Most S flexneri isolates were serotype Y. Our findings substantiated that enzootic shigellosis was more widespread at the National Zoological Park than signs of disease and results of a few bacteriologic cultures suggested. Those primate species affected were pinpointed, and the heterogeneity of Shigella spp involved was elucidated. Supportive diagnostic techniques were investigated and an unconventional protocol for performing bacteriologic culturing of fecal specimens was found useful in decreasing false-negative results. Epidemiologic findings and shedding patterns defined appropriateness of clinical management options. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT PATHOL,WASHINGTON,DC 20008. DEPT LAB SERV,DIV PATHOL,WALTER REED ARMY INST RES,WASHINGTON,DC 20012. JOHNS HOPKINS UNIV,SCH PUBL HLTH,DEPT INT MED,BALTIMORE,MD 21205. RP BANISH, LD (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ANIM HLTH,WASHINGTON,DC 20008, USA. NR 15 TC 16 Z9 16 U1 1 U2 9 PU AMER VETERINARY MEDICAL ASSOC PI SCHAUMBURG PA 1931 N MEACHAM RD SUITE 100, SCHAUMBURG, IL 60173-4360 SN 0003-1488 J9 J AM VET MED ASSOC JI J. Am. Vet. Med. Assoc. PD JUL 1 PY 1993 VL 203 IS 1 BP 126 EP 132 PG 7 WC Veterinary Sciences SC Veterinary Sciences GA LK830 UT WOS:A1993LK83000029 PM 8407446 ER PT J AU BANISH, LD SIMS, R BUSH, M SACK, D MONTALI, RJ AF BANISH, LD SIMS, R BUSH, M SACK, D MONTALI, RJ TI CLEARANCE OF SHIGELLA-FLEXNERI CARRIERS IN A ZOOLOGIC COLLECTION OF PRIMATES SO JOURNAL OF THE AMERICAN VETERINARY MEDICAL ASSOCIATION LA English DT Article ID ARTHROPATHY; MONKEYS AB In 1990, a high prevalence of Shigella flexneri was documented in the gibbon population at the National Zoological Park. The enzootic strain had been determined to be resistant to most antibiotics and had been responsible for animal deaths. Prevalence of Shigella spp was high in the entire primate population. To address the clinical problem, eradication was attempted by use of enrofloxacin. Facilities disinfection comprised a large part of Shigella clearance efforts. After the clearance protocol was completed gibbons, vs other primate species, were closely monitored for 16 months by subjecting their feces to bacteriologic culturing. The program was successful, with eradication Of the problematic strain of S flexneri. However, 10 to 12 months after completion of treatments, S sonnei was isolated from feces of 3 animals living in the same housing facility. C1 SMITHSONIAN INST,NATL ZOOL PK,DEPT PATHOL,WASHINGTON,DC 20008. DEPT LAB SERV,DIV PATHOL,WALTER REED ARMY INST RES,WASHINGTON,DC 20012. JOHNS HOPKINS UNIV,SCH PUBL HLTH,DEPT INTERNAL MED,BALTIMORE,MD 21205. RP BANISH, LD (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ANIM HLTH,WASHINGTON,DC 20008, USA. NR 15 TC 9 Z9 9 U1 2 U2 2 PU AMER VETERINARY MEDICAL ASSOC PI SCHAUMBURG PA 1931 N MEACHAM RD SUITE 100, SCHAUMBURG, IL 60173-4360 SN 0003-1488 J9 J AM VET MED ASSOC JI J. Am. Vet. Med. Assoc. PD JUL 1 PY 1993 VL 203 IS 1 BP 133 EP 136 PG 4 WC Veterinary Sciences SC Veterinary Sciences GA LK830 UT WOS:A1993LK83000030 PM 8407447 ER PT J AU BOCKSTAHLER, KR COATS, DW AF BOCKSTAHLER, KR COATS, DW TI GRAZING OF THE MIXOTROPHIC DINOFLAGELLATE GYMNODINIUM-SANGUINEUM ON CILIATE POPULATIONS OF CHESAPEAKE BAY SO MARINE BIOLOGY LA English DT Article ID POTERIOOCHROMONAS-MALHAMENSIS; QUANTITATIVE IMPORTANCE; OXYRRHIS-MARINA; PACIFIC-OCEAN; RATES; PHYTOPLANKTON; GROWTH; DYNAMICS; NITRATE; BACTERIVORY AB In situ grazing rates for the mixotrophic dinoflagellate Gymnodinium sanguineum Hirasaka feeding on nanociliate populations of Chesapeake Bay were determined in June and October of 1990 using a ''gut clearance/gut fullness'' approach. Recently ingested prey were digested beyond the point of recognition at a rate of approximately 23 % h - 1. Estimates of in situ ingestion and clearance ranged from 0 to 0.06 prey dinoflagellate - 1 h - 1 and 0 to 5.8 mul dinoflagellate-1 h-1, respectively, with daily removal of ciliate biomass representing 6 to 67 % of the less-than-or-equal-to 20-mum oligotrich standing stock. Daily consumption of ciliate biomass by G. sanguineum averaged 2.5 % of body carbon and 4.0 % of body nitrogen with maximal values of 11.6 and 18.5 %, respectively. Ingestion of ciliates may help balance nitrogen requirements for G. sanguineum and give this species an advantage over purely photosynthetic dinoflagellates in nitrogen limited environments. By preying on ciliates, these dinoflagellates reverse the normal flow of material from primary producer to consumer and thereby influence trophodynamics of the microbial food web in Chesapeake Bay. RP BOCKSTAHLER, KR (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. NR 62 TC 76 Z9 82 U1 1 U2 7 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD JUL PY 1993 VL 116 IS 3 BP 477 EP 487 DI 10.1007/BF00350065 PG 11 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA LN998 UT WOS:A1993LN99800015 ER PT J AU MARVIN, UB AF MARVIN, UB TI THE METEORITICAL SOCIETY - 1933 TO 1993 SO METEORITICS LA English DT Review AB In August, 1933, at the Field Museum of Natural History in Chicago, The Society for Research on Meteorites was founded with an enrollment of 57 charter members and Frederick C. Leonard and Harvey H. Nininger as the first President and Secretary-Treasurer, respectively. Within five years, the Society had doubled in size, with members from the U.S.A. and ten other nations. Annual meetings were suspended during World War II (1942 through 1945) and when it reconvened in 1946 the members adopted the name ''The Meteoritical Society''. By that time personal and professional antagonisms had arisen that threatened to fragment the Society and led, in 1949, to the resignation of Nininger and his wife. Throughout the 1950s the Society was widely regarded as a small, disorganized and essentially moribund organization. Revitalization of the Society began in the early 1960s after the advent of the Space Age when the Society steadily gained members with expertise in mineralogy, petrology, isotope geochemistry, electron microprobe and neutron activation analysis, and impact dynamics. When Nininger was persuaded rejoin in 1963, he found a renewed Society. In the election year of 1966 a group of youthful insurgents nominated an alternate slate to that proposed by the Council and won every contested seat on the Council except that of the Editor. The Society's first publication Contributions of the Society for Research on Meteorites was published as a section of Popular Astronomy and from 1935 to 1946 reprints of the items (articles, reviews, and notices) were bound and distributed separately each year. When the Society changed its name in 1946, its journal became Contributions of the Meteoritical Society, which continued publication until Popular Astronomy ceased publication in 1952. A new journal, Meteoritics, was instituted in 1953. After 1956, its publication lapsed for six years but began again in 1963 and has continued under the leadership of four successive editors becoming one of the most frequently cited geoscience journals. In 1970, the Society also became a co-sponsor with The Geochemical Society of Geochimica et Cosmochimica Acta, but the future of this arrangement remains in doubt. In 1938, the Society had gained considerable prestige by its acceptance as a full Affiliate of the American Association for the Advancement of Science, but in view of its increasingly international membership and activities the Society terminated its affiliation with the AAAS in 1976. Again in response to its international status, in 1992 The Meteoritical Society affiliated with the International Union of Geological Sciences. The Society held its first annual meeting outside North America at the Universitat Tubingen in West Germany in 1971. Subsequently, it met in Europe every second year until 1990, when it met at Perth in Western Australia. During the 1980s, the membership of the Society grew to more than 900 and the annual meetings attracted between 300 and 450 participants. As meteoritical research continues to probe the borderlands with astrophysics, planetary science, and terrestrial geology, and as younger members assume leadership roles, a productive future seems assured for both meteoritical science and The Meteoritical Society. C1 HARVARD UNIV,DEPT EARTH & PLANETARY SCI,CAMBRIDGE,MA 02138. RP MARVIN, UB (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 65 TC 10 Z9 10 U1 0 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD JUL PY 1993 VL 28 IS 3 BP 261 EP 314 PG 54 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA LN410 UT WOS:A1993LN41000002 ER PT J AU MAOZ, E AF MAOZ, E TI A FLUCTUATION DISSIPATION APPROACH TO DYNAMICAL FRICTION IN NONHOMOGENEOUS BACKGROUNDS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE METHODS-ANALYTICAL; CELESTIAL MECHANICS, STELLAR DYNAMICS ID SINKING SATELLITES; SPHERICAL SYSTEMS; ORBITAL DECAY; SIMULATIONS; GALAXY AB A formula is derived for the dynamical friction experienced by an object which is travelling in an arbitrary mass density field, assuming that the object's mass much exceeds that of a background particle, and that the background is stationary and is described by a global Maxwellian velocity distribution. This work extends a recent study which relates dynamical friction to the interaction of the object with background fluctuations in an infinite homogeneous medium. The new approach has some limitations, but it still provides a better estimate for the friction in non-homogeneous media than does Chandrasekhar's formula. The drag no longer depends only on local background characteristics as in the homogeneous case, but is a function of the global structure of the entire mass density field. In contrast to Chandrasekhar's formula, the frictional force now turns out to depend also on the object's direction of motion with respect to gradients in the surrounding mass distribution. RP MAOZ, E (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS 51,CAMBRIDGE,MA 02138, USA. NR 18 TC 29 Z9 29 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 1993 VL 263 IS 1 BP 75 EP 85 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LK787 UT WOS:A1993LK78700015 ER PT J AU WEIL, SE AF WEIL, SE TI COPYRIGHTS AND WRONGS + COMPLEX LEGAL ISSUES FOR MUSEUMS SO MUSEUM NEWS LA English DT Article RP WEIL, SE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC MUSEUMS PI WASHINGTON PA 1575 EYE ST, NW, STE 400, WASHINGTON, DC 20005 SN 0027-4089 J9 MUSEUM NEWS JI Mus. News PD JUL-AUG PY 1993 VL 72 IS 4 BP 40 EP & PG 0 WC Art SC Art GA LL543 UT WOS:A1993LL54300017 ER PT J AU JOHNSTON, PF AF JOHNSTON, PF TI SHIPBUILDING AT CRAMP-AND-SONS - A HISTORY AND GUIDE TO COLLECTIONS OF THE CRAMP,WILLIAM AND SONS SHIP AND ENGINE BUILDING COMPANY (1830-1927) AND THE CRAMP-SHIPBUILDING-COMPANY (1941-46) OF PHILADELPHIA - FARR,GE, BOSTWICK,BF, WILLIS,M SO PENNSYLVANIA MAGAZINE OF HISTORY AND BIOGRAPHY LA English DT Book Review RP JOHNSTON, PF (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU HISTORICAL SOC PA PI PHILADELPHIA PA 1300 LOCUST ST, PHILADELPHIA, PA 19107 SN 0031-4587 J9 PENN MAG HIST BIOG JI Pa. Mag. Hist. Biogr. PD JUL PY 1993 VL 117 IS 3 BP 237 EP 239 PG 3 WC History SC History GA LN674 UT WOS:A1993LN67400021 ER PT J AU JOHNSTON, PF AF JOHNSTON, PF TI LENTHALL,JOHN, NAVAL-ARCHITECT - A GUIDE TO PLANS AND DRAWINGS OF AMERICAN, NAVAL AND MERCHANT VESSELS, 1790-1874 - FARR,GE, BOSTWICK,BF SO PENNSYLVANIA MAGAZINE OF HISTORY AND BIOGRAPHY LA English DT Book Review RP JOHNSTON, PF (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU HISTORICAL SOC PA PI PHILADELPHIA PA 1300 LOCUST ST, PHILADELPHIA, PA 19107 SN 0031-4587 J9 PENN MAG HIST BIOG JI Pa. Mag. Hist. Biogr. PD JUL PY 1993 VL 117 IS 3 BP 237 EP 239 PG 3 WC History SC History GA LN674 UT WOS:A1993LN67400022 ER PT J AU YANG, XZ BURGDORFER, J AF YANG, XZ BURGDORFER, J TI STATISTICS OF AVOIDED CROSSINGS FOR GENERIC QUANTUM-SYSTEMS SO PHYSICAL REVIEW A LA English DT Article ID HYDROGEN-ATOM; MAGNETIC-FIELD; ENERGY-LEVELS; SPECTRUM; CHAOS; DISTRIBUTIONS; EXAMPLE AB The distribution of isolated avoided crossings in quantum systems whose classical counterparts possess a mixed phase space of regular and chaotic dynamics is investigated. The distribution function for the width is shown to consist of two components: a near-Gaussian distribution suggested by random matrix theory for the chaotic component and an approximately delta-shaped component originating from tori in the regular portion of phase space. A statistical measure for overlapping avoided crossing based on parametric correlations of energy levels is introduced and shown to be sensitive to the fraction of classically chaotic phase space. RP YANG, XZ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138, USA. NR 29 TC 11 Z9 11 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUL PY 1993 VL 48 IS 1 BP 83 EP 87 DI 10.1103/PhysRevA.48.83 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LM341 UT WOS:A1993LM34100018 ER PT J AU LAFYATIS, GP KIRBY, K DALGARNO, A AF LAFYATIS, GP KIRBY, K DALGARNO, A TI MOLECULAR CATION NHE-2+ SO PHYSICAL REVIEW A LA English DT Article ID CHARGE-TRANSFER; IONS; HELIUM AB The potential-energy curves of the low-lying 2SIGMA+ and 2PI states of the cation NHe2+ are calculated and it is shown that the lowest state of each symmetry has a potential well inside a repulsive Coulomb barrier that contains several long-lived vibrational levels. Estimates are made of the cross sections of the charge-transfer processes N2+ + He-->N+ + He+ which occur through transitions at avoided crossings of the molecular states. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP LAFYATIS, GP (reprint author), OHIO STATE UNIV,DEPT PHYS,COLUMBUS,OH 43210, USA. NR 15 TC 6 Z9 6 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUL PY 1993 VL 48 IS 1 BP 321 EP 325 DI 10.1103/PhysRevA.48.321 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LM341 UT WOS:A1993LM34100048 ER PT J AU IMAMOGLU, A AF IMAMOGLU, A TI QUANTUM-NONDEMOLITION MEASUREMENTS USING DISSIPATIVE ATOM-FIELD COUPLING - MONTE-CARLO WAVE-FUNCTION APPROACH SO PHYSICAL REVIEW A LA English DT Article ID PHOTON NUMBER; SYSTEM AB A continuous quantum-nondemolition measurement scheme that is based on intensity dependent atomic scattering in three-state systems is analyzed. The proposed scheme measures the number of photons in an optical cavity mode by observing the scattering rate of the atomic medium. The time evolution of the coupled atom-field system is analyzed using the Monte Carlo wave-function approach. The wave-function collapse occurs continuously as a result of the presence or absence of scattering events at each time instant. It is shown that the measurement is logically reversible and the information contained in the premeasurement wave function is preserved during the measurement interaction. RP IMAMOGLU, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,MS14,CAMBRIDGE,MA 02138, USA. NR 35 TC 7 Z9 7 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUL PY 1993 VL 48 IS 1 BP 770 EP 781 DI 10.1103/PhysRevA.48.770 PG 12 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LM341 UT WOS:A1993LM34100100 ER PT J AU HELLER, EJ TOMSOVIC, S AF HELLER, EJ TOMSOVIC, S TI POSTMODERN QUANTUM-MECHANICS SO PHYSICS TODAY LA English DT Article ID PERIODIC-ORBITS; HYDROGEN-ATOM; MAGNETIC-FIELD; CHAOTIC SYSTEMS; WAVE-FUNCTIONS; QUANTIZATION; SPECTRA; LONG; ABSORPTION; DYNAMICS C1 UNIV WASHINGTON,SEATTLE,WA 98195. RP HELLER, EJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 34 TC 139 Z9 139 U1 1 U2 7 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD JUL PY 1993 VL 46 IS 7 BP 38 EP 46 DI 10.1063/1.881358 PG 9 WC Physics, Multidisciplinary SC Physics GA LN088 UT WOS:A1993LN08800015 ER PT J AU ZOTZ, G WINTER, K AF ZOTZ, G WINTER, K TI SHORT-TERM REGULATION OF CRASSULACEAN ACID METABOLISM ACTIVITY IN A TROPICAL HEMIEPIPHYTE, CLUSIA-UVITANA SO PLANT PHYSIOLOGY LA English DT Article ID MESEMBRYANTHEMUM-CRYSTALLINUM; WATER-STRESS; GAS-EXCHANGE; C3-CAM TREE; LIGHT; CO2; ACCUMULATION AB Diel courses of net CO2 exchange of leaves were studied in Clusia uvitana (Clusiaceae), a tropical Crassulacean acid metabolism (CAM) hemiepiphyte, growing in the crown of a 47-m tall kapok tree on Barro Colorado Island, Panama. Measurements on days without precipitation showed that net uptake of atmospheric CO2 occurred at night, a feature of CAM, as well as in the early morning and late afternoon. During 36 h of almost continuous rainfall, nocturnal net CO2 uptake was abolished and the diel pattern of net CO2 exchange became similar to that of a C3 plant. Exposing well-watered, potted plants of Clusia in the laboratory to temperatures and photosynthetic photon flux densities similar to those during the tropical rainstorm also abolished nocturnal net CO2 uptake. In contrast, Kalanchoe pinnata (Crassulaceae), an obligate CAM plant, still showed net CO2 dark fixation following the same low-light and moderate-temperature conditions, albeit at decreased rates. During these 12-h photoperiods, titratable acidity in Clusia increased slightly above its high level measured at the end of the previous dark period, whereas in Kalanchoe, the acid content decreased by about 40%. A survey among outer canopy leaves of Clusia on Barro Colorado Island showed that leaves that exhibited little or no nocturnal acidification maintained high levels of H+ at dawn and dusk. Progressively lower levels of H+ at dusk were accompanied by progressively higher nocturnal increases in H+. The data suggest that in C. uvitana the rapid switching between CAM- and C3-type carbon fixation that may occur within 24 h in response to environmental changes is controlled by the acidity status of the leaves in the light. Nocturnal CO2 fixation is enhanced by conditions that decrease the organic acid content during the light period. C1 SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. NR 22 TC 41 Z9 42 U1 0 U2 4 PU AMER SOC PLANT PHYSIOLOGISTS PI ROCKVILLE PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 SN 0032-0889 J9 PLANT PHYSIOL JI Plant Physiol. PD JUL PY 1993 VL 102 IS 3 BP 835 EP 841 PG 7 WC Plant Sciences SC Plant Sciences GA LM877 UT WOS:A1993LM87700016 ER PT J AU BRICENO, C CALVET, N GOMEZ, M HARTMANN, LW KENYON, SJ WHITNEY, BA AF BRICENO, C CALVET, N GOMEZ, M HARTMANN, LW KENYON, SJ WHITNEY, BA TI 1ST RESULTS OF THE CIDA SCHMIDT SURVEY - SELECTED ZONES IN TAURUS-AURIGA SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID MAIN-SEQUENCE STARS; MOLECULAR CLOUD; DARK CLOUDS; EMISSION; PERSEUS AB We have begun an objective-prism Halpha survey of star-forming regions using the CIDA 1 m Schmidt Camera, with a limiting magnitude V almost-equal-to 18. We report here first results for selected areas of the Taurus-Auriga molecular clouds. Of the list of candidates found in the objective-prism plates, twelve stars have been confirmed as pre-main sequence by the detection of the Li I 6707 angstrom absorption line. Five of these stars are in the dark cloud L1544, where only one T Tauri star was previously known. The new stars have very late spectral types and most have estimated masses between 0.2 M. and 0.3 M.. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. INST ESTUDIS CATALANS,SOC CATALANA FIS,ASTROFIS GRP,BARCELONA,SPAIN. RP BRICENO, C (reprint author), CTR INVEST ASTRON,AP P 264,MERIDA 5101A,VENEZUELA. OI Kenyon, Scott/0000-0003-0214-609X NR 29 TC 43 Z9 43 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 1993 VL 105 IS 689 BP 686 EP 692 DI 10.1086/133221 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LN087 UT WOS:A1993LN08700002 ER PT J AU STONE, RPS KRAFT, RP PROSSER, CF AF STONE, RPS KRAFT, RP PROSSER, CF TI THE OPTICAL-SPECTRUM OF FG SAGITTAE DURING ITS RECENT DECLINE IN BRIGHTNESS SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID PHOTOMETRY; PLANETARY AB We describe low- and intermediate-resolution optical spectra of the peculiar variable star FG Sagittae that were obtained during the later stages of its current episode of sharply diminished optical luminosity. In the region from lambda5600 to lambda6700 angstrom, the line spectrum is essentially the same as it was in 1983: it contains lines of Fe-peak elements typical of luminous stars of spectral type G or early K, together with a forest of lines due to heavy elements associated with traditional s-process species, e.g., Zr, Ba, Ce, La, Sm, Y, etc. Estimates of (B-V), derived from these flux-calibrated spectra, show that from early November 1992 onward, the continuum grew progressively redder until by the end of 1992, the color of the central star became even redder than it was before the onset of the current episode. We caution that colors derived from aperture photometry may be seriously contaminated by the flux from emission lines of the planetary nebula surrounding FG Sge, and may cause the observed colors to appear anomalously too negative. The present results are compatible with a model in which the diminution in optical luminosity is the result of the ejection of a semitransparent dust shell by the central star, as proposed by Woodward et al. (1993, ApJL, in press). There is no compelling evidence to suggest that the central star is returning to its pre-1960 state within the domain of hot stars. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP STONE, RPS (reprint author), UNIV CALIF SANTA CRUZ OBSERV,LICK OBSERV,SANTA CRUZ,CA 95064, USA. NR 35 TC 12 Z9 12 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 1993 VL 105 IS 689 BP 755 EP 760 DI 10.1086/133227 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LN087 UT WOS:A1993LN08700008 ER PT J AU GINGERICH, O AF GINGERICH, O TI INVENTING THE FLAT EARTH - COLUMBUS AND MODERN HISTORIANS - RUSSELL,JB SO SPECULUM-A JOURNAL OF MEDIEVAL STUDIES LA English DT Book Review RP GINGERICH, O (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MEDIEVAL ACAD OF AMER PI CAMBRIDGE PA 1430 MASSACHUSETTS AVE, CAMBRIDGE, MA 02138 SN 0038-7134 J9 SPECULUM JI Speculum-J. Mediev. Stud. PD JUL PY 1993 VL 68 IS 3 BP 885 EP 885 DI 10.2307/2865060 PG 1 WC Medieval & Renaissance Studies SC Arts & Humanities - Other Topics GA LZ009 UT WOS:A1993LZ00900102 ER PT J AU ABUASAB, MS CANTINO, PD NOWICKE, JW SANG, T AF ABUASAB, MS CANTINO, PD NOWICKE, JW SANG, T TI SYSTEMATIC IMPLICATIONS OF POLLEN MORPHOLOGY IN CARYOPTERIS (LABIATAE) SO SYSTEMATIC BOTANY LA English DT Article ID VERBENACEAE AB Caryopteris, an Asian genus of 16 species, has greater pollen diversity than has been reported in any other genus of Labiatae. The pollen morphology of 15 species is documented here. Three pollen types are distinguished on the basis of exine structure and sculpturing: spinulose to spinose with slender, finely divided columellae (alternatively interpretable as an expanded tectum); verrucate with a well defined tectum and thick, sparsely branched columellae; and suprareticulate to microreticulate with moderately thick, sparsely branched columellae. Thirteen species are tricolpate, Caryopteris divaricata is triporate, and C. nepalensis is 6-pantocolpate. Pollen morphology and correlated variation in floral and fruit morphology suggest that Caryopteris comprises three primary phenetic groups. However, two recent cladistic analyses (one based in part on the pollen features documented here) indicate that the genus is para- or polyphyletic and that only one of the three phenetic subgroups is clearly monophyletic. Recircumscription of the genus is recommended, but this should await completion of current studies that will facilitate its subdivision into monophyletic taxa. C1 OHIO UNIV,DEPT ENVIRONM & PLANT BIOL,ATHENS,OH 45701. SMITHSONIAN INST,DEPT BOT,NHB 166,WASHINGTON,DC 20560. COLL SCI & TECHNOL,DEPT BIOL,ABU DIES,ISRAEL. OHIO STATE UNIV,DEPT PLANT BIOL,COLUMBUS,OH 43210. NR 29 TC 15 Z9 15 U1 1 U2 3 PU AMER SOC PLANT TAXONOMISTS PI BRONX PA NEW YORK BOTANICAL GARDEN, BRONX, NY 10458-5126 SN 0363-6445 J9 SYST BOT JI Syst. Bot. PD JUL-SEP PY 1993 VL 18 IS 3 BP 502 EP 515 DI 10.2307/2419422 PG 14 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA LP767 UT WOS:A1993LP76700009 ER PT J AU LONG, PO AF LONG, PO TI DIGIORGIO,FRANCESCO - CHECKLIST AND HISTORY OF MANUSCRIPTS AND DRAWINGS IN AUTOGRAPHS AND COPIES FROM CA 1470 TO 1687 AND RENEWED COPIES (1764-1839) - SCAGLIA,G SO TECHNOLOGY AND CULTURE LA English DT Book Review RP LONG, PO (reprint author), SMITHSONIAN INST,DIBNER LIB,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 1993 VL 34 IS 3 BP 674 EP 675 DI 10.2307/3106719 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA MC595 UT WOS:A1993MC59500011 ER PT J AU SHARRER, GT AF SHARRER, GT TI COLE,ROBERT WORLD - AGRICULTURE AND SOCIETY IN EARLY MARYLAND - CARR,LG, MENARD,RR, WALSH,LS SO TECHNOLOGY AND CULTURE LA English DT Book Review RP SHARRER, GT (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 1993 VL 34 IS 3 BP 694 EP 696 DI 10.2307/3106731 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA MC595 UT WOS:A1993MC59500023 ER PT J AU REUNOV, A RICE, ME AF REUNOV, A RICE, ME TI ULTRASTRUCTURAL OBSERVATIONS ON SPERMATOGENESIS IN PHASCOLION-CRYPTUM (SIPUNCULA) SO TRANSACTIONS OF THE AMERICAN MICROSCOPICAL SOCIETY LA English DT Article AB The testis of the sipunculan Phascolion cryptum extends as a narrow fringe of tissue along the base of the retractor muscle to the ventral nerve cord. Composed of groups of spermatogonia, it is, for the most part, covered by peritoneal cells. Clusters of germ cells are released from the testis into the coelomic fluid; the earliest stages in the coelom appear to be spermatocytes. Connected by intercellular bridges, the spermatocytes develop synchronously within a cluster. Proacrosomal vesicles, produced by several Golgi complexes, appear in primary spermatocytes. Also occurring as floating, synchronously developing clusters, the spermatids retain the intercellular connections. During spermiogenesis, the acrosomal vesicle, formed by a coalescence of small proacrosomal vesicles in the basal part of the spermatid, migrates to the apical part of the cell to complete the formation of the acrosome. Small mitochondria apparently unite to form the four or five large mitochondria of the midpiece of the mature sperm. The distal centriole has a pericentriolar complex consisting of nine radially oriented elements; it forms the basal body of the tail, which has a standard arrangement of axonemal microtubules (9 + 2). The structure of the fully formed spermatozoon is typical of the ''primitive'' type of sperm that has been noted previously for several species of sipunculans and some other marine invertebrates with external fertilization. C1 SMITHSONIAN MARINE STN LINK PORT,FT PIERCE,FL 34946. RP REUNOV, A (reprint author), ACAD SCI VLADIVOSTOK,INST MARINE BIOL,VLADIVOSTOK 690032,RUSSIA. NR 19 TC 11 Z9 17 U1 0 U2 1 PU AMER MICROSCOPICAL SOC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 SN 0003-0023 J9 T AM MICROSC SOC PD JUL PY 1993 VL 112 IS 3 BP 195 EP 207 DI 10.2307/3226678 PG 13 WC Microscopy SC Microscopy GA LY412 UT WOS:A1993LY41200002 ER PT J AU ORING, LW REED, JM ALBERICO, JAR FLEISCHER, RC AF ORING, LW REED, JM ALBERICO, JAR FLEISCHER, RC TI FEMALE CONTROL OF PATERNITY - MORE THAN MEETS THE EYE SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Letter ID SPOTTED SANDPIPER C1 SMITHSONIAN INST,GENET LAB,WASHINGTON,DC 20560. RP ORING, LW (reprint author), UNIV NEVADA,ECOL EVOLUT & CONSERVAT BIOL PROGRAM,1000 VALLEY RD,RENO,NV 89512, USA. NR 9 TC 3 Z9 3 U1 0 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, OXON, ENGLAND OX5 1GB SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD JUL PY 1993 VL 8 IS 7 BP 259 EP 259 DI 10.1016/0169-5347(93)90203-2 PG 1 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA LJ571 UT WOS:A1993LJ57100010 PM 21236163 ER PT J AU ROUSE, GW AF ROUSE, GW TI NEW FABRICIOLA SPECIES (POLYCHAETA, SABELLIDAE, FABRICIINAE) FROM THE EASTERN ATLANTIC, WITH A DESCRIPTION OF SPERM AND SPERMATHECAL ULTRASTRUCTURE SO ZOOLOGICA SCRIPTA LA English DT Article AB New species in the genus Fabriciola Friedrich are described. Fabriciola is defined by a single synapomorphy, the presence of non-vascularized, ventral filamentous appendages. Otherwise the genus is variable, with differences among species in chaetae, eyes, and peristomial organization. The new species, Fabriciola flammula, F. liguronis and F. parvus, reflect this heterogeneity. Fabriciola liguronis has spermathecae in the radiolar crown of females, the first record of these structures in Fabriciola, but F. flammula and F. parvus lack spermathecae. Sperm ultrastructure in all three species share apomorphies with other fabriciins, but vary in other respects. Fabriciola may be paraphyletic, but material of the type species F. spongicola (Southern, 1921) has been unobtainable so far, and detailed study of this species is required to define the genus Fabriciola adequately. RP ROUSE, GW (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT INVERTEBRATE ZOOL,WASHINGTON,DC 20560, USA. RI Rouse, Greg/F-2611-2010 OI Rouse, Greg/0000-0001-9036-9263 NR 23 TC 26 Z9 26 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0300-3256 J9 ZOOL SCR JI Zool. Scr. PD JUL PY 1993 VL 22 IS 3 BP 249 EP 261 DI 10.1111/j.1463-6409.1993.tb00356.x PG 13 WC Evolutionary Biology; Zoology SC Evolutionary Biology; Zoology GA MD857 UT WOS:A1993MD85700004 ER PT J AU MCLAUGHLIN, BM BELL, KL AF MCLAUGHLIN, BM BELL, KL TI ELECTRON COLLISIONAL EXCITATION OF INTERMULTIPLET 1S(2)2S(2)2P(3), 1S(2)2S2P(4) AND 1S(2)2S(2)2P(3) TO 1S(2)2S2P(4) FORBIDDEN TRANSITIONS IN O-II SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Article ID OPACITY CALCULATIONS; IMPACT EXCITATION; ATOMIC OXYGEN; STRENGTHS; PROGRAM; IONS AB Electron collisional excitation strengths are calculated, using an eleven-state ab initio R-matrix method in LS coupling, for singly ionized atomic oxygen. All intermultiplet forbidden n = 2 transitions from the 1s(2)2s(2)2p3 (4S(o), 2D(o), 2P(o)) and the 1s(2)2s2p4 (4P(e), 2D(e), 2P(e), 2S(e)) levels are investigated. Effective collision strengths and rate coefficients are also presented for all possible forbidden n = 2 transitions between these multiplets over the temperature range 5000-1000 000 K. These results have wide ranging applications in many laboratory and astrophysical plasmas and, being more accurate, should be used in preference to previous values available in the literature. C1 QUEENS UNIV BELFAST,DEPT APPL MATH & THEORET PHYS,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. RP MCLAUGHLIN, BM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 34 TC 13 Z9 13 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD JUN 28 PY 1993 VL 26 IS 12 BP 1797 EP 1812 DI 10.1088/0953-4075/26/12/008 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LQ268 UT WOS:A1993LQ26800008 ER PT J AU DUBINSKI, J DACOSTA, LN GOLDWIRTH, DS LECAR, M PIRAN, T AF DUBINSKI, J DACOSTA, LN GOLDWIRTH, DS LECAR, M PIRAN, T TI VOID EVOLUTION AND THE LARGE-SCALE STRUCTURE SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, THEORY; GALAXIES, CLUSTERING; LARGE-SCALE STRUCTURE OF UNIVERSE ID EINSTEIN-DESITTER UNIVERSE; GALAXIES; INFALL; MATTER AB We investigate the evolution and interaction of voids in an Einstein-de Sitter universe. Using N-body simulations, we study the growth of different configurations of negative top-hat density perturbations. We find that adjacent voids merge to form larger voids. Thin planar walls form between the merging voids. The peculiar velocity is tangential to a given wall and rises linearly from the wall center. The density contrast of the walls steadily declines as the walls are stretched by the greater rate of expansion within the new void resulting from the merger. A simple hierarchical configuration of negative perturbations demonstrates that smaller scale voids effectively disappear within larger voids as larger scales become nonlinear. The remnants of previous structure formation are frozen in within evolving voids. The evolution of a void is not significantly affected by the collapse of a neighboring positive perturbation of the same scale. The characteristic size of voids which fill the volume of the universe at a given epoch has a narrow distribution suggesting that the large-scale structure appears as a network of close-packed voids of approximately the same size. RP DUBINSKI, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 30 TC 80 Z9 80 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1993 VL 410 IS 2 BP 458 EP 468 DI 10.1086/172762 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LG695 UT WOS:A1993LG69500002 ER PT J AU PRIMINI, FA FORMAN, W JONES, C AF PRIMINI, FA FORMAN, W JONES, C TI HIGH-RESOLUTION X-RAY OBSERVATIONS OF THE CENTRAL REGION OF M31 WITH THE ROSAT SATELLITE SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (M31); GALAXIES, NUCLEI; X-RAYS, GALAXIES ID GLOBULAR-CLUSTERS; LUMINOSITY FUNCTIONS; ASTRONOMICAL DATA; UPPER LIMITS; BULGE; POPULATION; EVOLUTION; DYNAMICS; RATIO; STARS AB We report the results of a 48,000 s observation of the central approximately 34' of M31 with the ROSAT HRI. We detect 86 X-ray sources with luminosities above approximately 1.4 x 10(36) ergs s-1 (3.5 x 10(-4) counts s-1). Eighteen sources are identified with globular clusters and two with supernova remnants. A point source coincident with the optical and radio nucleus is also detected. The cumulative luminosity distribution for all sources within 5' (approximately 1 kpc) of the nucleus flattens below approximately 2 x 10(37) ergs s-1. An extrapolation of this distribution to fainter luminosities indicates that only approximately 15%-26% of the diffuse X-ray emission in the bulge can be attributed to faint unresolved sources from this distribution. Estimates for contributions from other, less luminous X-ray source populations cannot account for the remainder, and we conclude that much of the unresolved X-ray emission in the bulge is either truly diffuse or due to a new class of X-ray sources. A comparison of the current observations with Einstein observations made 10 years ago indicates that approximately 42% of the sources within 7.5' of the nucleus are variable. The spatial distribution and number density of X-ray sources in M31 appear distinctly different from those in our Galaxy. RP PRIMINI, FA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Primini, Francis/0000-0002-6077-0643; Forman, William/0000-0002-9478-1682 NR 48 TC 104 Z9 104 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1993 VL 410 IS 2 BP 615 EP 625 DI 10.1086/172779 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LG695 UT WOS:A1993LG69500019 ER PT J AU GWINN, CR BARTEL, N CORDES, JM AF GWINN, CR BARTEL, N CORDES, JM TI ANGULAR BROADENING OF PULSARS AND THE DISTRIBUTION OF INTERSTELLAR PLASMA FLUCTUATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, STRUCTURE; PULSARS, GENERAL; SUPERNOVA REMNANTS; TECHNIQUES, INTERFEROMETRIC ID LOW GALACTIC LATITUDES; COMPACT RADIO-SOURCE; SUPERNOVA REMNANT; DENSITY TURBULENCE; COSMIC-RAYS; SCATTERING; VLBI; SCINTILLATION; ACCELERATION; PROPAGATION AB Comparison of angular and temporal broadening for 10 pulsars suggests a uniform distribution of scattering material in the interstellar plasma with localized, strong scattering near young supernova remnants. Angular broadening and temporal broadening both measure the integrated strength of scattering along the line of sight, but with different weighting functions. Comparison of the two thus yields information on the distribution of scattering material along the line of sight. We report new measurements of angular diameter for the scattering disks of eight pulsars, and discuss two measurements from the literature. We compare these results with published measurements of temporal broadening. Scattering disks of four pulsars are unresolved, but are close to the speckle regime of interstellar scattering. Four of the objects show moderate scattering. In the context of a model consisting of a thin screen superposed on a uniform medium, comparison of angular and temporal broadening suggests that the localized component of scattering has strength approximately 3 times that of the uniform medium. Signals from the Crab (0531 + 21) and Vela (0833 - 45) pulsars are heavily scattered by their surrounding supernova remnants; scattering by the remnants is more than 38 times as strong as by the uniform medium. The fluctuations responsible for this scattering may be associated with cosmic-ray acceleration. We compare strengths and spatial spectra of the scattering material in the supernova remnants that enclose these pulsars, and in the supernova remnant CTB 80, which encloses pulsar 1951 + 32. Remnants show significant differences in scattering properties. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. YORK UNIV,DEPT PHYS & ASTRON,N YORK M3J 1P3,ONTARIO,CANADA. CORNELL UNIV,DEPT ASTRON,ITHACA,NY 14853. ARECIBO OBSERV,NATL ASTRON & IONOSPHERE CTR,ARECIBO,PR 00612. RP GWINN, CR (reprint author), UNIV CALIF SANTA BARBARA,DEPT PHYS,SANTA BARBARA,CA 93106, USA. NR 61 TC 51 Z9 51 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1993 VL 410 IS 2 BP 673 EP 685 DI 10.1086/172784 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LG695 UT WOS:A1993LG69500024 ER PT J AU DALPINO, EMD BENZ, W AF DALPINO, EMD BENZ, W TI 3-DIMENSIONAL SIMULATIONS OF PROTOSTELLAR JETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, JETS; HYDRODYNAMICS; ISM, JETS AND OUTFLOWS; SHOCK WAVES; STARS, MASS LOSS; STARS, PRE-MAIN-SEQUENCE ID HERBIG-HARO OBJECTS; INTERSTELLAR BOW SHOCKS; EMISSION-LINE PROFILES; PREDICTED LONG-SLIT; ASTROPHYSICAL JETS; YOUNG STARS; NUMERICAL SIMULATIONS; RESOLUTION; MODELS; SPECTROSCOPY AB We present the first results of fully three-dimensional (3D) simulations of supersonic, radiatively cooling jets using the smoothed particle hydrodynamics technique (SPH). Our results qualitatively agree with the two-dimensional (2D) simulations of Blondin, Fryxell, & Konigl (1990), although the removal of the axisymmetry has resulted in relevant structural differences, especially at the jet head where a cold shell is formed from the condensation of shock-heated material. In particular, we found that the shell is not only dynamically unstable but also may undergo oscillations in density, which are attributed to global thermal instabilities. These effects may have important consequences on the dynamics and emission pattern of the observed HH objects associated to young stellar jets. We discuss the implications of our results in the interpretation of the observed properties of the stellar jets and HH objects. We also compare the structure of radiative cooling and adiabatic 3D jets. C1 UNIV SAO PAULO, INST ASTRON & GEOFIS, BR-04301 SAO PAULO, BRAZIL. UNIV ARIZONA, LUNAR & PLANETARY LAB, TUCSON, AZ 85721 USA. UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85724 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RI de Gouveia Dal Pino, Elisabete/H-9560-2013 OI de Gouveia Dal Pino, Elisabete/0000-0001-8058-4752 NR 45 TC 63 Z9 63 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1993 VL 410 IS 2 BP 686 EP 695 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LG695 UT WOS:A1993LG69500025 ER PT J AU MORSE, JA HEATHCOTE, S CECIL, G HARTIGAN, P RAYMOND, JC AF MORSE, JA HEATHCOTE, S CECIL, G HARTIGAN, P RAYMOND, JC TI THE BOW SHOCK AND MACH DISK OF HH-111V SO ASTROPHYSICAL JOURNAL LA English DT Article DE SHOCK WAVES; STARS, INDIVIDUAL (HH 111); STARS, PRE-MAIN-SEQUENCE ID HERBIG-HARO OBJECTS; STELLAR JET; MODELS; STARS; VELOCITIES; WAVES AB We present spatially resolved line profiles in Halpha and [S II] lambdalambda6716, 6731 across the working surface region in the Herbig-Haro object HH 111V. Data were acquired with the Rutgers/CTIO imaging Fabry-Perot interferometer on the CTIO 4 m telescope at approximately 1.3'' FWHM spatial and approximately 35 km s-1 FWHM kinetic resolution. We separate Mach disk emission spatially and kinematically from the bow shock emission. We have used the Halpha flux measured at the apex of the bow shock to estimate the preshock density of approximately 200 cm-3. Our detailed measurements of the electron density as a function of position and velocity across the bow shock, combined with new models of the bow shock emission, show that an ambient magnetic field of approximately 30 muG inhibits the compression of the postshock gas. Our models indicate that the magnetic field also contributes to extending the cooling distance behind the shock to resolvable scales, as observed in the spatial separation of [S II] and Halpha in the emission-line images of Reipurth et al. However, the ram pressure at the bow shock HH 111V exceeds the magnetic energy density by a factor of approximately 10(3), so the magnetic field is not large enough to change the direction of the flow. The preshock medium must flow away from the stellar energy source at approximately 300 km s-1 to account for the observed kinematics of the line emission in HH 111V. Hence, this working surface is a secondary ejection moving into the wake of an earlier ejection. HH 111 is the third case (HH 34 and HH 47 are other examples) of a stellar jet where the brightest bow shock moves into the wake of a previous high-velocity ejection. Balancing the ram pressures in the bow shock and Mach disk yields an estimated jet-to-ambient density ratio approximately 10, similar to our previous estimate for the HH 34 jet (Morse et al.). C1 UNIV N CAROLINA,DEPT PHYS & ASTRON,CHAPEL HILL,NC 27599. CERRO TOLOLO INTERAMER OBSERV,LA SERENA,CHILE. UNIV MASSACHUSETTS,FIVE COLL RADIO ASTRON OBSERV,AMHERST,MA 01003. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 39 TC 55 Z9 55 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1993 VL 410 IS 2 BP 764 EP 776 DI 10.1086/172793 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LG695 UT WOS:A1993LG69500033 ER PT J AU STARK, G YOSHINO, K SMITH, PL ESMOND, JR ITO, K STEVENS, MH AF STARK, G YOSHINO, K SMITH, PL ESMOND, JR ITO, K STEVENS, MH TI HIGH-RESOLUTION ABSORPTION CROSS-SECTION MEASUREMENTS OF CARBON-MONOXIDE AT 20-K BETWEEN 96.7 AND 98.8 NANOMETERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE MOLECULAR DATA; TECHNIQUES, SPECTROSCOPIC; ULTRAVIOLET, GENERAL ID INTERSTELLAR CO; 115 NM; PHOTODISSOCIATION; MOLECULES; PHOTOABSORPTION; SPECTRA; BANDS AB Photoabsorption cross sections for five CO bands, at wavelengths between 96.7 and 98.8 nm, have been measured at high-resolution in a supersonic jet-cooled source at the Photon Factory synchrotron facility. New integrated cross sections are reported for the K-X, L'-X, and L-X bands. Low-temperature spectra of the J-X and W-X bands, which were used in the determination of the absorbing CO column densities, are also presented. The rotational structures of the K-X, L'-X, and L-X bands do not overlap in the low-temperature (almost-equal-to 20 K) spectra, allowing for the first unambiguous determination of these band oscillator strengths. We also report revised room temperature measurements of integrated cross sections for the K-X, L'-X, and L-X bands, in which distortions in the measured spectra due to insufficient instrumental resolution have been minimized; the revised room temperature integrated cross sections are consistent with the low-temperature results. C1 USN,RES LAB,EO HULBURT CTR SPACE RES,WASHINGTON,DC 20375. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NATL LAB HIGH ENERGY PHYS,PHOTON FACTORY,TSUKUBA,IBARAKI 305,JAPAN. RP STARK, G (reprint author), WELLESLEY COLL,DEPT PHYS,WELLESLEY,MA 02181, USA. OI Stevens, Michael/0000-0003-1082-8955 NR 22 TC 20 Z9 20 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1993 VL 410 IS 2 BP 837 EP 842 DI 10.1086/172801 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LG695 UT WOS:A1993LG69500041 ER PT J AU COOL, AM GRINDLAY, JE KROCKENBERGER, M BAILYN, CD AF COOL, AM GRINDLAY, JE KROCKENBERGER, M BAILYN, CD TI DISCOVERY OF MULTIPLE LOW-LUMINOSITY X-RAY SOURCES IN NGC-6397 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, CLOSE; GLOBULAR CLUSTERS, INDIVIDUAL, NGC-6397; X-RAYS, STARS ID POST-CORE-COLLAPSE; GLOBULAR-CLUSTERS; CATACLYSMIC VARIABLES; MASS; SYSTEMS AB We report the discovery of multiple low-luminosity X-ray sources near the center of the nearby post-core-collapse globular cluster NGC 6397. In an 18 ks exposure of the cluster with the ROSAT High Resolution Imager (HRI), seven distinct sources with significance greater than 4 u are detected in the 36' diameter field of view. At least three of these sources are very likely cluster members given their positions less than 1' from the cluster center. The source closest to the center is clearly extended and may be due to a group of three or more point sources which are incompletely resolved from one another. If this is the case, the cluster contains at least five point sources with luminosities in the range of L(x) congruent-to 2-10 x 10(31) ergs s-1 in the ROSAT band (0.1-2.4 keV). Additional fainter sources or low-level diffuse emission may also be required to fully account for the observed flux. These are the faintest X-ray sources known in globulars. Their luminosities, numbers, and spatial distribution are consistent with their being cataclysmic variables and support the hypothesis that the low-luminosity X-ray sources discovered with the Einstein Observatory (Hertz & Grindlay 1983) represent high-luminosity members of a larger population of CVs in clusters. C1 YALE UNIV,DEPT ASTRON,NEW HAVEN,CT 06511. RP COOL, AM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 36 TC 46 Z9 46 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1993 VL 410 IS 2 BP L103 EP L106 DI 10.1086/186890 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LG697 UT WOS:A1993LG69700012 ER PT J AU HERTZ, P GRINDLAY, JE BAILYN, CD AF HERTZ, P GRINDLAY, JE BAILYN, CD TI A SUPERSOFT VARIABLE LOW-LUMINOSITY X-RAY SOURCE IN THE GLOBULAR-CLUSTER M3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GLOBULAR CLUSTERS, INDIVIDUAL (M3); NOVAE, CATACLYSMIC VARIABLES; X-RAYS, STARS ID WHITE-DWARFS; SYSTEMS; BINARY; STATE; NOVAE AB The globular cluster M3 (NGC 5272) was observed twice with the ROSAT high-resolution imager in order to study the low-luminosity X-ray source 1E 1339.8 + 2837. In 1992 January 1E 1339.8 + 2837 had an X-ray luminosity of 2 x 10(35) ergs s-1 (0.1-2.4 keV), over an order of magnitude brighter than it was when observed with the Einstein Observatory. The source was unresolved and very soft (kT congruent-to 20 eV); such supersoft outbursts would be difficult to detect in the vast majority of globular clusters which are more heavily absorbed than M3. In 1992 June the source was too faint to be detected (<2.8 x 10(33) ergs s-1). The soft outburst luminosity (L(bol) congruent-to 1.2 x 10(36) ergs s-1) and the blackbody radius (R congruent-to 7.7 x 10(8) cm) suggest that 1E 1339.8 + 2837 is a cataclysmic variable in which much of the luminosity is generated by steady nuclear burning of accreted material on the surface of the white dwarf primary. C1 YALE UNIV,DEPT ASTRON,NEW HAVEN,CT 06511. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP HERTZ, P (reprint author), USN,RES LAB,EO HULBURT CTR SPACE RES,CODE 7621-5,WASHINGTON,DC 20375, USA. NR 40 TC 33 Z9 33 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 1993 VL 410 IS 2 BP L87 EP L90 DI 10.1086/186886 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LG697 UT WOS:A1993LG69700008 ER PT J AU WEEKES, TC AF WEEKES, TC TI GAMMA-RAY ASTRONOMY ABOVE 100 GEV SO ANNALS OF THE NEW YORK ACADEMY OF SCIENCES LA English DT Article ID CRAB-NEBULA; TEV; SEARCH; CYGNUS-X-3; RADIATION; EMISSION RP WEEKES, TC (reprint author), HARVARD UNIV,SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,POB 97,AMADO,AZ 85645, USA. NR 33 TC 0 Z9 0 U1 0 U2 0 PU NEW YORK ACAD SCIENCES PI NEW YORK PA 2 E 63RD ST, NEW YORK, NY 10021 SN 0077-8923 J9 ANN NY ACAD SCI JI Ann. N.Y. Acad. Sci. PD JUN 15 PY 1993 VL 688 BP 240 EP 249 DI 10.1111/j.1749-6632.1993.tb43900.x PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LM125 UT WOS:A1993LM12500020 PM 26469425 ER PT J AU WACHLIN, FC RYBICKI, GB MUZZIO, JC AF WACHLIN, FC RYBICKI, GB MUZZIO, JC TI A PERTURBATION PARTICLE METHOD FOR STABILITY STUDIES OF STELLAR-SYSTEMS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE INSTABILITIES; METHODS, NUMERICAL; CELESTIAL MECHANICS, STELLAR DYNAMICS AB We discuss a numerical method for investigating the stability of stellar systems that uses an analytic distribution function to describe a stellar system in equilibrium and 'perturbation particles' to represent departures from that equilibrium state. The particles are used only to represent the perturbation, and statistical fluctuations due to the finite number of particles are therefore much less severe than in full N-body codes. We provide a general description of the method, recipes for particular aspects of its implementation, and an example of its application to a simple model with known analytical solution. C1 CONSEJO NACL INVEST CIENTIFICAS & TECN REPUBL ARGENTINA,PROGRAMA FOTOMETRIA & ESTRUCTURA GALACT,RA-1900 LA PLATA,ARGENTINA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP WACHLIN, FC (reprint author), NATL UNIV LA PLATA,FAC CIENCIAS ASTRON & GEOFIS,RA-1900 LA PLATA,ARGENTINA. NR 6 TC 5 Z9 5 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 15 PY 1993 VL 262 IS 4 BP 1007 EP 1012 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LH525 UT WOS:A1993LH52500022 ER PT J AU YI, I VISHNIAC, ET AF YI, I VISHNIAC, ET TI STOCHASTIC-ANALYSIS OF THE INITIAL CONDITION CONSTRAINTS ON CHAOTIC INFLATION SO PHYSICAL REVIEW D LA English DT Article ID QUANTUM-FIELD-THEORY; SCALAR FIELD; UNIVERSE MODELS; DYNAMICS; FLUCTUATIONS; SPACE AB We use stochastic dynamics to examine the probability of successful inflation from various initial conditions at the Planck epoch. This approach allows us to approximate the.effect of strong quantum fluctuations at the earliest epoch of inflation, including fluctuations in the local expansion rate. The well-known classical attractors along the slow-roll trajectory exist even when large quantum fluctuations in the early Planck epoch are included. However, our results suggest that a significant fraction of the initial condition phase space which leads to a successful inflationary stage in the classical analysis actually fails to inflate. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP YI, I (reprint author), UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712, USA. NR 47 TC 14 Z9 14 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD JUN 15 PY 1993 VL 47 IS 12 BP 5280 EP 5294 DI 10.1103/PhysRevD.47.5280 PG 15 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA LH172 UT WOS:A1993LH17200013 ER PT J AU YI, I VISHNIAC, ET AF YI, I VISHNIAC, ET TI SCALAR FIELD QUANTUM FLUCTUATIONS AND FINE-TUNING IN CHAOTIC INFLATIONARY MODELS SO PHYSICAL REVIEW D LA English DT Article ID STOCHASTIC INFLATION; DENSITY PERTURBATIONS; SITTER SPACE; UNIVERSE; GENERATION AB During chaotic inflation, the dispersion of a scalar field can show interesting nonlinear effects. This is not seen in treatments which combine a deterministic description for the mean-field evolution with a diffusion approximation for the quantum fluctuations. We derive a criterion which distinguishes the diffusive regime from the nonlinear regime using stochastic dynamics in models of noninteracting multiple scalar fileds. In the nonlinear regime, dispersion estimates based on a simple diffusion approximation fail due to a strong nonlinear drift effect. We give some simple numerical examples to support this result. We apply our results to a double inflation model and show that estimates of the probability of successful inflation depend on a correct treatment of nonlinear effects. Including them greatly reduces the amount of fine-tuning necessary in this model. C1 UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712. RP YI, I (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Vishniac, Ethan/0000-0002-2307-3857 NR 28 TC 3 Z9 3 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD JUN 15 PY 1993 VL 47 IS 12 BP 5295 EP 5303 DI 10.1103/PhysRevD.47.5295 PG 9 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA LH172 UT WOS:A1993LH17200014 ER PT J AU SADEGHPOUR, HR CAVAGNERO, M AF SADEGHPOUR, HR CAVAGNERO, M TI FORMATION AND DECAY OF THE 3(1)4+ (1)P(O)AUTOIONIZING RESONANCE OF HELIUM SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Letter ID DOUBLY-EXCITED-STATES; PHOTOABSORPTION; CLASSIFICATION; ATOMS; RULES; HE AB We present results of an eigenchannel R-matrix calculation of the photoabsorption spectrum of He below He+(n = 3) hold. The observed n{upsilon}m(A) =3 {1}4+ resonance is found to decay with an 84.4% branching ratio to the 2{1}o ('2pepsilond') channel, in violation of a radial correlation propensity rule, DELTAA = 0. The DELTAupsilon = 0 propensity rule is satisfied, however, indicating that angular correlation is preserved in the decay of this resonance. C1 UNIV KENTUCKY,DEPT PHYS & ASTRON,LEXINGTON,KY 40506. RP SADEGHPOUR, HR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 21 TC 8 Z9 8 U1 1 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD JUN 14 PY 1993 VL 26 IS 11 BP L271 EP L274 DI 10.1088/0953-4075/26/11/002 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LJ826 UT WOS:A1993LJ82600002 ER PT J AU JACKSON, JBC JUNG, P COATES, AG COLLINS, LS AF JACKSON, JBC JUNG, P COATES, AG COLLINS, LS TI DIVERSITY AND EXTINCTION OF TROPICAL AMERICAN MOLLUSKS AND EMERGENCE OF THE ISTHMUS OF PANAMA SO SCIENCE LA English DT Article ID NEOGENE; GEOCHRONOLOGY AB The gradual closure of the Panamanian seaway and the resulting environmental change stimulated an increase in Caribbean molluscan diversity rather than the mass extinction hypothesized previously on the basis of inadequate data. Upheaval of molluscan faunas did occur suddenly throughout tropical America at the end of the Pliocene as a result of more subtle, unknown causes. There is no necessary correlation between the magnitude of regional shifts in abiotic conditions and the subsequent biological response. C1 NAT HIST MUSEUM,CH-4001 BASEL,SWITZERLAND. UNIV MICHIGAN,MUSEUM PALEONTOL,ANN ARBOR,MI 48109. RP JACKSON, JBC (reprint author), SMITHSONIAN TROP RES INST,CTR TROP PALEOECOL,UNIT 0948,APO AA,MIAMI,FL 34002, USA. NR 50 TC 142 Z9 145 U1 0 U2 14 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD JUN 11 PY 1993 VL 260 IS 5114 BP 1624 EP 1626 DI 10.1126/science.260.5114.1624 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LG176 UT WOS:A1993LG17600021 PM 17810203 ER PT J AU KNOWLTON, N WEIGT, LA SOLORZANO, LA MILLS, DK BERMINGHAM, E AF KNOWLTON, N WEIGT, LA SOLORZANO, LA MILLS, DK BERMINGHAM, E TI DIVERGENCE IN PROTEINS, MITOCHONDRIAL-DNA, AND REPRODUCTIVE COMPATIBILITY ACROSS THE ISTHMUS OF PANAMA SO SCIENCE LA English DT Article ID EASTERN PACIFIC; 2 SIDES; GENETICS; NEOGENE AB It is widely believed that gene flow connected many shallow water populations of the Caribbean and eastern Pacific until the Panama seaway closed 3.0 to 3.5 million years ago. Measurements of biochemical and reproductive divergence for seven closely related, transisthmian pairs of snapping shrimps (Alpheus) indicate, however, that isolation was staggered rather than simultaneous. The four least divergent pairs provide the best estimate for rates of molecular divergence and speciation. Ecological, genetic, and geological data suggest that gene flow was disrupted for the remaining three pairs by environmental change several million years before the land barrier was complete. RP KNOWLTON, N (reprint author), SMITHSONIAN TROP RES INST,UNIT 0948,APO AA,MIAMI,FL 34002, USA. RI Mills, DeEtta/G-8532-2015 OI Mills, DeEtta/0000-0002-9977-7834 NR 45 TC 387 Z9 395 U1 3 U2 43 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD JUN 11 PY 1993 VL 260 IS 5114 BP 1629 EP 1632 DI 10.1126/science.8503007 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LG176 UT WOS:A1993LG17600023 PM 8503007 ER PT J AU JONES, C STERN, C FALCO, E FORMAN, W DAVID, L SHAPIRO, I FABIAN, AC AF JONES, C STERN, C FALCO, E FORMAN, W DAVID, L SHAPIRO, I FABIAN, AC TI DISCOVERY OF A NEW COMPONENT IN THE GRAVITATIONALLY LENSED QUASAR 0957+561 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GRAVITATIONAL LENSING; QUASARS, INDIVIDUAL (0957+561); X-RAYS, GALAXIES ID RAY-EMITTING GAS; COOLING FLOWS; PERSEUS CLUSTER; DARK MATTER; GALAXIES; EINSTEIN; MODELS; Q0957+561; IMAGES; REGION AB We have analyzed Einstein High Resolution Imager (HRI) and Imaging Proportional Counter (IPC) observations of the gravitationally lensed quasar 0957 + 561. The X-ray emission appears as an approximate semicircle extending from the northern quasar image (A) to the southern image (B). We find unresolved X-ray emission associated with B, while A lies in an extended region. Although, for the epoch of the X-ray observations, the ratio of the optical flux from image B to that from image A is 0.76, the HRI observations show that the emission from around quasar image B is only about one-third that from image A. This difference in ratios implies the presence of another component in 0957 + 561. Since this ratio is found in each of the two HRI observations which were taken 6 months apart, it is unlikely that the difference in the ratios observed in X-ray and optical wavelengths is caused by dramatic changes in the quasar flux on a time scale less than the difference in the light propagation time for the two images. We use a model for the lens, including a giant galaxy and its surrounding cluster, to infer the X-ray source distribution and luminosity. This model implies the existence of an extended source of X-ray emission offset from the unresolved source associated with the quasar nucleus. The extended component has a diameter approximately 1'' to 3'', offset 0.''7 northeast of the quasar. The IPC observation of 0957 + 561 shows that the spectrum of the emission is soft compared to that of other X-ray emitting quasars. We discuss possible sources for the origin of the X-ray emission and suggest that it could arise from radiative cooling of hot gas surrounding the quasar. We also suggest that the detection of the extended emission in 0957 + 561 is possible only because of the large magnification provided by the intervening lens. C1 UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 OHA,ENGLAND. RP JONES, C (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,SMITHSONIAN ASTROPHYS OBSERV,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Forman, William/0000-0002-9478-1682 NR 31 TC 6 Z9 6 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1993 VL 410 IS 1 BP 21 EP 28 DI 10.1086/172720 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE330 UT WOS:A1993LE33000003 ER PT J AU SHASTRI, P WILKES, BJ ELVIS, M MCDOWELL, J AF SHASTRI, P WILKES, BJ ELVIS, M MCDOWELL, J TI QUASAR X-RAY-SPECTRA REVISITED SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ACTIVE; QUASARS, EMISSION LINES; QUASARS, GENERAL; RADIO CONTINUUM, GALAXIES; X-RAYS, GALAXIES ID FE-II EMISSION; OPTICALLY SELECTED QUASARS; RADIO LUMINOSITY FUNCTION; LOW-REDSHIFT QUASARS; VLA OBSERVATIONS; SEYFERT-GALAXIES; STELLAR OBJECTS; JET; QSOS; CATALOG AB A sample of 45 quasars observed by the IPC on the Einstein satellite is used to reexamine the relationship of the soft (0.2-3.5 keV) X-ray energy index with radio properties and the optical Fe ii emission. We find that (1) the tendency for radio-loud quasars to have systematically flatter X-ray energy indices than radio-quiet quasars is confirmed with the soft X-ray excess having negligible effect; (2) there is a tendency for the flatness of the X-ray slope to correlate with radio core dominance for radio-loud quasars, suggesting that a component of the X-ray emission is relativistically beamed; (3) for the radio-quiet quasars, the soft X-ray energy indices with a mean of approximately 1.0 are consistent with the indices found at higher energies (2-10 keV), although steeper than those observed for Seyfert 1 galaxies (also 2-10 keV) where the reflection model gives a good fit to the data; (4) the correlation of Fe II emission line strength with X-ray energy index is confirmed for radio-quiet quasars using a subset of 18 objects. The radio-loud quasars show no evidence for a correlation. This relation suggests a connection between the ionizing continuum and line emission from the broad emission-line region (BELR) of radio-quiet quasars, but in the opposite sense to that predicted by current photoionization models; (5) the correlations of X-ray slope with radio core dominance and Fe II equivalent width within the radio-loud and radio-quiet subclasses, respectively, imply that the observed wide range of X-ray energy indices is real rather than due to the large measuring uncertainties for individual objects. C1 UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OI Wilkes, Belinda/0000-0003-1809-2364 NR 67 TC 68 Z9 68 U1 1 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1993 VL 410 IS 1 BP 29 EP 38 DI 10.1086/172721 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE330 UT WOS:A1993LE33000004 ER PT J AU LADD, EF LADA, EA MYERS, PC AF LADD, EF LADA, EA MYERS, PC TI AN INFRARED SURVEY FOR EMBEDDED YOUNG STARS IN THE PERSEUS MOLECULAR CLOUD COMPLEX SO ASTROPHYSICAL JOURNAL LA English DT Article DE INFRARED, STARS; ISM, CLOUDS; STARS, PRE-MAIN-SEQUENCE ID CARBON-MONOXIDE EMISSION; HERBIG-HARO OBJECTS; DARK CLOUDS; DENSE CORES; OPTICAL OBSERVATIONS; BIPOLAR OUTFLOWS; PROTOSTARS; BARNARD-5; NGC-1333; EXTINCTION AB We searched the Perseus molecular cloud complex for isolated, embedded, and presumably young stars using the survey data collected with the Infrared Astronomical Satellite (IRAS) and previously published visual extinction data. Of the 23 source positions which satisfied both our IRAS color and visual extinction tests, we imaged 18 (the other five have been previously studied at 2 mum) and identified the 2 mum counterparts of 11 IRAS sources. We have estimated the luminosities and mean frequencies of these sources and compare these properties with a similarly selected group of sources from the Taurus-Aurip cloud. We find that the isolated sources in Perseus cloud have a slightly higher average luminosity and a distinctly lower average mean frequency than the sources in our Taurus sample. These results suggest that the Perseus cloud is intermediate in its star-forming character between the predominantly low-mass star-forming regions like Taurus, and those which are capable of producing very high mass stars, like the clouds in Orion. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. KITT PEAK NATL OBSERV,TUCSON,AZ 85726. RP LADD, EF (reprint author), UNIV HAWAII,INST ASTRON,2680 WOODLAWN DR,HONOLULU,HI 96822, USA. NR 63 TC 53 Z9 53 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1993 VL 410 IS 1 BP 168 EP 178 DI 10.1086/172735 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE330 UT WOS:A1993LE33000018 ER PT J AU TORRELLES, JM VERDESMONTENEGRO, L HO, PTP RODRIGUEZ, LF CANTO, J AF TORRELLES, JM VERDESMONTENEGRO, L HO, PTP RODRIGUEZ, LF CANTO, J TI FROM BIPOLAR TO QUADRUPOLAR - THE COLLIMATION PROCESSES OF THE CEPHEUS-A OUTFLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE H-PI REGIONS; ISM, INDIVIDUAL (CEPHEUS-A); ISM, JETS AND OUTFLOWS; ISM, MOLECULES ID HERBIG-HARO OBJECTS; OB3 MOLECULAR CLOUD; H-II REGIONS; STAR-FORMATION; INFRARED OBSERVATIONS; INTERSTELLAR AMMONIA; RADIO OBSERVATIONS; MASS OUTFLOW; CEP-A; CORE AB We present new high-angular (approximately 2'') and -velocity (approximately 0.3 km s-1) resolution observations in the (J, K) = (1, 1) and (2, 2) ammonia lines toward Cepheus A using the VLA D-configuration. As previously reported, the high-density gas is mainly distributed in three clumps, Cep A-1, Cep A-2, and Cep A-3. Cep A-1 and Cep A-3 constitute an interstellar elongated structure (approximately 2.'3 x 0.'4, or approximately 0.5 x 0.08 pc), with the stellar activity center located at its northwest edge. We find that Cep A-1 and Cep A-3 are located, respectively, between the two main pairs of the blue- and redshifted CO lobes of the quadrupolar molecular outflow. This implies that the interstellar disklike structure cannot collimate the bipolar outflow near its origin in the east-west direction. The high-velocity outflow and the photons of its powering source seem to be producing significant perturbations of the morphological, kinematical, and temperature structures at the edges of the ammonia condensations. We suggest that the interstellar high-density condensations are diverting and redirecting the molecular outflow at scales of approximately 0.05-0.5 pc, with Cep A-1 and Cep A-3 splitting in two halves, respectively, the blue- and redshifted lobes of an originally bipolar outflow already collimated in the east-west direction at circumstellar scales. Part of the high-density gas located at the edges of the interstellar ammonia condensations may be in the process of being incorporated into the general high-velocity molecular outflow by a dragging effect. However, the overall observed motions in the interstellar high-density gas could be bound by the observed mass in the region. HW 2 is embedded in a circumstellar (approximately 3.3 x 2.''3, or approximately 2400 x 1700 AU; pa. = 22-degrees) high-density [n(H2) congruent-to 3 x 10(7)(X(NH3)/10(-8))-1 cm-3] clump of approximately 2(X(NH3)/10(-8))-1 M.. The high rotational temperatures [T(R)(22-11) = 40-50 K] and the large velocity dispersions in the ammonia emission (sigma congruent-to 3-4 km s-1) found toward this position lead us to favor this object as the powering source of the high-velocity outflow. The observed motions of the circumstellar molecular gas could reflect the bound motions of the gas (e.g., rotation or infall) around a central mass of approximately 10-20 M., or alternatively the perturbation of the ps by the wind of the central source. This circumstellar clump could be related to the circumstellar disk previously suggested from infrared continuum and maser line observations. We find that gas temperatures as a function of the projected distance r with respect to HW 2 can be fitted by T(R)(22-11) is-proportional-to r(-alpha), with alpha = 0.3-0.6. These indices are quite similar to those expected if heating of the molecular gas is via collisions with hot dust heated by the radiation of the central star(s). The observed luminosity in the region is enough to heat the gas up to the observed temperatures. This analysis suggests that similar VLA studies of radial temperature profiles in other star-forming regions may be very useful for understanding heating processes and identifying exciting sources. C1 Univ Nacl Autonoma Mexico, INST ASTRON, MEXICO CITY 04510, DF, MEXICO. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP CSIC, INST ASTROFIS ANDALUCIA, AP CORREOS 3004, C SANCHO PANZA S-N, E-18080 GRANADA, SPAIN. OI Torrelles, Jose Maria/0000-0002-6896-6085 NR 51 TC 50 Z9 50 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1993 VL 410 IS 1 BP 202 EP 217 DI 10.1086/172738 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE330 UT WOS:A1993LE33000021 ER PT J AU FLEMING, TA GIAMPAPA, MS SCHMITT, JHMM BOOKBINDER, JA AF FLEMING, TA GIAMPAPA, MS SCHMITT, JHMM BOOKBINDER, JA TI STELLAR CORONAE AT THE END OF THE MAIN-SEQUENCE - A ROSAT SURVEY OF THE LATE M-DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, CORONAE; STARS, LATE-TYPE; X-RAYS, STARS ID ASTRONOMICAL DATA; STARS; LHS-2924 AB We present X-ray data, both detections and upper limits, from the ROSAT all-sky survey for most known M dwarfs later than type M5, as well as from selected ROSAT pointed observations of some of these stars. We compare these data with similar data for early M dwarfs in an attempt to probe the nature of the magnetic dynamo and coronal heating mechanism for the very late M dwarfs, which are presumably totally convective. Our results indicate that late M dwarfs can have coronae which are just as active as those for the early M dwarfs and that coronal heating efficiency for ''saturated'' stars (as evidenced from L(X)/L(bol)) does not drop at spectral type M6. C1 UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. MAX PLANCK INST EXTRATERR PHYS,W-8046 GARCHING,GERMANY. NATL OPT ASTRON OBSERV,NATL SOLAR OBSERV,TUCSON,AZ 85726. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 29 TC 119 Z9 119 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 1993 VL 410 IS 1 BP 387 EP 392 DI 10.1086/172755 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE330 UT WOS:A1993LE33000038 ER PT J AU DEVORKIN, D AF DEVORKIN, D TI INSIDE NASA - HIGH-TECHNOLOGY AND ORGANIZATIONAL-CHANGE IN THE AMERICAN SPACE PROGRAM - MCCURDY,HE SO NATURE LA English DT Book Review RP DEVORKIN, D (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD JUN 3 PY 1993 VL 363 IS 6428 BP 407 EP 407 DI 10.1038/363407a0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LE938 UT WOS:A1993LE93800042 ER PT J AU STANLEY, DJ WARNE, AG AF STANLEY, DJ WARNE, AG TI SEA-LEVEL AND INITIATION OF PREDYNASTIC CULTURE IN THE NILE DELTA SO NATURE LA English DT Article ID LATE QUATERNARY AB PREDYNASTIC occupation of the Nile valley and delta, dating back to at least 5000 BC, has been attributed by most archaeologists to environmental factors, primarily regional climate change and fluctuating Nile flood stages1-5. Here we propose instead that initiation of farming settlements in the Nile delta was closely related to eustatic sea level. We present geological analyses of late Quaternary subsurface sections throughout the delta which reveal that the deceleration in sea-level rise that occurred at about 6500-5500 BC was a prime factor in the accumulation of Nile silt, and the creation of the widespread and fertile delta plain. As rising sea level reduced the gradient of the river course, a system of meandering Nile distributaries evolved, with increased overbank deposition burying the former (early Holocene), partially vegetated sandy plain. The broadening, seasonally flooded, fecund plain, with its increasing plant cover, provided a setting that was conducive to evolving agricultural activity and was therefore instrumental in the development of Predynastic communities in the Nile delta. RP STANLEY, DJ (reprint author), SMITHSONIAN INST,MEDITERRANEAN BASIN PROGRAM,PALEOBIOL E-207 NMNH,WASHINGTON,DC 20560, USA. NR 30 TC 36 Z9 37 U1 0 U2 6 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD JUN 3 PY 1993 VL 363 IS 6428 BP 435 EP 438 DI 10.1038/363435a0 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LE938 UT WOS:A1993LE93800054 ER PT J AU JOHNSTON, PF AF JOHNSTON, PF TI THE ART OF MEDIEVAL TECHNOLOGY - IMAGES OF NOAH THE SHIPBUILDER - UNGER,RW SO AMERICAN NEPTUNE LA English DT Book Review RP JOHNSTON, PF (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU PEABODY MUSEUM PI SALEM PA E INDIA MARINE HALL, SALEM, MA 01970 SN 0003-0155 J9 AM NEPTUNE JI Am. Neptune PD SUM PY 1993 VL 53 IS 3 BP 209 EP 210 PG 2 WC History SC History GA LQ530 UT WOS:A1993LQ53000005 ER PT J AU KULIK, G AF KULIK, G TI SPECIAL ISSUE ON MULTICULTURALISM - EDITORS INTRODUCTION SO AMERICAN QUARTERLY LA English DT Editorial Material RP KULIK, G (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 SN 0003-0678 J9 AM QUART JI Am. Q. PD JUN PY 1993 VL 45 IS 2 BP R7 EP R8 PG 2 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA LG979 UT WOS:A1993LG97900001 ER PT J AU BACKWELL, PRY JENNIONS, MD AF BACKWELL, PRY JENNIONS, MD TI MATE CHOICE IN THE NEOTROPICAL FROG, HYLA-EBRACCATA - SEXUAL SELECTION, MATE RECOGNITION AND SIGNAL SELECTION SO ANIMAL BEHAVIOUR LA English DT Note C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP BACKWELL, PRY (reprint author), UNIV WITWATERSRAND,DEPT ZOOL,PRIVATE BAG 3,JOHANNESBURG 2050,SOUTH AFRICA. RI Jennions, Michael/C-7560-2009; Backwell, Patricia/C-8883-2009 OI Jennions, Michael/0000-0001-9221-2788; NR 12 TC 17 Z9 19 U1 1 U2 2 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD JUN PY 1993 VL 45 IS 6 BP 1248 EP 1250 DI 10.1006/anbe.1993.1150 PG 3 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA LH449 UT WOS:A1993LH44900020 ER PT J AU DIAFERIO, A RAMELLA, M GELLER, MJ FERRARI, A AF DIAFERIO, A RAMELLA, M GELLER, MJ FERRARI, A TI ARE GROUPS OF GALAXIES VIRIALIZED SYSTEMS SO ASTRONOMICAL JOURNAL LA English DT Article ID N-BODY SIMULATIONS; COMPACT-GROUPS; DARK MATTER; LUMINOSITY FUNCTION; REDSHIFT SURVEY; CFA SURVEY; EVOLUTION; CATALOG AB Groups are systems of galaxies with crossing times t(cr) much smaller than the Hubble time. Most of them have t(cr) < 0.1H-0(-1). The usual interpretation is that they are in virial equilibrium. We compare the data of the group catalog [Ramella et al., ApJ, 344, 57 (1989)] selected from the CfA redshift survey extension with different N-body models. We show that the distributions of kinematic and dynamical quantities of the groups in the CfA catalog can be reproduced by a single collapsing group observed along different line of sights. This result shows that (a) projection effects dominate the statistics of these systems, and (b) observed groups of galaxies are probably still in the collapse phase. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OSSERV ASTRON TRIESTE,I-34131 TRIESTE,ITALY. OSSERV ASTRON TORINO,I-10025 PINO TORINESE,ITALY. RP DIAFERIO, A (reprint author), UNIV MILAN,DIPARTIMENTO FIS,VIA CELORIA 16,I-20133 MILAN,ITALY. NR 43 TC 38 Z9 38 U1 0 U2 2 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 1993 VL 105 IS 6 BP 2035 EP 2046 DI 10.1086/116581 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE322 UT WOS:A1993LE32200003 ER PT J AU ALDCROFT, TL ELVIS, M BECHTOLD, J AF ALDCROFT, TL ELVIS, M BECHTOLD, J TI A SAMPLE OF LOBE-DOMINATED QUASARS WITH MG-II ABSORPTION-LINES SO ASTRONOMICAL JOURNAL LA English DT Article ID LOW-REDSHIFT QSOS; SPECTRA; SYSTEMS; SIZE AB We present a sample of quasars which are lobe-dominated in their radio emission and contain Mg II absorption line systems. This sample will be useful in a search for redshifted H I 21 cm absorbers which are along lines of sight different from the optical. These systems will allow the measurement of the linear size and related physical parameters of the absorption line clouds. Since quasars appropriate for this study are rare, building this sample requires a substantial database of radio and optical observations. We have defined a set of criteria for selecting these objects and obtained the necessary data, from the literature and from new optical and Very Large Array (VLA) observations, to assemble a sample based on these criteria. Out of 4234 Quasi Stellar Objects (QSOs), we find 31 lobe-dominated quasars which are appropriate for optical and radio absorption line study in the Northern hemisphere. We have obtained or located optical spectra for 29 of these 31 quasars. In the optical spectra we find 17 Mg II absorption systems, with redshifts between 0.3 and 1.4 and Mg II lambda2796 rest equivalent widths between 0.3 and 2.0 angstrom. Based on statistics of 21 cm absorption in Mg II selected QSOs we expect this sample of 17 systems to yield one or two new H I absorbers. In this paper we give an analysis of our criteria, discuss the sample, and present new VLA observations of 16 quasars. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. RP ALDCROFT, TL (reprint author), STANFORD UNIV,DEPT PHYS,STANFORD,CA 94305, USA. NR 34 TC 14 Z9 14 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 1993 VL 105 IS 6 BP 2054 EP 2063 DI 10.1086/116583 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE322 UT WOS:A1993LE32200005 ER PT J AU MAIA, MAG DACOSTA, LN GIOVANELLI, R HAYNES, MP AF MAIA, MAG DACOSTA, LN GIOVANELLI, R HAYNES, MP TI OBSERVATIONS OF SOUTHERN DWARF GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article ID SURFACE BRIGHTNESS GALAXIES; PISCES-PERSEUS SUPERCLUSTER; MORPHOLOGICAL SEGREGATION; REDSHIFT SURVEY; UNIVERSE; SAMPLE AB Here we present the results of neutral hydrogen observations of dwarf galaxies in the southern hemisphere. About half of the 88 objects observed are galaxies selected, but optically undetected, for the Southern Sky Redshift Survey. The remaining objects are smaller galaxies, down to the 1' diameter limit of the ESO catalog, in the southern and northern galactic caps (b > \30-degrees\ and -37.5-degrees less-than-or-equal-to delta less-than-or-equal-to -17.5-degrees). C1 OBSERV NACL,BR-20921 RIO JANEIRO,BRAZIL. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CORNELL UNIV,CTR RADIOPHYS & SPACE RES,ITHACA,NY 14853. RP MAIA, MAG (reprint author), CORNELL UNIV,NATL ASTRON & IONOSPHERE CTR,SPACE SCI BLDG,ITHACA,NY 14853, USA. NR 23 TC 7 Z9 7 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 1993 VL 105 IS 6 BP 2107 EP 2117 DI 10.1086/116588 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE322 UT WOS:A1993LE32200010 ER PT J AU SCHMIDT, BP KIRSHNER, RP SCHILD, R LEIBUNDGUT, B JEFFERY, D WILLNER, SP PELETIER, R ZABLUDOFF, AI PHILLIPS, MM SUNTZEFF, NB HAMUY, M WELLS, LA SMITH, RC BALDWIN, JA WELLER, WG NAVARETTE, M GONZALEZ, L FILIPPENKO, AV SHIELDS, JC STEIDEL, CC PERLMUTTER, S PENNYPACKER, C SMITH, CK PORTER, AC BOROSON, TA STATHAKIS, R CANNON, R PETERS, J HORINE, E FREEMAN, KC WOMBLE, DS STONE, RPS MARSCHALL, LA PHILLIPS, AC SAHA, A BOND, HE AF SCHMIDT, BP KIRSHNER, RP SCHILD, R LEIBUNDGUT, B JEFFERY, D WILLNER, SP PELETIER, R ZABLUDOFF, AI PHILLIPS, MM SUNTZEFF, NB HAMUY, M WELLS, LA SMITH, RC BALDWIN, JA WELLER, WG NAVARETTE, M GONZALEZ, L FILIPPENKO, AV SHIELDS, JC STEIDEL, CC PERLMUTTER, S PENNYPACKER, C SMITH, CK PORTER, AC BOROSON, TA STATHAKIS, R CANNON, R PETERS, J HORINE, E FREEMAN, KC WOMBLE, DS STONE, RPS MARSCHALL, LA PHILLIPS, AC SAHA, A BOND, HE TI PHOTOMETRIC AND SPECTROSCOPIC OBSERVATIONS OF SN-1990E IN NGC-1035 - OBSERVATIONAL CONSTRAINTS FOR MODELS OF TYPE-II SUPERNOVAE SO ASTRONOMICAL JOURNAL LA English DT Article ID LARGE MAGELLANIC CLOUD; BOLOMETRIC LIGHT-CURVE; DISTANCE SCALE; STANDARD STARS; CERRO-TOLOLO; SN-1987A; 1987A; SPECTROPHOTOMETRY; EMISSION; NGC-4618 AB We present 126 photometric and 30 spectral observations of SN 1990E spanning from 12 days before B maximum to 600 days past discovery. These observations show that SN 1990E was of type II-P, displaying hydrogen in its spectrum, and the characteristic plateau in its light curve. SN 1990E is one of the few SNe II which has been well observed before maximum light, and we present evidence that this SN was discovered very soon after its explosion. In the earliest spectra we identify, for the first time, several N II lines. We present a new technique for measuring extinction to SNe II based on the evolution of absorption lines, and use this method to estimate the extinction to SN 1990E, A(V) = 1.5 +/- 0. 3 mag. From our photometric data we have constructed a bolometric light curve for SN 1990E and show that, even at the earliest times, the bolometric luminosity was falling rapidly. We use the late-time bolometric light curve to show that SN 1990E trapped a majority of the gamma rays produced by the radioactive decay of Co-56, and estimate that SN 1990E ejected 0.073+0.018/+0.051 M. of Ni-56, an amount virtually identical to that of SN 1987A. C1 CERRO TOLOLO INTERAMER OBSERV,LA SERENA,CHILE. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. UNIV CALIF BERKELEY,CTR PARTICLE ASTROPHYS,BERKELEY,CA 94720. LAWRENCE BERKELEY LAB,BERKELEY,CA 94720. KITT PEAK NATL OBSERV,TUCSON,AZ 85702. ANGLO AUSTRALIAN OBSERV,EPPING,NSW 2121,AUSTRALIA. EL WHIPPLE OBSERV,AMADO,AZ 85721. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,WODEN,ACT 2606,AUSTRALIA. UNIV CALIF SAN DIEGO,CTR ASTROPHYS & SPACE SCI,LA JOLLA,CA 92093. UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064. GETTYSBURG COLL,DEPT PHYS,GETTYSBURG,PA 17325. UNIV WASHINGTON,DEPT ASTRON FM20,SEATTLE,WA 98195. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. RP SCHMIDT, BP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. RI Peletier, Reynier/B-9633-2012; Smith, Craig/D-7927-2015; Perlmutter, Saul/I-3505-2015; Hamuy, Mario/G-7541-2016; OI Smith, Craig/0000-0001-5829-8303; Perlmutter, Saul/0000-0002-4436-4661; Schmidt, Brian/0000-0001-6589-1287 NR 66 TC 47 Z9 47 U1 1 U2 7 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 1993 VL 105 IS 6 BP 2236 EP 2250 DI 10.1086/116602 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE322 UT WOS:A1993LE32200024 ER PT J AU FRANKLIN, F LECAR, M MURISON, M AF FRANKLIN, F LECAR, M MURISON, M TI CHAOTIC ORBITS AND LONG-TERM STABILITY - AN EXAMPLE FROM ASTEROIDS OF THE HILDA GROUP SO ASTRONOMICAL JOURNAL LA English DT Article ID ORIGINAL DISTRIBUTION; SOLAR-SYSTEM; RESONANCES; JUPITER; SATURN AB This paper calculates Lyapunov times, T(L), for certain members of the Hilda minor planets, a group that librates at the 3:2 mean motion resonance with Jupiter. We find that many are definitely chaotic, but that the resulting escape times T(c), obtained from a relation that we recently published [Lecar et al., AJ, 104, 1230 (1992)] does not conflict with their being present today. On the other hand, we show that bodies with libration amplitudes 10 to 20 deg larger than the maximum currently found would have escaped during the lifetime of the solar system. We interpret this behavior as ''observational'' support for the relation between T(L) and T(c) that LFM inferred from numerical simulations. Consideration of T(L)'s for real and hypothetical objects with low proper eccentricities at and near the Hilda group lends further support. RP FRANKLIN, F (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 9 TC 19 Z9 19 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 1993 VL 105 IS 6 BP 2336 EP 2343 DI 10.1086/116611 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE322 UT WOS:A1993LE32200033 ER PT J AU SODERBLOM, DR STAUFFER, JR MACGREGOR, KB JONES, BF AF SODERBLOM, DR STAUFFER, JR MACGREGOR, KB JONES, BF TI THE EVOLUTION OF ANGULAR-MOMENTUM AMONG ZERO-AGE MAIN-SEQUENCE SOLAR-TYPE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE OPEN CLUSTERS AND ASSOCIATIONS, GENERAL; STARS, EVOLUTION; STARS, ROTATION ID LOW-MASS STARS; HORIZONTAL-BRANCH STARS; CHROMOSPHERIC EMISSION; ROTATIONAL VELOCITIES; CONVECTIVE CORE; OPEN CLUSTERS; INTERMEDIATE; PLEIADES; MODELS; MEMBERS AB We consider a survey of rotation among F, G, and K dwarfs of the Pleiades in the context of other young clusters (alpha Persei and the Hyades) and pre-main-sequence (PMS) stars (in Taurus-Auriga and Orion) in order to examine how the angular momentum of a star like the Sun evolves during its early life on the main sequence. The rotation of PMS stars can be evolved into distributions like those seen in the young clusters if there is only modest, rotation-independent angular momentum loss prior to the ZAMS. Even then, the ultrafast rotators (UFRs, or ZAMS G and K dwarfs with v sin i greater-than-or-similar-to 30 km s-1) must owe their extra angular momentum to their conditions of formation and to different angular momentum loss rates above a threshold velocity, for it is unlikely that these stars had angular momentum added as they neared the ZAMS, nor can a spread in ages within a cluster account for the range of rotation seen. Only a fraction of solar-type stars are thus capable of becoming UFRs, and it is not a phase that all stars experience. Simple scaling relations (like the Skumanich relation) applied to the observed surface rotation rates of young solar-type stars cannot reproduce the way in which the Pleiades evolves into the Hyades, especially the dramatic convergence in rotation rates seen among the lowest masses. Also, the Hyades has a strongly mass-dependent distribution of rotation, a dependence that is subtle or absent in the Pleiades, at least for (B - V) greater-than-or-similar-to 0.6. We argue that invoking internal differential rotation in these ZAMS stars can explain several aspects of the observations and thus can provide a consistent picture of ZAMS angular momentum evolution. Models with gradual core-envelope recoupling during the early main sequence lifetime of a solar-type star reproduce the qualitative features of the observed distributions of rotational velocities. However, much better observations of PMS stars-especially those found under conditions akin to open clusters-are needed to better determine the initial conditions that these stars actually experience. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NATL CTR ATMOSPHER RES,HIGH ALTITUDE OBSERV,BOULDER,CO 80307. UNIV CALIF SANTA CRUZ,LICK OBSERV,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. RP SODERBLOM, DR (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 62 TC 108 Z9 108 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1993 VL 409 IS 2 BP 624 EP 634 DI 10.1086/172694 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LC832 UT WOS:A1993LC83200014 ER PT J AU HARTIGAN, P RAYMOND, J AF HARTIGAN, P RAYMOND, J TI THE FORMATION AND EVOLUTION OF SHOCKS IN STELLAR JETS FROM A VARIABLE WIND SO ASTROPHYSICAL JOURNAL LA English DT Article DE HYDRODYNAMICS; ISM, JETS AND OUTFLOWS; SHOCK WAVES; STARS, MASS LOSS; STARS, PRE-MAIN-SEQUENCE ID HERBIG-HARO OBJECTS; T-TAURI STARS; ENERGY-SOURCE; BOW SHOCK; STEADY; EMISSION; MODELS; HH-34 AB Recent observations of jets from young stars indicate that the bright emission knots in these jets form at least in part because the jet varies in velocity and produces low-velocity shocks in the flow. In this paper we use a one-dimensional fluid dynamics code that includes detailed cooling by line emission to investigate how shocks develop and evolve in a variable wind. Supersonic velocity perturbations in a jet always steepen and form a pair of shocks (called the ''forward'' and ''reverse'' shocks), which separate gradually as the flow evolves. Line emission from the hot ps between these shocks has a low-excitation spectrum and large radial and tangential motions with respect to the exciting source, in agreement with observations of stellar jets. The forward shock has a larger shock velocity than the reverse shock if a density enhancement accompanies the velocity perturbation. If there is no initial density perturbation then the forward and reverse shocks have equal shock velocities, and if the density perturbation is negative (corresponding to constant mass loss) then the reverse shock has a larger shock velocity. In all cases except the constant mass-loss scenario the forward shock radiates more [S II] lambdalambda6716, 6731 emission than the reverse shock because the material that encounters the reverse shock must first pass through a rarefaction wave. The total [S II] emission produced by modest (approximately 40 km s-1) velocity perturbations rises rapidly as the shocks develop, and then either increases or decreases gradually (depending on the size of the perturbation) over tens of years. Models with strong magnetic fields have lower line fluxes and lower excitation than models without fields, and the perturbations disperse more rapidly if a magnetic field is present. Knots from variable stellar jets show how much the stellar winds change over time scales of approximately 10 years. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP HARTIGAN, P (reprint author), UNIV MASSACHUSETTS,FIVE COLL ASTRON DEPT,AMHERST,MA 01003, USA. NR 37 TC 81 Z9 81 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 1993 VL 409 IS 2 BP 705 EP 719 DI 10.1086/172700 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LC832 UT WOS:A1993LC83200020 ER PT J AU YI, I VISHNIAC, ET AF YI, I VISHNIAC, ET TI INFLATIONARY STOCHASTIC DYNAMICS AND THE STATISTICS OF LARGE-SCALE STRUCTURE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE COSMOLOGY, THEORY; GALAXIES, FORMATION; LARGE-SCALE STRUCTURE OF UNIVERSE ID COLD DARK MATTER; NON-GAUSSIAN FLUCTUATIONS; N-BODY SIMULATIONS; DENSITY PERTURBATIONS; INITIAL CONDITIONS; CHAOTIC INFLATION; SITTER SPACE; UNIVERSE; GALAXIES; FIELD AB We examine the nonlinear multiplicative stochastic behavior of chaotic inflation with an emphasis on possible non-Gaussian statistics in initial conditions for cosmological large-scale structure formation. Large-scale mode-mode couplings are analyzed using stochastic dynamics. We reach the following conclusions: 1. Coarse-grained (long-wavelength) scalar fields become nonlinear stochastic variables whose evolution shows behavior unexpected in the classical analysis. The interplay between the classical roll-down (drift) and quantum mechanical fluctuations (diffusion) makes the evolution of the scalar fields extremely nonclassical. Only during the very late stages of chaotic inflation do the scalar fields acquire their classical interpretation (i.e., as deterministic variables). 2. The statistics of initial conditions for cosmological density fluctuations depend on the details of scalar field dynamics during inflation. A non-Gaussian distribution of density fluctuations is a generic feature in chaotic inflation models. However, the astrophysical importance of this effect is strongly model dependent. Generally, deviations from Gaussian statistics are dependent on the strength of the nonlinear self-interaction of the scalar fields. Adiabatic fluctuations were expected to show significant non-Gaussian effects in single shot inflation only on superhorizon scales due to the strong constraint imposed by the cosmic microwave background radiation anisotropy limit. This conclusion is valid for a wide range of models. 3. In a simple chaotic double inflation model, non-Gaussian effects can be astrophysically significant, especially on very large scales. In this model, non-Gaussian statistics can be weakly scale dependent. Non-Gaussian effects could be observable on large scales at a level of approximately a few standard deviations. We also find that some chaotic potentials, designed to give non-scale-invariant density fluctuations, result in strong non-Gaussian phase correlations. 4. In multiple field models, non-Gaussian effects can be important. This depends on the nature of the secondary fields (massive or massless). Multiple field dynamics can provide non-Gaussian statistics as well as nonflat (scale-dependent) spectra. We point out that initial conditions for the large-scale structure in inflationary scenarios in the simplest models are Gaussian to a very high precision. However, as we are forced to consider more finely tuned models of inflation, Gaussian initial conditions should not be taken for granted, even on astrophysically interesting (i.e., observable) scales. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP UNIV TEXAS, DEPT ASTRON, AUSTIN, TX 78712 USA. OI Vishniac, Ethan/0000-0002-2307-3857 NR 75 TC 16 Z9 16 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 1993 VL 86 IS 2 BP 333 EP 364 DI 10.1086/191782 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LD674 UT WOS:A1993LD67400001 ER PT J AU AVERY, JW SHAFAGATI, A TURNER, A WHEELER, JW WELDON, PJ AF AVERY, JW SHAFAGATI, A TURNER, A WHEELER, JW WELDON, PJ TI BETA-SPRINGENE IN THE PARACLOACAL GLAND SECRETIONS OF THE SMOOTH-FRONTED CAIMAN (PALEOSUCHUS-TRIGONATUS) SO BIOCHEMICAL SYSTEMATICS AND ECOLOGY LA English DT Note DE PARACLOACAL GLANDS; BETA-SPRINGENE; SMOOTH-FRONTED CAIMAN; PALEOSUCHUS-TRIGONATUS C1 TEXAS A&M UNIV SYST,DEPT BIOL,COLL STN,TX 77843. HOWARD UNIV,DEPT CHEM,WASHINGTON,DC 20059. SMITHSONIAN INST,NATL ZOOL PK,DEPT HERPETOL,WASHINGTON,DC 20008. NR 6 TC 14 Z9 15 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0305-1978 J9 BIOCHEM SYST ECOL JI Biochem. Syst. Ecol. PD JUN PY 1993 VL 21 IS 4 BP 533 EP 534 DI 10.1016/0305-1978(93)90112-5 PG 2 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA LG699 UT WOS:A1993LG69900014 ER PT J AU DONNAY, TJ BEISSINGER, SR AF DONNAY, TJ BEISSINGER, SR TI APPLE SNAIL (POMACEA-DOLIODES) AND FRESH-WATER CRAB (DILOCARCINUS-DENTATUS) POPULATION FLUCTUATIONS IN THE LLANOS OF VENEZUELA SO BIOTROPICA LA English DT Article DE APPLE SNAIL; DENSITY CHANGES; DILOCARCINUS; FRESH-WATER CRAB; LLANOS; POMACEA; POPULATION FLUCTUATION; SEASONAL STRATEGIES; VENEZUELA; WETLANDS ID KITE; SPECIALIST; BEHAVIOR AB From July through November 1988 and 1989, apple snail (Pomacea doliodes) and freshwater crab (Dilocarcinus dentatus) populations were surveyed in rice plantations and seasonal wetlands (or ''esteros'') in the llanos of Venezuela to determine seasonal changes in density and size. Rice plantation sites had significantly higher densities and larger snails than did estero sites. Snail density did not differ significantly between months or years. In contrast, the density and size of freshwater crabs varied significantly by month but not between habitats or years: crabs were smaller and in greatest numbers at the beginning of the rainy season, and then declined in density but increased in size by November. The sex ratio of D. dentatus was skewed towards females, a ratio which was consistent across habitats and months. Fluctuations in snail and crab density and size are discussed in relation to the effects of wetland flooding regimes on the life history characteristics of these animals. C1 YALE UNIV, SCH FORESTRY & ENVIRONM STUDIES, 205 PROSPECT ST, NEW HAVEN, CT 06511 USA. SMITHSONIAN INST, NATL ZOOL PK, DEPT ZOOL RES, WASHINGTON, DC 20008 USA. RI Beissinger, Steven/F-3809-2012 NR 38 TC 20 Z9 21 U1 2 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 EI 1744-7429 J9 BIOTROPICA JI Biotropica PD JUN PY 1993 VL 25 IS 2 BP 206 EP 214 DI 10.2307/2389184 PG 9 WC Ecology SC Environmental Sciences & Ecology GA LJ682 UT WOS:A1993LJ68200007 ER PT J AU PAEZ, VP BOCK, BC RAND, AS AF PAEZ, VP BOCK, BC RAND, AS TI INHIBITION OF EVOKED CALLING OF DENDROBATES-PUMILIO DUE TO ACOUSTIC INTERFERENCE FROM CICADA CALLING SO BIOTROPICA LA English DT Note DE AMBIENT NOISE; DENDROBATIDAE; INTERFERENCE; NEOTROPICS; POISON DART FROG; TERRITORY; VOCALIZATION ID SHIFTS; BIRDS C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP PAEZ, VP (reprint author), OHIO UNIV,DEPT BIOL SCI,ATHENS,OH 45701, USA. NR 16 TC 16 Z9 18 U1 1 U2 5 PU ASSN TROP BIOL PI ST LOUIS PA MISSOURI BOTANICAL GARDEN 2345 TOWER GROVE AVE, ST LOUIS, MO 63110 SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JUN PY 1993 VL 25 IS 2 BP 242 EP 245 DI 10.2307/2389189 PG 4 WC Ecology SC Environmental Sciences & Ecology GA LJ682 UT WOS:A1993LJ68200012 ER PT J AU LOWEN, R AF LOWEN, R TI GENIUS IN THE SHADOWS - LANOUETTE,W, SILARD,B SO BULLETIN OF THE ATOMIC SCIENTISTS LA English DT Book Review RP LOWEN, R (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU EDUC FOUNDATION NUCLEAR SCI PI CHICAGO PA 6042 SOUTH KIMBARK, CHICAGO, IL 60637 SN 0096-3402 J9 B ATOM SCI JI Bull. Atom. Scient. PD JUN PY 1993 VL 49 IS 5 BP 51 EP 52 PG 2 WC International Relations; Social Issues SC International Relations; Social Issues GA LD971 UT WOS:A1993LD97100018 ER PT J AU NEEDELL, AA AF NEEDELL, AA TI TRUTH IS OUR WEAPON - PROJECT TROY, POLITICAL WARFARE, AND GOVERNMENT-ACADEMIC RELATIONS IN THE NATIONAL-SECURITY STATE SO DIPLOMATIC HISTORY LA English DT Article RP NEEDELL, AA (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,DEPT SPACE HIST,WASHINGTON,DC 20560, USA. NR 75 TC 31 Z9 31 U1 0 U2 2 PU BLACKWELL SCIENCE INC PI CAMBRIDGE PA 238 MAIN ST, CAMBRIDGE, MA 02142 SN 0145-2096 J9 DIPLOMATIC HIST JI Dipl. Hist. PD SUM PY 1993 VL 17 IS 3 BP 399 EP 420 DI 10.1111/j.1467-7709.1993.tb00588.x PG 22 WC History SC History GA LN264 UT WOS:A1993LN26400003 ER PT J AU SCHNEIDER, LS MURRAY, SS AF SCHNEIDER, LS MURRAY, SS TI DISTRIBUTED COMPUTING NOW - APPLICATION ENVIRONMENTS SO DR DOBBS JOURNAL LA English DT Article C1 HARVARD SMITHSONIAN CTR ASTROPHYS,DIV HIGH ENERGY ASTROPHYS,CAMBRIDGE,MA 02138. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MILLER FREEMAN, INC PI SAN MATEO PA 411 BOREL AVE, SAN MATEO, CA 94402-3522 SN 1044-789X J9 DR DOBBS J JI Dr. Dobbs J. PD JUN PY 1993 VL 18 IS 6 BP 82 EP & PG 0 WC Computer Science, Software Engineering SC Computer Science GA KZ686 UT WOS:A1993KZ68600018 ER PT J AU FRENCH, RG NICHOLSON, PD COOKE, ML ELLIOT, JL MATTHEWS, K PERKOVIC, O TOLLESTRUP, E HARVEY, P CHANOVER, NJ CLARK, MA DUNHAM, EW FORREST, W HARRINGTON, J PIPHER, J BRAHIC, A GRENIER, I ROQUES, F ARNDT, M AF FRENCH, RG NICHOLSON, PD COOKE, ML ELLIOT, JL MATTHEWS, K PERKOVIC, O TOLLESTRUP, E HARVEY, P CHANOVER, NJ CLARK, MA DUNHAM, EW FORREST, W HARRINGTON, J PIPHER, J BRAHIC, A GRENIER, I ROQUES, F ARNDT, M TI GEOMETRY OF THE SATURN SYSTEM FROM THE 3 JULY 1989 OCCULTATION OF 28-SGR AND VOYAGER OBSERVATIONS SO ICARUS LA English DT Article ID RADIO OCCULTATION; URANIAN RINGS; STELLAR OCCULTATION; ENCKE GAP; FEATURES; ORBITS; IDENTIFICATION; ENCOUNTER; MOONLET; NEPTUNE C1 CORNELL UNIV,DEPT ASTRON,ITHACA,NY 14853. MIT,DEPT EARTH ATMOSPHER & PLANETARY SCI,CAMBRIDGE,MA 02139. MIT,DEPT PHYS,CAMBRIDGE,MA 02139. CALTECH,PALOMAR OBSERV,PASADENA,CA 91125. HARVARD SMITHSONIAN CTR ASTROPHYS,CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712. NEW MEXICO STATE UNIV,DEPT ASTRON,LAS CRUCES,NM 88003. KANSAS STATE UNIV AGR & APPL SCI,DEPT ART,MANHATTAN,KS 66506. NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. UNIV ROCHESTER,DEPT ASTRON,ROCHESTER,NY 14627. OBSERV PARIS,F-92190 MEUDON,FRANCE. RP FRENCH, RG (reprint author), WELLESLEY COLL,DEPT ASTRON,WELLESLEY,MA 02181, USA. RI Harrington, Joseph/E-6250-2011 NR 70 TC 66 Z9 66 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD JUN PY 1993 VL 103 IS 2 BP 163 EP 214 DI 10.1006/icar.1993.1066 PG 52 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LK928 UT WOS:A1993LK92800001 ER PT J AU HUBBARD, WB PORCO, CC HUNTEN, DM RIEKE, GH RIEKE, MJ MCCARTHY, DW HAEMMERLE, V CLARK, R TURTLE, EP HALLER, J MCLEOD, B LEBOFSKY, LA MARCIALIS, R HOLBERG, JB LANDAU, R CARRASCO, L ELIAS, J BUIE, MW PERSSON, SE BOROSON, T WEST, S MINK, DJ AF HUBBARD, WB PORCO, CC HUNTEN, DM RIEKE, GH RIEKE, MJ MCCARTHY, DW HAEMMERLE, V CLARK, R TURTLE, EP HALLER, J MCLEOD, B LEBOFSKY, LA MARCIALIS, R HOLBERG, JB LANDAU, R CARRASCO, L ELIAS, J BUIE, MW PERSSON, SE BOROSON, T WEST, S MINK, DJ TI THE OCCULTATION OF 28-SGR BY SATURN - SATURN POLE POSITION AND ASTROMETRY SO ICARUS LA English DT Article ID TITANS ATMOSPHERE; NEPTUNE; URANUS; MODELS; RADIUS C1 OBSERV ASTRON SAN PEDRO MARTIR,22860 ENSENADA,BAJA CALIFORNIA,MEXICO. CERRO TOLOLO INTERAMER OBSERV,LA SERENA 1353,CHILE. LOWELL OBSERV,FLAGSTAFF,AZ 86001. MT WILSON,PASADENA,CA 91101. LAS CAMPANAS OBSERV,PASADENA,CA 91101. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP HUBBARD, WB (reprint author), UNIV ARIZONA,TUCSON,AZ 85721, USA. RI Turtle, Elizabeth/K-8673-2012 OI Turtle, Elizabeth/0000-0003-1423-5751 NR 22 TC 27 Z9 27 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD JUN PY 1993 VL 103 IS 2 BP 215 EP 234 DI 10.1006/icar.1993.1067 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LK928 UT WOS:A1993LK92800002 ER PT J AU KULIK, G AF KULIK, G TI ASPIRATIONS AND ANXIETIES - NEW-ENGLAND WORKERS AND THE MECHANIZED FACTORY SYSTEM, 1815-1850 - ZANDERMAN,DA SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review RP KULIK, G (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD JUN PY 1993 VL 80 IS 1 BP 261 EP 262 DI 10.2307/2079751 PG 2 WC History SC History GA LE392 UT WOS:A1993LE39200049 ER PT J AU WINKER, K AF WINKER, K TI SPECIMEN SHRINKAGE IN TENNESSEE WARBLERS AND TRAILS FLYCATCHERS SO JOURNAL OF FIELD ORNITHOLOGY LA English DT Article AB Guidelines for morphometric sexing of monochromatic species are frequently based on museum specimens. These specimens tend to shrink when they dry, introducing a potential source of error that is typically ignored when sexing guidelines are applied to living birds. Shrinkage can amount to as much as 4% of the length of living body components, and investigators should correct their field data before applying museum-derived sexing criteria. Studies in the literature and data from Tennessee Warblers (Vermivora peregrina) and ''Traill's'' flycatchers (Empidonax ''traillii'') suggest that suitable correction factors will vary with taxon and body component. RP WINKER, K (reprint author), CONSERVAT & RES CTR,NATL ZOOL PK,FRONT ROYAL,VA 22630, USA. RI Winker, Kevin/M-2042-2014 OI Winker, Kevin/0000-0002-8985-8104 NR 16 TC 31 Z9 38 U1 0 U2 0 PU ASSOC FIELD ORNITHOLOGISTS PI BELOIT PA BELOIT COLLEGE, DEPT BIOLOGY, 700 COLLEGE ST, BELOIT, WI 53511 SN 0273-8570 J9 J FIELD ORNITHOL JI J. Field Ornithol. PD SUM PY 1993 VL 64 IS 3 BP 331 EP 336 PG 6 WC Ornithology SC Zoology GA LQ769 UT WOS:A1993LQ76900007 ER PT J AU WELDON, PJ DEMETER, BJ ROSSCOE, R AF WELDON, PJ DEMETER, BJ ROSSCOE, R TI A SURVEY OF SHED SKIN-EATING (DERMATOPHAGY) IN AMPHIBIANS AND REPTILES SO JOURNAL OF HERPETOLOGY LA English DT Note ID LIFE-HISTORY; ECOLOGY C1 TEXAS A&M UNIV SYST,DEPT BIOL,COLL STN,TX 77843. RP WELDON, PJ (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT HERPETOL,WASHINGTON,DC 20008, USA. NR 57 TC 26 Z9 38 U1 1 U2 6 PU SOC STUD AMPHIBIANS REPTILES PI OXFORD PA DEPT OF ZOOLOGY MIAMI UNIV, OXFORD, OH 45056 SN 0022-1511 J9 J HERPETOL JI J. Herpetol. PD JUN PY 1993 VL 27 IS 2 BP 219 EP 228 DI 10.2307/1564942 PG 10 WC Zoology SC Zoology GA MB996 UT WOS:A1993MB99600017 ER PT J AU PEIRIS, JSM DITTUS, WPJ RATNAYAKE, CB AF PEIRIS, JSM DITTUS, WPJ RATNAYAKE, CB TI SEROEPIDEMIOLOGY OF DENGUE AND OTHER ARBOVIRUSES IN A NATURAL-POPULATION OF TOQUE MACAQUES (MACACA-SINICA) AT POLONNARUWA, SRI-LANKA SO JOURNAL OF MEDICAL PRIMATOLOGY LA English DT Article DE CALIFORNIA SEROGROUP VIRUSES; LUMBO; SNOWSHOE HARE VIRUS; JAPANESE ENCEPHALITIS; BATAI; CHANDIPURA ID INFECTION AB A seroepidemiological study of arboviruses infecting 115 wild toque macaques (Macaca sinica) at Polonnaruwa, Sri Lanka showed a high prevalence of antibodies to dengue and Lumbo viruses. There was low seroprevalence of Chandipura (2/115) and Batai (1/115) virus antibodies, but no seropositivity to Chikungunya or Sindbis. There was no serological evidence of infection by Japanese encephalitis (JE) virus in spite of large human epidemics in the study area, indicating that toque macaques are unlikely to be an epidemiologically relevant host in the maintenance cycle of JE virus. C1 INST FUNDAMENTAL STUDIES,KANDY,SRI LANKA. UNIV PERADENIYA,FAC MED,DEPT MICROBIOL,PERADENIYA,SRI LANKA. SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20560. NR 24 TC 32 Z9 33 U1 0 U2 7 PU MUNKSGAARD INT PUBL LTD PI COPENHAGEN PA 35 NORRE SOGADE, PO BOX 2148, DK-1016 COPENHAGEN, DENMARK SN 0047-2565 J9 J MED PRIMATOL JI J. Med. Primatol. PD JUN PY 1993 VL 22 IS 4 BP 240 EP 245 PG 6 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA MH768 UT WOS:A1993MH76800002 PM 8230174 ER PT J AU GIBLINDAVIS, RM MUNDOOCAMPO, M BALDWIN, JG NORDEN, BB BATRA, SWT AF GIBLINDAVIS, RM MUNDOOCAMPO, M BALDWIN, JG NORDEN, BB BATRA, SWT TI DESCRIPTION OF BURSAPHELENCHUS-ABRUPTUS N-SP (NEMATA, APHELENCHOIDIDAE), AN ASSOCIATE OF A DIGGER BEE SO JOURNAL OF NEMATOLOGY LA English DT Article DE ANTHOPHORA-ABRUPTA; APHELENCHOIDIDAE; BEE; BURSAPHELENCHUS-ABRUPTUS N-SP; B-FRAUDULENTUS; B-KOLYMENSIS; B-MUCRONATUS; B-XYLOPHILUS; DUFOURS GLAND; MORPHOLOGY; MYCOPHAGY; NEMATODE; SCANNING ELECTRON MICROSCOPY; TAXONOMY ID PINE WOOD; BIOLOGY; GLANDS; TREES AB Bursaphelenchus abruptus n. sp., an associate of the digger bee, Anthophora abrupta (Hymenoptera: Anthophoridae), is described and illustrated. Bursaphelenchus abruptus n. sp. can be differentiated from other species of Bursaphelenchus by the absence of head annules, stylet length, length of the postuterine sac, shape of female tail, spicule morphology, and male caudal papillae arrangement. Two plant-pathogenic fungi, Monilinia fructicola and Botrytis cinerea, and a Monilia sp. isolated from an adult bee from Prince Georges County, Maryland, were good hosts for B. abruptus n. sp. Dauer juveniles (JIII) of B. abruptus n. sp. were isolated from the reproductive tracts of A. abrupta from Montgomery County, Alabama, for measurements and comparison with J2-JIII intermolts from a 4-week-old monoxenic culture on Monilia sp. Gonad lengths in dauer juveniles isolated from A. abrupta were highly variable (49 +/- 23 mum SD; range 21-93 mum; n = 29) compared with J2-JIII intermolts from culture (28 +/- 7 mum SD; range = 16-42 mum; n = 16), suggesting that postembryonic gonad development may continue while dauers are in the bee host. Adult males and females of B. abruptus n. sp. were examined with scanning electron microscopy (SEM) for ultrastructural comparisons with other members of the genus Bursaphelenchus. C1 UNIV CALIF RIVERSIDE,DEPT NEMATOL,RIVERSIDE,CA 92521. SMITHSONIAN INST,DEPT ENTOMOL,WASHINGTON,DC 20560. USDA,BEE RES LAB,BELTSVILLE,MD 20705. RP GIBLINDAVIS, RM (reprint author), UNIV FLORIDA,INST FOOD & AGR SCI,FT LAUDERDALE RES & EDUC CTR,3205 COLL AVE,FT LAUDERDALE,FL 33314, USA. NR 17 TC 32 Z9 42 U1 0 U2 3 PU SOC NEMATOLOGISTS PI LAKELAND PA 3012 SKYVIEW DRIVE, LAKELAND, FL 33801-7072 SN 0022-300X J9 J NEMATOL JI J. Nematol. PD JUN PY 1993 VL 25 IS 2 BP 161 EP 172 PG 12 WC Zoology SC Zoology GA LF982 UT WOS:A1993LF98200006 PM 19279754 ER PT J AU FAUST, MA AF FAUST, MA TI SURFACE-MORPHOLOGY OF THE MARINE DINOFLAGELLATE SINOPHYSIS-MICROCEPHALUS (DINOPHYCEAE) FROM A MANGROVE-ISLAND, TWIN CAYS, BELIZE SO JOURNAL OF PHYCOLOGY LA English DT Article DE BELIZE; DETRITUS; DINOPHYCEAE; DINOPHYSALES; LIGHT MICROSCOPY; MANGROVE; MARINE ENVIRONMENT; MORPHOLOGY; SCANNING ELECTRON MICROSCOPY; SINOPHYSIS-MICROCEPHALUS AB Sinophysis microcephalus Nie and Wang 1944 is a nonphotosynthetic, tropical, benthic, dinophysoid dinoflagellate. I isolated it from floating detritus on a subtropical mangrove island, Twin Cays, Belize, Central America, and describe its micromorphology from light and scanning electron micrographs. Cells of S. microcephalus are circular to subcircular and compressed laterally with a cell size of 42-44 mum long and 33-35 mum wide and with a length / width ratio of 1.25-1.28. Areolae are numerous, 368-550 per valve, ranging in size from 0.75 to 2.0 mum. Pores are oblong and deeper at the valve's center and pentagonal-shaped at the plate margin. The well-defined cingulum is narrow and deeply incised with a smooth surface. The epitheca is small, moderately convex, and divided into two large, highly ornate, asymmetrical plates: the left and right epithecal plates. The left epithecal plate bears two slightly curved, upright anterior projections located dorsally adjacent to the epithecal list, a relatively large opening, and three smaller openings compressed against the sagittal suture. The right plate contains a wide megacytic zone with two parallel ridges, a fairly large oblong apical pore in ventral position adjacent to the cingulum, and eight areolae each with a round, uniform-sized pore opening. There are two long and narrow sulcal lists, gently convex with a smooth edge without structure or ribs. The left sulcal list has an ear-shaped lobe, a form of a primitive dinophysoid list. The megacytic zone is smooth and expands unevenly during cell division. The epitheca and sulcus distinguishes S. microcephalus from all examined Dinophysis. RP FAUST, MA (reprint author), NATL MUSEUM NAT HIST,SMITHSONIAN INST,DEPT BOT,4201 SILVER HILL RD,SUITLAND,MD 20746, USA. NR 26 TC 22 Z9 24 U1 0 U2 0 PU PHYCOLOGICAL SOC AMER INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD JUN PY 1993 VL 29 IS 3 BP 355 EP 363 DI 10.1111/j.0022-3646.1993.00355.x PG 9 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA LJ876 UT WOS:A1993LJ87600014 ER PT J AU VANDERMEULEN, J AF VANDERMEULEN, J TI PLANNING FOR VJ-DAY BY THE UNITED-STATES-ARMY AIR FORCES AND THE ATOMIC-BOMB CONTROVERSY SO JOURNAL OF STRATEGIC STUDIES LA English DT Article RP VANDERMEULEN, J (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 41 TC 0 Z9 0 U1 0 U2 0 PU FRANK CASS CO LTD PI LONDON PA 11 GAINSBOROUGH ROAD, LONDON, ENGLAND E11 1RS SN 0140-2390 J9 J STRATEGIC STUD JI J. Strateg. Stud. PD JUN PY 1993 VL 16 IS 2 BP 227 EP 239 PG 13 WC International Relations; Political Science SC International Relations; Government & Law GA LX726 UT WOS:A1993LX72600004 ER PT J AU MARINESCU, M SADEGHPOUR, HR DALGARNO, A AF MARINESCU, M SADEGHPOUR, HR DALGARNO, A TI HIGH-FREQUENCY 2-PHOTON IONIZATION OF HELIUM AND CESIUM SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA B-OPTICAL PHYSICS LA English DT Article ID ALKALI-METAL ATOMS; MULTIPHOTON ABSORPTION; GROUND-STATE; HYDROGEN; THRESHOLD; FIELD; CS AB Calculations of the two-photon ionization of metastable levels of helium and the first three s levels of cesium are presented. The calculations are carried out to second order in a perturbation expansion and are valid for low laser intensities. The behavior of the ionization cross section at high photon frequencies omega is studied, and it is found that the N-photon ionization cross section behaves as sigma(N) is-proportional-to omega-(2N+1/2). This analytic asymptotic behavior is verified numerically in the case of two-photon ionization. RP MARINESCU, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 33 TC 8 Z9 8 U1 1 U2 7 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 SN 0740-3224 J9 J OPT SOC AM B JI J. Opt. Soc. Am. B-Opt. Phys. PD JUN PY 1993 VL 10 IS 6 BP 988 EP 992 DI 10.1364/JOSAB.10.000988 PG 5 WC Optics SC Optics GA LF374 UT WOS:A1993LF37400005 ER PT J AU KAPLAN, M ROSENTHAL, M AF KAPLAN, M ROSENTHAL, M TI BATTLEMENTS, TEMPLES AND THE LANDSCAPE OF TUKA - THE ARCHAEOLOGICAL RECORD OF A CULTURAL TRANSFORMATION IN 19TH-CENTURY FIJI SO JOURNAL OF THE POLYNESIAN SOCIETY LA English DT Article C1 SMITHSONIAN INST,WASHINGTON,DC 20560. RP KAPLAN, M (reprint author), VASSAR COLL,POUGHKEEPSIE,NY 12601, USA. NR 41 TC 2 Z9 2 U1 0 U2 0 PU POLYNESIAN SOC INC PI PRIVATE BAG PA ANTHROPOL DEPT UNIV AUCKLAND, PRIVATE BAG, AUCKLAND, NEW ZEALAND SN 0032-4000 J9 J POLYNESIAN SOC JI J. Polyn. Soc. PD JUN PY 1993 VL 102 IS 2 BP 121 EP 145 PG 25 WC Anthropology SC Anthropology GA LR314 UT WOS:A1993LR31400001 ER PT J AU ALLEN, ME OFTEDAL, OT ULLREY, DE AF ALLEN, ME OFTEDAL, OT ULLREY, DE TI EFFECT OF DIETARY CALCIUM-CONCENTRATION ON MINERAL-COMPOSITION OF FOX GECKOS (HEMIDACTYLUS-GARNOTI) AND CUBAN TREE FROGS (OSTEOPILUS-SEPTENTRIONALIS) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE GECKO; TREE FROG; DIET; CALCIUM; PHOSPHORUS; ENDOLYMPHATIC SAC; HEMIDACTYLUS-GARNOTI; OSTEOPILUS-SEPTENTRIONALIS AB The effects of two dietary calcium levels were evaluated in fox geckos (Hemidactylus garnoti) and Cuban tree frogs (Osteopilus septentrionalis). Individually housed geckos (n = 13) and frogs (n = 23) were fed for 7 mo on crickets that were manipulated to be either high (HiCa) or low (LoCa) in calcium concentration. Crickets in the HiCa treatment contained 1.26% calcium (Ca) and 0.89% phosphorus (P) on a dry matter basis (DMB), as compared with 0.23% Ca and 0.82% P (DMB) in LoCa crickets. At the end of the experiment, Ca and P concentrations of the frogs and geckos were analyzed. Geckos maintained on HiCa crickets contained more Ca (4.02% DMB) than did geckos fed LoCa crickets (3.43% DMB), but there were no differences in P concentrations. However, even HiCa geckos contained less Ca and P than did geckos that died before the experiment was begun (5.22% Ca, 2.18% P DMB). The decline in body Ca and P concentration may relate to the large amounts of Ca and P invested in egg production by some animals, as well as a lack of ultraviolet (UV) irradiation needed for vitamin D synthesis. Radiographic evaluation did not reveal any differences between HiCa and LoCa geckos in bone density or endolymphatic Ca stores. Dietary treatment did not produce differences in Ca, P, or radiographic appearance of the tree frogs, but there was a significant difference between males and females in Ca concentration (males, 4.7%; females, 3.5% DMB). No sexual difference in Ca concentration was found among wild-caught tree frogs (five males, 14 females). Although geckos and tree frogs responded differently to dietary Ca, we recommend that crickets or other insects be supplemented with Ca when used as food for reptiles and amphibians. Other factors such as water quality, UV light, photoperiod, transpiration, and reproductive status may also influence Ca homeostasis. C1 MICHIGAN STATE UNIV,DEPT ANIM SCI,E LANSING,MI 48824. RP ALLEN, ME (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 20 TC 12 Z9 14 U1 1 U2 11 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 1993 VL 24 IS 2 BP 118 EP 128 PG 11 WC Veterinary Sciences SC Veterinary Sciences GA LM648 UT WOS:A1993LM64800004 ER PT J AU DONOGHUE, AM JOHNSTON, LA ARMSTRONG, DL SIMMONS, LG WILDT, DE AF DONOGHUE, AM JOHNSTON, LA ARMSTRONG, DL SIMMONS, LG WILDT, DE TI BIRTH OF A SIBERIAN TIGER CUB (PANTHERA-TIGRIS-ALTAICA) FOLLOWING LAPAROSCOPIC INTRAUTERINE ARTIFICIAL-INSEMINATION SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Note DE TIGER; PANTHERA-TIGRIS; LAPAROSCOPY; ARTIFICIAL INSEMINATION; INTRAUTERINE ID INVITRO FERTILIZATION; SEMEN; SPERMATOZOA; EWES; PUMA AB A 7-yr-old female Siberian tiger (Panthera tigris altaica) was treated with equine chorionic gonadotropin followed 80 hr later by human chorionic gonadotropin (hCG) to stimulate follicular development and ovulation, respectively. Laparoscopy 46 hr after hCG revealed that the ovaries contained eight fresh corpora lutea and six preovulatory follicles. A 16-gauge catheter was inserted transabdominally into each uterine horn, and 16.8 x 10(6) motile spermatozoa (from a male designated by the Siberian Tiger Species Survival Plan [SSP]) were inseminated. Pregnancy was confirmed 45 days after insemination by ultrasound, and a single healthy male cub was born at 111 days of gestation. These results demonstrate for the first time that assisted reproductive technology can be used to produce genetically valuable offspring from parents identified and recommended by an SSP program. C1 HENRY DOORLY ZOO,OMAHA,NE 68107. RP DONOGHUE, AM (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ANIM HLTH,WASHINGTON,DC 20008, USA. NR 23 TC 33 Z9 33 U1 0 U2 9 PU AMER ASSOC Z00 VETERINARIANS PI MEDIA PA 6 NORTH PENNELL ROAD, MEDIA, PA 19063 SN 1042-7260 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD JUN PY 1993 VL 24 IS 2 BP 185 EP 189 PG 5 WC Veterinary Sciences SC Veterinary Sciences GA LM648 UT WOS:A1993LM64800013 ER PT J AU STANLEY, DJ CHEN, ZY AF STANLEY, DJ CHEN, ZY TI YANGTZE DELTA, EASTERN CHINA .1. GEOMETRY AND SUBSIDENCE OF HOLOCENE DEPOCENTER SO MARINE GEOLOGY LA English DT Letter AB Stratigraphic analysis of 59 borings serves to define the subsurface configuration of late Quaternary deposits of the outer Yangtze delta, including both subaerial lower plain and its contiguous submerged sector. Isopachous maps of the Holocene sediment section reveal a linear thickened trend parallel to the lower Yangtze estuary-Chongming island, which extends seaward (southeast) to the mid-shelf. Maps depicting depths of the Holocene to late Pleistocene contact also highlight this thickened northwest to southeast trend, and a deep downward-bowing depression formed by the sedimentary sequence seaward of the Yangtze mouth. Radiocarbon-dated facies in the cores serve to calculate long-term averaged subsidence rates for the Holocene section: 0.1 to 3.0 mm/year on land, and 1.6 to 4.4 mm/year at sea. This preliminary information is vital for planning coastal protection (erosion, salt water intrusion) in this densely populated, low-lying region vulnerable to marine inundation. C1 E CHINA NORMAL UNIV,DEPT GEOG,SHANGHAI 200062,PEOPLES R CHINA. RP STANLEY, DJ (reprint author), SMITHSONIAN INST,DIV SEDIMENTOL,E-207 NMNH,WASHINGTON,DC 20560, USA. NR 29 TC 33 Z9 35 U1 2 U2 7 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0025-3227 J9 MAR GEOL JI Mar. Geol. PD JUN PY 1993 VL 112 IS 1-4 BP 1 EP 11 DI 10.1016/0025-3227(93)90157-Q PG 11 WC Geosciences, Multidisciplinary; Oceanography SC Geology; Oceanography GA LL301 UT WOS:A1993LL30100001 ER PT J AU CHEN, ZY STANLEY, DJ AF CHEN, ZY STANLEY, DJ TI YANGTZE DELTA, EASTERN CHINA .2. LATE QUATERNARY SUBSIDENCE AND DEFORMATION SO MARINE GEOLOGY LA English DT Letter AB Late Quaternary deposits, examined on high-resolution seismic profiles, provide evidence of Recent subsidence of the outer Yangtze delta in the East China Sea. Deformed late Pleistocene strata and mud diapirs, tilted bedding, and gas-deformed structures in Holocene sequences record remobilization of underconsolidated sediment within and adjacent to the Yangtze depocenter. Deformation types and their specific position relative to the depocenter record displacement of sediment as a result of Quaternary overburden and probable compaction and deep-seated tectonic motion. The configuration of depositional sequences demonstrates that subsidence in the outer Yangtze delta has continued from the late Pleistocene to the present. C1 E CHINA NORMAL UNIV,DEPT GEOG,SHANGHAI 200062,PEOPLES R CHINA. SMITHSONIAN INST,DIV SEDIMENTOL,WASHINGTON,DC 20560. NR 25 TC 35 Z9 42 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0025-3227 J9 MAR GEOL JI Mar. Geol. PD JUN PY 1993 VL 112 IS 1-4 BP 13 EP 21 DI 10.1016/0025-3227(93)90158-R PG 9 WC Geosciences, Multidisciplinary; Oceanography SC Geology; Oceanography GA LL301 UT WOS:A1993LL30100002 ER PT J AU GAFFEY, MJ BURBINE, TH BINZEL, RP AF GAFFEY, MJ BURBINE, TH BINZEL, RP TI ASTEROID SPECTROSCOPY - PROGRESS AND PERSPECTIVES SO METEORITICS LA English DT Review ID REMOTE-SENSING IMPLICATIONS; INFRARED JHK PHOTOMETRY; NEAR-EARTH ASTEROIDS; LOW-ALBEDO ASTEROIDS; S-TYPE ASTEROIDS; REFLECTANCE SPECTRA; PARENT BODIES; OUTER-BELT; CARBONACEOUS CHONDRITES; AQUEOUS ALTERATION AB The following discussion is divided into seven major sections. The first section outlines the scientific background and justification for asteroid studies in the context of understanding the formation and early evolution of the solar system. The second section briefly reviews the nature and distribution of the asteroid population. The third section discusses several major unresolved issues in asteroid and meteorite science which can potentially be addressed by asteroid remote sensing investigations. The fourth section outlines the nature and definition of the asteroid taxonomic classes. The fifth section summarizes the existing asteroidal spectral (and other remote sensing) data sets which are used to determine compositions and the techniques employed in the interpretation of such data. The sixth section explores the compositional meaning and diversity of these taxonomic classes and suggests meteoritic analogues for the taxonomic types. The seventh section describes the conclusions-or preliminary results-of several recent asteroid investigations which have focused on particular unsolved issues of the asteroid-meteorite relationship and of the early solar system properties. The final section discusses the overall conclusions and future directions. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. MIT,DEPT EARTH ATMOSPHER & PLANETARY SCI,CAMBRIDGE,MA 02139. RP GAFFEY, MJ (reprint author), RENSSELAER POLYTECH INST,DEPT EARTH & ENVIRONM SCI,TROY,NY 12180, USA. NR 184 TC 151 Z9 151 U1 0 U2 3 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD JUN PY 1993 VL 28 IS 2 BP 161 EP 187 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA LJ270 UT WOS:A1993LJ27000003 ER PT J AU DEVORKIN, D AF DEVORKIN, D TI EXPLORING THE SUN - SOLAR SCIENCE SINCE GALILEO - HUFBAUER,K SO MINERVA LA English DT Book Review RP DEVORKIN, D (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MINERVA PI LONDON PA 19 NOTTINGHAM ROAD, LONDON, ENGLAND SW17 7EA SN 0026-4695 J9 MINERVA JI Minerva PD SUM PY 1993 VL 31 IS 2 BP 246 EP 252 PG 7 WC Education & Educational Research; History & Philosophy Of Science; Social Sciences, Interdisciplinary SC Education & Educational Research; History & Philosophy of Science; Social Sciences - Other Topics GA LN409 UT WOS:A1993LN40900007 ER PT J AU SYER, D NARAYAN, R AF SYER, D NARAYAN, R TI STEADY FLOW ON TO A CONVEYOR BELT - CAUSAL VISCOSITY AND SHEAR SHOCKS SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ACCRETION, ACCRETION DISKS; HYDRODYNAMICS; SHOCK WAVES ID INTERSTELLAR BUBBLES; INHOMOGENEOUS-MEDIUM; ACCRETION DISKS; EVOLUTION AB In hydrodynamics, a shock occurs when a supersonic flow encounters a downstream obstacle and makes a sudden transition to a subsonic velocity. There is a shock rather than a smooth transition because information about the downstream boundary condition, carried by sound waves, does not reach the supersonic upstream fluid. We describe here analogous shear shocks which occur when information about the transverse velocity, i.e. the component of velocity in the plane of the shock front, is unable to penetrate upstream. This could be the case were a fluid flowing perpendicularly on to a conveyor belt about which, even in principle, the fluid far upstream had no knowledge. We consider a model of viscosity which has a finite propagation speed of shear information, and show that it produces two kinds of shear shock. A 'pure shear shock' corresponds to a transition from a superviscous to a subviscous state with no discontinuity in the velocity. The transverse velocity is continuous throughout this shock; however, the velocity profile acquires an extra degree of freedom on the downstream side which is used to accommodate the downstream boundary condition. A 'mixed shear shock' has a shear transition occurring at the same location as a normal adiabatic or radiative shock. The flow makes a sudden jump from a supersonic superviscous velocity to a subsonic subviscous state, and there is a discontinuity in both the normal and transverse components of the velocity. A discontinuity in the transverse velocity is not usually allowed in a regular shock, but it is permitted in a mixed shear shock because of the introduction of causality into the model of viscous interactions. We derive a generalized version of the Rankine-Hugoniot conditions for mixed shear shocks and present self-consistent numerical solutions to a model two-dimensional problem in which an axisymmetric radially infalling stream encounters a spinning star. The numerical examples illustrate various features of the pure and mixed shear shocks. The calculations are performed using a polytropic equation of state with adiabatic shocks, as well as an ideal gas equation of state with radiative shocks. C1 UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 0HA,ENGLAND. CANADIAN INST THEORET ASTROPHYS,MACLENNAN LABS,TORONTO M5S 1A1,ON,CANADA. RP SYER, D (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 27 TC 11 Z9 11 U1 1 U2 1 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 1993 VL 262 IS 3 BP 749 EP 763 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LE855 UT WOS:A1993LE85500022 ER PT J AU BOYLE, JJ ALTUN, Z KELLY, HP AF BOYLE, JJ ALTUN, Z KELLY, HP TI PHOTOIONIZATION CROSS-SECTION CALCULATION OF ATOMIC TUNGSTEN SO PHYSICAL REVIEW A LA English DT Article ID RESONANCE STRUCTURE; PHOTO-IONIZATION AB A photoionization cross-section calculation of atomic tungsten is performed in the formalism of many-body perturbation theory for photon energies ranging from the ionization threshold of tungsten to 150 eV. Nonrelativistic orbitals are used in the basis set and relativistic corrections are included. We consider excitations from the 4f, 5s, 5p, 5d, and 6s subshells. The effects of the strong 5p(6)5d4-->5p(5)5d5 and 4f(14)5d4-->4f(13)5d5 transitions are included as resonant contributions to the 5d partial cross section. Our results indicate that the 5d partial cross section dominates the total cross section below 100 eV. C1 MARMARA UNIV,DEPT PHYS,ISTANBUL,TURKEY. UNIV VIRGINIA,DEPT PHYS,CHARLOTTESVILLE,VA 22901. RP BOYLE, JJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. RI Boyle, James/N-6634-2016 OI Boyle, James/0000-0003-0804-3390 NR 41 TC 16 Z9 16 U1 0 U2 2 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 1993 VL 47 IS 6 BP 4811 EP 4830 DI 10.1103/PhysRevA.47.4811 PG 20 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LF727 UT WOS:A1993LF72700037 ER PT J AU IMAMOGLU, A AF IMAMOGLU, A TI LOGICAL REVERSIBILITY IN QUANTUM-NONDEMOLITION MEASUREMENTS SO PHYSICAL REVIEW A LA English DT Note ID SYSTEM AB We show that it is possible to make a logically reversible quantum-nondemolition measurement of an optical-field photon number, where the measurement preserves all the information contained in the premeasurement wave function. The nonunitary dynamics of the proposed scheme is analyzed using a Monte Carlo wave-function approach. RP IMAMOGLU, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 20 TC 31 Z9 31 U1 1 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUN PY 1993 VL 47 IS 6 BP R4577 EP R4580 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LF727 UT WOS:A1993LF72700008 ER PT J AU SORLIN, O GUILLEMAUDMUELLER, D MUELLER, AC BORREL, V DOGNY, S POUGHEON, F KRATZ, KL GABELMANN, H PFEIFFER, B WOHR, A ZIEGERT, W PENIONZHKEVICH, YE LUKYANOV, SM SALAMATIN, VS ANNE, R BORCEA, C FIFIELD, LK LEWITOWICZ, M SAINTLAURENT, MG BAZIN, D DETRAZ, C THIELEMANN, FK HILLEBRANDT, W AF SORLIN, O GUILLEMAUDMUELLER, D MUELLER, AC BORREL, V DOGNY, S POUGHEON, F KRATZ, KL GABELMANN, H PFEIFFER, B WOHR, A ZIEGERT, W PENIONZHKEVICH, YE LUKYANOV, SM SALAMATIN, VS ANNE, R BORCEA, C FIFIELD, LK LEWITOWICZ, M SAINTLAURENT, MG BAZIN, D DETRAZ, C THIELEMANN, FK HILLEBRANDT, W TI DECAY PROPERTIES OF EXOTIC N-SIMILAR-OR-EQUAL-TO-28-S AND CL NUCLEI AND THE CA-48/CA-46 ABUNDANCE RATIO SO PHYSICAL REVIEW C LA English DT Article ID DELAYED NEUTRON EMISSION; ALLENDE METEORITE; ISOTOPIC ANOMALIES; MASS FORMULA; NUCLEOSYNTHESIS; INCLUSIONS; MODEL; SN-1987A; GANIL; RANGE AB Beta-decay half-lives and beta-delayed neutron-emission probabilities of the very neutron-rich nuclei 44S and Cl-45-47 have been measured. These isotopes, which lie at or close to the N = 28 magic shell, were produced in interactions of a 60 MeV/U 48Ca beam from GANIL (Grand Accelerateur National d'Ions Lourds) with a 64Ni target, and were separated by the doubly achromatic spectrometer LISE (Ligne d'Ions Super Epluches). Their decay was studied by a beta-n time correlation measurement. The results are compared to recent model predictions and indicate a rapid weakening of the N = 28 shell effect below Ca-48(20)28. The nuclear structure effects reflected in the decay properties of the exotic S and Cl isotopes may be the clue for the astrophysical understanding of the unusual 48Ca/46Ca abundance ratio measured in the solar system as well as the Ca-Ti-Cr anomalies observed in E. King inclusions of the Al-lende meteorite. C1 UNIV MAINZ, INST KERNCHEM, W-6500 MAINZ, GERMANY. JOINT INST NUCL RES, NUCL REACT LAB, DUBNA, RUSSIA. GRAND ACCELERATEUR NATL IONS LOURDS, F-14021 CAEN, FRANCE. CEN BORDEAUX, F-33170 GRADIGNAN, FRANCE. INST SCI MAT RAYONNEMENT, PHYS CORPUSCULAIRE LAB, F-14032 CAEN, FRANCE. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. INST ATOM PHYS, BUCHAREST, ROMANIA. MAX PLANCK INST ASTROPHYS, W-8046 GARCHING, GERMANY. AUSTRALIAN NATL UNIV, CANBERRA, ACT 2601, AUSTRALIA. RP CNRS, INST NATL PHYS NUCL & PHYS PARTICULES, INST PHYS NUCL, F-91406 ORSAY, FRANCE. NR 73 TC 137 Z9 137 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9985 EI 2469-9993 J9 PHYS REV C JI Phys. Rev. C PD JUN PY 1993 VL 47 IS 6 BP 2941 EP 2953 DI 10.1103/PhysRevC.47.2941 PG 13 WC Physics, Nuclear SC Physics GA LF956 UT WOS:A1993LF95600059 ER PT J AU COLLINS, MJ AF COLLINS, MJ TI 1ST AMONG EQUALS - THE SELECTION OF NASA SPACE SCIENCE EXPERIMENTS - NAUGLE,JE SO PUBLIC HISTORIAN LA English DT Book Review RP COLLINS, MJ (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD SUM PY 1993 VL 15 IS 3 BP 78 EP 81 PG 4 WC History SC History GA LQ704 UT WOS:A1993LQ70400020 ER PT J AU HARTQUIST, TW RAWLINGS, JMC WILLIAMS, DA DALGARNO, A AF HARTQUIST, TW RAWLINGS, JMC WILLIAMS, DA DALGARNO, A TI THE REGULATORY AND DIAGNOSTIC ROLES OF CHEMISTRY IN LOW-MASS STAR-FORMATION SO QUARTERLY JOURNAL OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article ID DENSE MOLECULAR CLOUDS; INTERSTELLAR CLOUDS; ASTRONOMICAL FLOWS; GAS CLOUDS; MODELS; ABUNDANCES; EVOLUTION; DIFFUSION; AMMONIA; CORES AB We describe the different types of interstellar clouds and those sub-units in them that develop in the process of low-mass star formation. An introduction to the ion-molecule chemistry that plays a role in the production of the simple molecules in those objects is given. Within the large clouds containing star forming regions, molecular clumps with visual extinctions of about one magnitude are observed to be numerous. We consider these clumps to be the progenitors of star forming regions. We argue that they are longer-lived than more opaque starless clumps because the ionization level, controlled by the S+ abundance, falls with increasing visual extinction, leading to a larger decay rate of turbulence and a decreasing contribution of turbulent pressure to cloud support. Once the collapse of a molecular clump with most gas phase sulphur in the form of S+ is initiated, the collapse probably occurs on a free-fall timescale and results in the formation of a cluster consisting of dense cores and an intercore medium. We present theoretical results for the chemical evolution during the collapse that leads to the appearance of such a cluster. Low-mass stars are born in dense cores, and the winds of the stars react on the core cluster, so that ablation of cores occurs. Molecular diagnostics of the wind-core interface structure, relevant to the study of the structures and evolution of a large variety of dynamic diffuse astronomical sources consisting of condensations embedded in more tenuous media, have been identified in theoretical investigations. For instance, one may determine whether mixing of gas occurs at a magnetized interface, or if mixing is inhibited and only momentum and energy transfer between wind and core gas takes place. The ablated core gas and stellar wind may settle in the intercore medium, and a subsequent generation of cores partially composed of the ablated gas and wind may form. We consider the chemical signatures that if observed would establish whether later generation cores actually form. The detailed mapping of emissions from a number of molecular species, and the interpretation of those data, would permit the inference of the time required for intercore gas to collapse to create cores and the survival time of the cores. Infall within a core to form a star has not been detected though young stars exist in many cores. Broad components should arise in infalling gas, and searches for broad wings associated with NH3 emission features have been unsuccessful. The absence of broad wings is possibly due to the freeze-out of NH3 onto dust grain surfaces. The abundances of some other species should actually rise as moderate freeze-out onto dust of heavy elements from the gas phase occurs. We identify species that should have emission features with broad components in collapsing cores, and discuss the insight that such detections will bring to our understanding of star formation. C1 UNIV OXFORD,DEPT PHYS ASTROPHYS,NUCL PHYS LAB,OXFORD OX1 3RH,ENGLAND. UMIST,DEPT MATH,MANCHESTER M60 1QD,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP HARTQUIST, TW (reprint author), MAX PLANCK INST EXTRATERRESTRIAL PHYS,W-8046 GARCHING,GERMANY. NR 50 TC 35 Z9 35 U1 0 U2 2 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8738 J9 Q J ROY ASTRON SOC JI Q. J. R. Astron. Soc. PD JUN PY 1993 VL 34 IS 2 BP 213 EP 233 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LF438 UT WOS:A1993LF43800006 ER PT J AU MASON, MA AF MASON, MA TI THE BLOOD-THAT-RUNS-THROUGH-THE-VEINS - THE CREATION OF IDENTITY AND A CLIENTS EXPERIENCE OF CUBAN-AMERICAN SANTERIA-DILOGUN DIVINATION SO TDR-THE DRAMA REVIEW-A JOURNAL OF PERFORMANCE STUDIES LA English DT Article C1 AMERICAN UNIV,DEPT PHILOSOPHY & RELIG,WASHINGTON,DC 20016. RP MASON, MA (reprint author), SMITHSONIAN INST,ANACOSTIA MUSEUM,WASHINGTON,DC 20560, USA. NR 32 TC 0 Z9 0 U1 0 U2 0 PU MIT PRESS PI CAMBRIDGE PA 55 HAYWARD ST JOURNALS DEPT, CAMBRIDGE, MA 02142 SN 1054-2043 J9 TDR-DRAMA REV-J PERF JI TDR-Drama Rev.-J. Perform. Stud. PD SUM PY 1993 VL 37 IS 2 BP 119 EP 130 DI 10.2307/1146253 PG 12 WC Theater SC Theater GA LF211 UT WOS:A1993LF21100008 ER PT J AU NORTON, RL AF NORTON, RL TI 1ST AUTUMNAL REPORT OF BIRDS FROM RUM CAY, BAHAMAS SO WILSON BULLETIN LA English DT Note C1 SMITHSONIAN MIGRATORY BIRD CTR,NATL ZOOL PK,WASHINGTON,DC 20008. NR 0 TC 1 Z9 1 U1 0 U2 0 PU WILSON ORNITHOLOGICAL SOC PI ANN ARBOR PA MUSEUM OF ZOOLOGY UNIV MICHIGAN, ANN ARBOR, MI 48109 SN 0043-5643 J9 WILSON BULL JI Wilson Bull. PD JUN PY 1993 VL 105 IS 2 BP 361 EP 364 PG 4 WC Ornithology SC Zoology GA LF571 UT WOS:A1993LF57100017 ER PT J AU RYAN, MJ RAND, AS AF RYAN, MJ RAND, AS TI SEXUAL SELECTION AND SIGNAL EVOLUTION - THE GHOST OF BIASES PAST SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY OF LONDON SERIES B-BIOLOGICAL SCIENCES LA English DT Article; Proceedings Paper CT DISCUSSION MEETING OF THE ROYAL SOC OF LONDON : THE EVOLUTION AND DESIGN OF ANIMAL SIGNALLING SYSTEMS CY OCT 28-29, 1992 CL LONDON, ENGLAND SP ROYAL SOC LONDON ID FEMALE MATE CHOICE; PHYSALAEMUS-PUSTULOSUS; MATING PREFERENCES; SENSORY EXPLOITATION; NEOTROPICAL FROG; PREDATION; PARADOX; MALES; MITE; LEK AB The evolution of female mating preferences is an important key to understanding the evolution of signal diversity. Several hypotheses for preference evolution invoke different processes but all can produce the same end results: thus comparisons of extant traits and preferences within and among populations have made little progress in discriminating among competing hypotheses. Some of these hypotheses, however, do make different predictions as to the historical sequence of trait-preference evolution, and thus can be discriminated with appropriate phylogenetic analyses. We explore this approach in an analysis of the evolution of calls and call preferences in a monophyletic group of frogs, the Physalaemus pustulosus species group. In this clade there are pre-existing preferences for four call traits. These data reject hypotheses that invoke coevolution (good genes, runaway sexual selection) and females evolving preferences to choose males providing better resources, and instead support the hypothesis of sensory exploitation that suggests that males evolve traits that match pre-existing biases in the female's sensory system. We suggest that some of the difficulty in understanding preference evolution might derive from defining a preference only by those extant stimuli that elicit the preference. Our results suggest that preferences might be more general, and that signal diversity might arise from alternative means for eliciting the same preference. Furthermore, we discuss some difficulties with utilizing both population-based comparisons and phylogenetic approaches and suggest that the greatest progress will be made by addressing the problem of preference evolution at several levels of analysis. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP RYAN, MJ (reprint author), UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712, USA. NR 44 TC 230 Z9 235 U1 3 U2 49 PU ROYAL SOC LONDON PI LONDON PA 6 CARLTON HOUSE TERRACE, LONDON, ENGLAND SW1Y 5AG SN 0962-8436 J9 PHILOS T ROY SOC B JI Philos. Trans. R. Soc. Lond. Ser. B-Biol. Sci. PD MAY 29 PY 1993 VL 340 IS 1292 BP 187 EP 195 DI 10.1098/rstb.1993.0057 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA LG324 UT WOS:A1993LG32400004 ER PT J AU BEEHLER, BM AF BEEHLER, BM TI BATESON AND PEACOCKS TAILS SO NATURE LA English DT Letter RP BEEHLER, BM (reprint author), SMITHSONIAN INST,DIV BIRDS,WILDLIFE CONSERVAT SOC & CONSERVAT INT,MRC 116,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 4 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD MAY 27 PY 1993 VL 363 IS 6427 BP 308 EP 308 DI 10.1038/363308b0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LD917 UT WOS:A1993LD91700033 PM 8497312 ER PT J AU IMAMOGLU, A YAMAMOTO, Y AF IMAMOGLU, A YAMAMOTO, Y TI NOISE SUPPRESSION IN SEMICONDUCTOR P-I-N JUNCTIONS - TRANSITION FROM MACROSCOPIC SQUEEZING TO MESOSCOPIC COULOMB BLOCKADE OF ELECTRON-EMISSION PROCESSES SO PHYSICAL REVIEW LETTERS LA English DT Article ID LASER; LIGHT AB We analyze noise suppression properties of a constant-current driven p-i-n heterojunction. It is shown that the junction capacitance and temperature determine the minimum measurement time required for obtaining sub-Poissonian electron injection. As the capacitance of the junction is reduced, the noise spectrum develops a ''regulated single electron emission peak'' at the single electron charging frequency, indicating regulation of the individual thermionic emission events and therefore a transition from macroscopic squeezing to Coulomb blockade regime. C1 STANFORD UNIV, EL GINZTON LAB, STANFORD, CA 94305 USA. NIPPON TELEGRAPH & TEL PUBL CORP, BASIC RES LABS, MUSASHINO, TOKYO 180, JAPAN. RP IMAMOGLU, A (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, 60 GARDEN ST, MS 14, CAMBRIDGE, MA 02138 USA. RI Yamamoto, Yoshihisa/A-2811-2012 NR 12 TC 51 Z9 51 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD MAY 24 PY 1993 VL 70 IS 21 BP 3327 EP 3330 DI 10.1103/PhysRevLett.70.3327 PG 4 WC Physics, Multidisciplinary SC Physics GA LC943 UT WOS:A1993LC94300038 ER PT J AU HUCHRA, J AF HUCHRA, J TI THE ANDROMEDA GALAXY - HODGE,P SO SCIENCE LA English DT Book Review RP HUCHRA, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAY 21 PY 1993 VL 260 IS 5111 BP 1175 EP 1175 DI 10.1126/science.260.5111.1175 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA LC942 UT WOS:A1993LC94200050 PM 17806359 ER PT J AU MOULD, JR AKESON, RL BOTHUN, GD HAN, M HUCHRA, JP ROTH, J SCHOMMER, RA AF MOULD, JR AKESON, RL BOTHUN, GD HAN, M HUCHRA, JP ROTH, J SCHOMMER, RA TI THE VELOCITY-FIELD OF CLUSTERS OF GALAXIES WITHIN 100-MEGAPARSECS .2. NORTHERN CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, OBSERVATIONS; GALAXIES, CLUSTERING; GALAXIES, DISTANCES AND REDSHIFTS; RADIO LINES, ATOMIC ID POOR CLUSTERS; REDSHIFT SURVEY; DISTANCE SCALE; IRAS GALAXIES; CD GALAXIES; WIDTH RELATION; SUPERCLUSTER; MOTION AB Distances and peculiar velocities for galaxies in eight clusters and groups have been determined by means of the near-infrared Tully-Fisher relation. With the possible exception of a group halfway between us and the Hercules Cluster, we observe peculiar velocities of the same order as the measuring errors of approximately 400 km s-1. This result is consistent with the earlier Arecibo study by Aaronson and coworkers. The present sample is drawn from the northern galactic hemisphere and delineates a quiet region in the Hubble flow. This contrasts with the large-scale flows seen in the Hydra-Centaurus and Perseus-Pisces regions. We compare the observed peculiar velocities with predictions based upon the gravity field inferred from the IRAS redshift survey. The differences between the observed and predicted peculiar motions are generally small, except near dense structures, where the observed motions exceed the predictions by significant amounts. Kinematic models of the velocity field are also compared with the data. We cannot distinguish between parameterized models with a great attractor or models with a bulk flow. C1 NATL ASTRON & IONOSPHER CTR,ARECIBO OBSERV,ARECIBO,PR. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CERRO TOLOLO INTERAMER OBSERV,LA SERENA,CHILE. UNIV OREGON,EUGENE,OR 97403. UNIV TEXAS,DEPT ASTRON,AUSTIN,TX 78712. RP MOULD, JR (reprint author), CALTECH,PALOMAR OBSERV,105-24,PASADENA,CA 91125, USA. NR 60 TC 62 Z9 62 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1993 VL 409 IS 1 BP 14 EP 27 DI 10.1086/172638 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LB038 UT WOS:A1993LB03800002 ER PT J AU KUIJKEN, K AF KUIJKEN, K TI SELF-CONSISTENT MODELS FOR TRIAXIAL GALAXIES WITH FLAT ROTATION CURVES - THE DISK CASE SO ASTROPHYSICAL JOURNAL LA English DT Article DE CELESTIAL MECHANICS, STELLAR DYNAMICS; GALAXIES, KINEMATICS AND DYNAMICS; GALAXIES, STRUCTURE ID SCALE-FREE MODELS; ELLIPTICAL GALAXIES; DENSITY; HALOS AB We examine the possibility of constructing scale-free triaxial logarithmic potentials self-consistently, using Schwarzschild's linear programing method. In particular, we explore the limit of nonaxisymmetric disks. In this case it is possible to reduce the problem to the self-consistent reconstruction of the disk surface density on the unit circle, a considerably simpler problem than the usual two- or three-dimensional one. Models with surface densities of the form SIGMA = [x(n) + (y/q)] -1/n with n = 2 or 4 are investigated. We show that the complicated shapes of the ''boxlet'' orbit families (which replace the box orbit family found in potentials with smooth cores) limit the possibility of building self-consistent models, though elliptical disks of axis ratio above 0.7 and a restricted range of boxier models can be constructed. This result relies on using sufficiently fine bins, smaller than the 10-degrees bins commonly used in two- or three-dimensional investigations. It also indicates the need for caution in interpreting N-body models of triaxial halos in which the core of the potential is numerically smoothed. RP KUIJKEN, K (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MAIL STOP 20,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 19 TC 21 Z9 21 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1993 VL 409 IS 1 BP 68 EP 74 DI 10.1086/172642 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LB038 UT WOS:A1993LB03800006 ER PT J AU SITKO, ML SITKO, AK SIEMIGINOWSKA, A SZCZERBA, R AF SITKO, ML SITKO, AK SIEMIGINOWSKA, A SZCZERBA, R TI MULTIFREQUENCY OBSERVATIONS OF THE OPTICALLY-ACTIVE RADIO-QUIET QUASAR GQ COMAE .2. ULTRAVIOLET, OPTICAL, AND INFRARED CONTINUUM VARIABILITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE DUST, EXTINCTION; GALAXIES, PHOTOMETRY; INFRARED, GALAXIES; QUASARS, INDIVIDUAL (GQ COMAE); ULTRAVIOLET, GALAXIES ID ACCRETION DISK MODELS; BROAD-LINE REGION; GALACTIC NUCLEI; ENERGY-DISTRIBUTIONS; UBVRI PHOTOMETRY; BLACK-HOLE; POLARIZATION; EMISSION; SPECTRA; TEMPERATURE AB This paper summarizes the data and preliminary results of a 3 yr long project to monitor the continuum variability of GQ Comae (PG 1202 + 281) from 0.12 mum to 3.5 mum. Substantial variability in the optical/ultraviolet flux was observed. The variability is examined using a geometrically thin accretion disk model. The model is able to reproduce the variations, but contains problems with physical consistency. A comparison of the optical/ultraviolet data and the infrared data indicates that the flux at 2.2 mum did not respond to the optical-ultraviolet continuum increase until nearly 250 days after the outburst and suggests that the variable flux at this wavelength is due to heated dust. We model the infrared emission with a dust component which is heated by the radiation from the accretion disk. We show that a simple model using a disklike distribution Of heated dust grains can explain most of the infrared variability in a natural way. C1 UNIV CINCINNATI,CINCINNATI OBSERV,CINCINNATI,OH 45221. NICOLAUS COPERNICUS ASTRON CTR,PL-00716 WARSAW,POLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85724. KITT PEAK NATL OBSERV,NATL OPT ASTRON OBSERV,TUCSON,AZ 85726. UNIV HAWAII,INFRARED TELESCOPE FACIL,HONOLULU,HI 96822. RP SITKO, ML (reprint author), UNIV CINCINNATI,DEPT PHYS,CINCINNATI,OH 45221, USA. NR 54 TC 28 Z9 28 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1993 VL 409 IS 1 BP 139 EP 148 DI 10.1086/172649 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LB038 UT WOS:A1993LB03800013 ER PT J AU GOMEZ, JF TORRELLES, JM TAPIA, M GOMEZ, Y RODRIGUEZ, LF ROTH, M HO, PTP AF GOMEZ, JF TORRELLES, JM TAPIA, M GOMEZ, Y RODRIGUEZ, LF ROTH, M HO, PTP TI FURTHER-STUDIES ON THE CHAMPAGNE PHASE OF GM-24 (IRAS-17136-3617) SO ASTROPHYSICAL JOURNAL LA English DT Article DE H-II REGIONS; ISM, INDIVIDUAL (GM-24); RADIO CONTINUUM, INTERSTELLAR ID H-II REGIONS AB We observed with the VLA the H II region associated with the cometary nebula GM 24 at the 3.6 and 6 cm continuum, the H92alpha recombination line, and the water maser line. These observations suggest the presence of a ''champagne'' flow of ionized gas. We detected two extended radio continuum sources emitting optically thin free-free radiation. The stronger one [S(nu)(total) congruent-to 4 Jy] is associated with GM 24, while the weaker one [S(nu)(total) congruent-to 0.1 Jy], located approximately 1'5 south of GM 24, is related to an optical nebula in the region. The maximum of radio continuum emission coincides with the source IRAS 17136-3617, which is the core of an infrared star cluster. The spectral line data show two velocity components toward GM 24 separated by approximately 10 km s-1. The velocity of the stronger and more compact component is close to the molecular cloud velocity, while its peak of line intensity coincides with the core of the star cluster. The largest H92alpha line widths (DELTAV congruent-to 46 km s-1) are also observed toward this position. The second velocity component (the weaker and extended one) is redshifted by approximately 10 km s-1 with respect to the velocity of the ambient molecular cloud. We suggest as a possible scenario that this velocity component constitutes emission from the ionized gas which is breaking out of the cloud and expanding away from us. A water maser source, with four velocity compoments, is located approximately 15'' southwest of the peak of the radio continuum emission. C1 CSIC, INST ASTROFIS ANDALUCIA, E-18080 GRANADA, SPAIN. CARNEGIE INST WASHINGTON, LAS CAMPANAS OBSERV, LA SERENA, CHILE. Univ Nacl Autonoma Mexico, INST ASTRON, MEXICO CITY 04510, DF, MEXICO. Univ Nacl Autonoma Mexico, INST ASTRON, ENSENADA 22830, BAJA CALIFORNIA, MEXICO. RP GOMEZ, JF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 NR 18 TC 3 Z9 3 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1993 VL 409 IS 1 BP 269 EP 274 DI 10.1086/172661 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LB038 UT WOS:A1993LB03800025 ER PT J AU BARSONY, M SCOVILLE, NZ CHANDLER, CJ AF BARSONY, M SCOVILLE, NZ CHANDLER, CJ TI DETECTION OF MAGNETOHYDRODYNAMIC SHOCKS IN THE L1551 OUTFLOW SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (L1551); ISM, JETS AND OUTFLOWS; MHD; RADIO LINES, ISM; SHOCK WAVES; TECHNIQUES, INTERFEROMETRIC ID HIGH-RESOLUTION IMAGES; MOLECULAR CLOUDS; BIPOLAR OUTFLOW; C-SHOCKS; WAVES; IRS-5; SHELL; FLOWS AB We report the results Of CO J = 1 --> 0 mapping of portions of the blue outflow lobe of L1551 with approximately 7'' (N-S) x 4'' (E-W) resolution, obtained with the three element OVRO millimeter array. Comparison of our interferometer mosaic with lower resolution single-dish data shows that we resolve the strongest single-dish emission regions into filamentary structures, such as are characteristic of shock fronts mapped via their near-infrared H2 emission in other outflow sources. We detect a continuous velocity gradient across the brightest filamentary structure in our maps. The projected, deconvolved, FWHM of this feature is 1-2 x 10(16) cm, similar to that predicted in theoretical models of C-shocks. Combined with the velocity gradient, this suggests that the emission originates from within a magnetohydrodynamic shock front, possibly resulting from the interaction of a stellar wind with dense, ambient material. In contrast, the discontinuous J-shocks expected in regions with low or no magnetic field should have a thickness less-than-or-equal-to 10(15) cm, which would be unresolved at our spatial resolution. Based on the shock models of Draine and coworkers, the magnetic field strengths required to account for the Structure are in the range 10-30 muG. We suggest future high spatial resolution mapping of this feature in its near-infrared CO and H2 emission, to characterize further the temperature and density structure of the neutral gas within the shock. C1 CALTECH,OWENS VALLEY RADIO OBSERV,PASADENA,CA 91125. RP BARSONY, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS-78,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 30 TC 10 Z9 10 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 1993 VL 409 IS 1 BP 275 EP 281 DI 10.1086/172662 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LB038 UT WOS:A1993LB03800026 ER PT J AU DIETRICH, M KOLLATSCHNY, W PETERSON, BM BECHTOLD, J BERTRAM, R BOCHKAREV, NG BOROSON, TA CARONE, TE ELVIS, M FILIPPENKO, AV GASKELL, CM HUCHRA, JP HUTCHINGS, JB KORATKAR, AP KORISTA, KT LAME, NJ LAOR, A MACALPINE, GM MALKAN, MA DEOLIVEIRA, CM NETZER, H PENFOLD, J PENSTON, MV PEREZ, E POGGE, RW RICHMOND, MW ROSENBLATT, EI SHAPOVALOVA, AI SHIELDS, JC SMITH, HA SMITH, PS SUN, WH THIELE, U VEILLEUX, S WAGNER, RM WILKES, BJ WILLS, BJ WILLS, D AF DIETRICH, M KOLLATSCHNY, W PETERSON, BM BECHTOLD, J BERTRAM, R BOCHKAREV, NG BOROSON, TA CARONE, TE ELVIS, M FILIPPENKO, AV GASKELL, CM HUCHRA, JP HUTCHINGS, JB KORATKAR, AP KORISTA, KT LAME, NJ LAOR, A MACALPINE, GM MALKAN, MA DEOLIVEIRA, CM NETZER, H PENFOLD, J PENSTON, MV PEREZ, E POGGE, RW RICHMOND, MW ROSENBLATT, EI SHAPOVALOVA, AI SHIELDS, JC SMITH, HA SMITH, PS SUN, WH THIELE, U VEILLEUX, S WAGNER, RM WILKES, BJ WILLS, BJ WILLS, D TI STEPS TOWARD DETERMINATION OF THE SIZE AND STRUCTURE OF THE BROAD-LINE REGION IN ACTIVE GALACTIC NUCLEI .4. INTENSITY VARIATIONS OF THE OPTICAL-EMISSION LINES OF NGC-5548 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ACTIVE; GALAXIES, FUNDAMENTAL PARAMETERS; GALAXIES, INDIVIDUAL (NGC-5548); GALAXIES, NUCLEI; GALAXIES, SEYFERT ID SEYFERT-GALAXIES; VARIABILITY; ARAKELIAN-120; ULTRAVIOLET; KINEMATICS; CONTINUUM; NGC-4151; GAS AB We present measurements of optical emission-line flux variations based on spectra of the Seyfert galaxy NGC 5548 obtained between 1988 December and 1989 October during the course of a large-scale international monitoring effort. The data presented here supplement previously published measurements of the UV lines and continuum, optical continuum, and broad Hbeta emission line. All of the measured optical emission lines, Halpha, Hbeta, Hgamma, He I lambda5876, and He II lambda4686, show the same qualitative behavior as the UV and optical continua, but with short time delays, or lags, which are different for the various lines. We apply cross-correlation analysis to measure the lags between the various lines and the continuum. We find similar lags with respect to the UV continuum for Halpha and Hbeta, 17 and 19 days, respectively. The lag for Hgamma is shorter (13 days), only somewhat larger than the lag measured for Lyalpha (about 10 days). The helium lines respond to continuum variations more rapidly than the hydrogen lines, with lags of about 7 days for He II lambda4686 and 11 days for He I lambda5876. C1 OHIO STATE UNIV,DEPT ASTRON,COLUMBUS,OH 43210. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. UNIV MOSCOW,STERNBERG ASTRON INST,MOSCOW V234,RUSSIA. NATL OPT ASTRON OBSERV,KITT PEAK NATL OBSERV,TUCSON,AZ 85726. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. DOMINION ASTROPHYS OBSERV,VICTORIA V8X 4M6,BC,CANADA. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. CARNEGIE INST WASHINGTON,PASADENA,CA 91101. INST ADV STUDY,PRINCETON,NJ 08540. RP DIETRICH, M (reprint author), UNIV GOTTINGEN,GEISMARLANDSTR 11,W-3400 GOTTINGEN,GERMANY. RI Mendes de Oliveira, Claudia/F-2391-2012; OI Mendes de Oliveira, Claudia/0000-0002-7736-4297; SUN, WEI-HSIN/0000-0002-7474-8658; Gaskell, C/0000-0003-4888-2009; Wilkes, Belinda/0000-0003-1809-2364; Perez, Enrique/0000-0001-9737-4559 NR 30 TC 77 Z9 77 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1993 VL 408 IS 2 BP 416 EP 427 DI 10.1086/172599 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LA024 UT WOS:A1993LA02400004 ER PT J AU LADA, CJ YOUNG, ET GREENE, TP AF LADA, CJ YOUNG, ET GREENE, TP TI INFRARED IMAGES OF THE YOUNG CLUSTER NGC-2264 SO ASTROPHYSICAL JOURNAL LA English DT Article DE INFRARED, STARS; OPEN CLUSTERS AND ASSOCIATIONS, INDIVIDUAL (NGC-2264); STARS, FORMATION ID OB1 MOLECULAR CLOUD; T-TAURI STARS; INTRINSIC COLORS; STELLAR OBJECTS; DISKS; PHOTOMETRY; ACCRETION AB We present the initial results of an extensive infrared imaging survey of the young cluster NGC 2264 and a nearby galactic control field. A large portion of the cluster was imaged in each of the three standard near-infrared colors (J, H, and K) with an infrared array camera. Similar observations were obtained of a large nearby region off the cluster and its associated molecular cloud. Comparison of these observations enabled us to estimate the size of the cluster population and investigate the nature of is members. In the region of the cluster surveyed at 2.2 mum (K), we detected more than 1,650 sources. After correcting for background/foreground field stars we find that the cluster contains 360 (+/- 130) members. We find that the slope of the K luminosity function of the cluster is significantly steeper than that expected for a cluster of ZAMS stars and appears to flatten out or turn over at an apparent K magnitude of roughly 13.0-14.0. Both the slope and the turnover in the luminosity function can be modeled with an underlying cluster mass function which is similar to the Miller-Scalo or local field star IMF, provided that a mass-luminosity relation appropriate for premain-sequence stars applies to the cluster population. From analysis of the JHK color-color diagrams of the cluster and control fields we find that approximately 170 sources observed toward the cluster have colors indicative of intrinsic excess infrared emission. Consequently, infrared excess stars appear to account for a relatively large fraction (50% +/- 20%) of the cluster membership. These stars have near-infrared colors similar to those of young emission-line stars such as classical T Tauri stars and Herbig AeBe stars. Circumstellar disk models can account for the colors of most of these sources. That circumstellar disks are inferred for such a large fraction of the cluster membership argues for disk lifetimes which are at least as long as the age of the cluster (i.e., 5 x 10(6) yr). Many of these stars are also characterized by relatively large amounts of extinction and may be partially embedded in the molecular cloud behind the cluster. C1 UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85724 USA. UNIV HAWAII, INST ASTRON, HONOLULU, HI 96822 USA. RP LADA, CJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 51 TC 82 Z9 82 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1993 VL 408 IS 2 BP 471 EP 483 DI 10.1086/172605 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LA024 UT WOS:A1993LA02400010 ER PT J AU HO, PTP PENG, YL TORRELLES, JM GOMEZ, JF RODRIGUEZ, LF CANTO, J AF HO, PTP PENG, YL TORRELLES, JM GOMEZ, JF RODRIGUEZ, LF CANTO, J TI A FLATTENED CLOUD CORE IN NGC-2024 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (NGC-2024); ISM, JETS AND OUTFLOWS; ISM, MOLECULES; RADIO LINES, ISM ID ORION-B NGC-2024; MOLECULAR CLOUD; PROTOSTELLAR CONDENSATIONS; NGC 2024; AMMONIA; THERMOMETER; OUTFLOWS; REGION; LINE AB The (J, K) = (1, 1) and (2, 2) NH, lines were mapped toward a molecular cloud core in NGC 2024 using the VLA in its C/D-configuration. This region is associated with one of the most highly collimated molecular outflows. We find that the molecular condensations associated with the far-infrared sources FIR 5, FIR 6, and FIR 7 have kinetic temperatures T(K) congruent-to 40 K. We also find line broadening toward FIR 6 and FIR 7. This suggests that these condensations may not be protostars heated by gravitational energy released during collapse but that they have an internal heating source. A flattened structure of ammonia emission is found extending parallel to the unipolar CO outflow structure, but displaced systematically to the east. If the NH3 emission traces the denser gas environment, there is no evidence that a dense gas structure is confining the molecular outflow. Instead, the location of the high-velocity outflow along the surface of the NH3 structure suggests that a wind is sweeping material from the surface of this elongated cloud core. C1 CSIC, INST ASTROFIS ANDALUCIA, E-18080 GRANADA, SPAIN. Univ Nacl Autonoma Mexico, INST ASTRON, MEXICO CITY 04510, DF, MEXICO. NANJING UNIV, NANJING, PEOPLES R CHINA. RP HO, PTP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. RI Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 NR 36 TC 16 Z9 16 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1993 VL 408 IS 2 BP 565 EP 572 DI 10.1086/172614 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LA024 UT WOS:A1993LA02400019 ER PT J AU ZUCKER, DB SOKER, N AF ZUCKER, DB SOKER, N TI THE MORPHOLOGY AND INTERACTION WITH THE INTERSTELLAR-MEDIUM OF THE PLANETARY-NEBULA IC-4593 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, STRUCTURE; PLANETARY NEBULAE, INDIVIDUAL (IC-4593) ID CENTRAL STARS; EVOLUTION; SHELLS AB We present a morphological study of the planetary nebula IC 4593, based on our observations in Halpha, [O III], and [S II]. From the Halpha intensity map, we calculate densities and masses for constituent structures and for the nebula as a whole. We argue that the morphology of IC 4593 suggests that it is moving supersonically through the ISM, and that the ISM shock may be thermally unstable, oscillating between adiabatic and radiative (isothermal) shock conditions. Spectroscopic observations are necessary to further explore the nature of the interaction between IC 4593 and the ISM. An improved understanding of such interactions will greatly expand the potential use of planetary nebulae to probe the ISM. C1 ORANIM UNIV,DIV MATH PHYS,IL-36910 TIVON,ISRAEL. RP ZUCKER, DB (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 25 TC 18 Z9 18 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1993 VL 408 IS 2 BP 579 EP 585 DI 10.1086/172616 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LA024 UT WOS:A1993LA02400021 ER PT J AU MCLAUGHLIN, BM BELL, KL AF MCLAUGHLIN, BM BELL, KL TI EFFECTIVE COLLISION STRENGTHS FOR O-II SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC DATA; ULTRAVIOLET, STARS ID OSCILLATOR-STRENGTHS; OPACITY CALCULATIONS; ATOMIC DATA; STATES; OXYGEN AB Accurate electron collisional excitation strengths OMEGA, from 11 state R-matrix calculations performed in LSpi coupling, are convoluted with a Maxwellian velocity distribution to obtain effective collision strengths UPSILON for a range of temperatures 5 x 10(3) K to 10(6) K for electron excitation of singly ionized atomic oxygen. This work considers electron collisional excitation of the O II ion from the 1s(2)2s(2)2p3 (S-4(o)) to the 1s(2)2s(2)2p3 (2D(o), P-2(o)) and to the higher lying 1s(2)2s2p4 (P-4(e)) and 1s(2)2s(2)2p(2)3s (P-4(e)) states. In addition, we consider the 1s(2)2s(2)2p3 (2D(o)) to 1s(2)2s(2)2p3 (P-2(o)) transition. Comparison with existing values in the literature indicates improved results for the effective collision strengths at all temperatures. C1 QUEENS UNIV BELFAST,DEPT APPL MATH & THEORET PHYS,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. RP MCLAUGHLIN, BM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 26 TC 41 Z9 41 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 1993 VL 408 IS 2 BP 753 EP 757 DI 10.1086/172635 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LA024 UT WOS:A1993LA02400040 ER PT J AU JAMES, M PERIVOLAROPOULOS, L VACHASPATI, T AF JAMES, M PERIVOLAROPOULOS, L VACHASPATI, T TI DETAILED STABILITY ANALYSIS OF ELECTROWEAK STRINGS SO NUCLEAR PHYSICS B LA English DT Article AB We give a detailed stability analysis of the Z-string in the standard electroweak model. We identify the mode that determines the stability of the string and numerically map the region of parameter space where the string is stable. For sin2theta(W) = 0.23, we find that the strings are unstable for a Higgs mass larger than 23 GeV. Given the latest constraints on the Higgs mass from LEP, this shows that, if the standard electroweak model is realized in nature, the existing vortex solutions are unstable. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,DIV THEORET ASTROPHYS,CAMBRIDGE,MA 02138. TUFTS UNIV,TUFTS INST COSMOL,DEPT PHYS & ASTRON,MEDFORD,MA 02155. RP JAMES, M (reprint author), UNIV CAMBRIDGE,DAMTP,SILVER ST,CAMBRIDGE CB3 9EW,ENGLAND. NR 15 TC 77 Z9 77 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0550-3213 J9 NUCL PHYS B JI Nucl. Phys. B PD MAY 3 PY 1993 VL 395 IS 3 BP 534 EP 546 DI 10.1016/0550-3213(93)90046-R PG 13 WC Physics, Particles & Fields SC Physics GA LC281 UT WOS:A1993LC28100002 ER PT J AU KRATZ, CA AF KRATZ, CA TI TRANSFORMATIONS OF AFRICAN MARRIAGE - PARKIN,D, NYAMWAYA,D SO AMERICAN ETHNOLOGIST LA English DT Book Review RP KRATZ, CA (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0094-0496 J9 AM ETHNOL JI Am. Ethnol. PD MAY PY 1993 VL 20 IS 2 BP 423 EP 424 DI 10.1525/ae.1993.20.2.02a00440 PG 2 WC Anthropology SC Anthropology GA LJ860 UT WOS:A1993LJ86000046 ER PT J AU CREEL, S WILDT, DE MONFORT, SL AF CREEL, S WILDT, DE MONFORT, SL TI AGGRESSION, REPRODUCTION, AND ANDROGENS IN WILD DWARF MONGOOSES - A TEST OF THE CHALLENGE HYPOTHESIS SO AMERICAN NATURALIST LA English DT Note ID SUPPRESSION; TESTOSTERONE; BEHAVIOR C1 TANZANIA NATL PARKS,SERENGETI WILDLIFE RES CTR,ARUSHA,TANZANIA. SMITHSONIAN INST,CONSERVAT & RES CTR,ENDOCRINE RES LAB,NATL ZOOL PK,FRONT ROYAL,VA 22630. NR 23 TC 52 Z9 53 U1 2 U2 13 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0003-0147 J9 AM NAT JI Am. Nat. PD MAY PY 1993 VL 141 IS 5 BP 816 EP 825 DI 10.1086/285509 PG 10 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA LR254 UT WOS:A1993LR25400011 PM 19426013 ER PT J AU SCHWEDE, G HENDRICHS, H MCSHEA, W AF SCHWEDE, G HENDRICHS, H MCSHEA, W TI SOCIAL AND SPATIAL-ORGANIZATION OF FEMALE WHITE-TAILED DEER, ODOCOILEUS-VIRGINIANUS, DURING THE FAWNING SEASON SO ANIMAL BEHAVIOUR LA English DT Article ID CERVUS-ELAPHUS L; BEHAVIOR; TERRITORIALITY; MOVEMENTS; MORTALITY C1 UNIV BIELEFELD,DEPT ETHOL,W-4800 BIELEFELD,GERMANY. SMITHSONIAN INST,CONSERVAT & RES CTR,NATL ZOOL PK,FRONT ROYAL,VA 22630. RP SCHWEDE, G (reprint author), NATL WILDLIFE RES CTR,POB 1086,TAIF,SAUDI ARABIA. NR 48 TC 41 Z9 42 U1 1 U2 18 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD MAY PY 1993 VL 45 IS 5 BP 1007 EP 1017 DI 10.1006/anbe.1993.1118 PG 11 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA LE946 UT WOS:A1993LE94600014 ER PT J AU HUCHRA, J LATHAM, DW DACOSTA, LN PELLEGRINI, PS WILLMER, CNA AF HUCHRA, J LATHAM, DW DACOSTA, LN PELLEGRINI, PS WILLMER, CNA TI THE MORPHOLOGICAL CATALOG OF GALAXIES EQUATORIAL SURVEY SO ASTRONOMICAL JOURNAL LA English DT Article ID REDSHIFTS AB We present 865 redshifts of galaxies located in the equatorial strip - 17.5-degrees less-than-or-equal-to delta less-than-or-equal-to - 2.5-degrees in the right ascension range 20h less-than-or-equal-to a less-than-or-equal-to 5h. Redshifts have been obtained for the complete sample of all 833 galaxies in the Morphological Catalog of Galaxies with magnitudes brighter than m = 14.5 (corresponding approximately to m(Zwicky) = 15.0). This sample also includes three galaxies from other sources with more reliable magnitudes, satisfying this limit, and 29 fainter galaxies, usually companions of the galaxies in the magnitude limited sample. Our maps of a very large volume of nearby space demonstrate a variety of coherent large scale structures which include large voids, 20-50h-1 Mpc in diameter and large walls at least 70h-1 Mpc across. C1 CNPQ,OBSERV NACL,S CRISTOVAO,RJ,BRAZIL. UNIV CALIF SANTA CRUZ,UCO,LICK OBSERV,SANTA CRUZ,CA 95064. RP HUCHRA, J (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 17 TC 40 Z9 40 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 1993 VL 105 IS 5 BP 1637 EP 1657 DI 10.1086/116543 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KZ644 UT WOS:A1993KZ64400002 ER PT J AU HAMILTON, D STAUFFER, JR AF HAMILTON, D STAUFFER, JR TI OPTICAL SPECTROSCOPY OF VERY LOW-MASS STARS IN THE PLEIADES SO ASTRONOMICAL JOURNAL LA English DT Article ID BROWN DWARFS; SPECTROPHOTOMETRY; LHS-2924; MODELS AB We have obtained optical spectrophotometry for several cool stars recently found by us in a deep multicolor optical survey of the Pleiades. This survey has the distinct advantage of analyzing stars, which if proven to be cluster members, are of a known age and metallicity, which cannot be said of local cool stars. In addition, we have also observed several stars studied by Berriman and Reid in order to place the Pleiades candidates relative to these nearby stars. Based upon analysis of the spectra of the nearby stars, we define several molecular band indices (four TiO and one VO) and one index which measures the slope of the virtual continuum in order to segregate and classify stars in terms of effective temperature. Some of these indices are well correlated, in a linear fashion, with log(T(eff)). Included in the analysis is the poorly understood cool star, LHS 2924, which continues to confuse the trends established with this analysis, by remaining an obvious outlier with one exception. The VO strength, as expected, roughly correlates with log(T(eff)) for the temperature range under consideration and the large scatter is almost certain to be due to metallicity variations. Only in the coolest of the Pleiades stars reported here is the VO index comparable to that of the local cool stars such as VB 10. However, in the remaining cool Pleiades stars the VO index is substantially lower and similar to that of G1 905. The pseudocontinuum index defined in this paper appears to be the most reliable effective temperature estimator for optical spectroscopic data even when the problematic LHS 2924 is included in the analysis. This index appears to be valid at least over the range 2100 K < T(eff) < 3000 K and is defined by flux density points which are not overtly influenced by TiO. With the exception of the strengths of atomic sodium and Halpha, the spectroscopic properties of VB 10 and that of the coolest Pleiades star are very similar. However, the bolometric magnitude of the coolest Pleiades star is 1-1.5 mag brighter. In this Pleiades star, atomic sodium is nearly twice as strong as that of VB 10 but the emission strength of Ha is only half as large. The brighter intrinsic luminosity is consistent with the star still contracting to the main sequence (hence spinning up) as would be expected for a star that is 70 Myr and only 0.1 M.. The other cool Pleiades stars tend to be similar in properties to that of G1 905. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP HAMILTON, D (reprint author), CALTECH,PALOMAR OBSERV,PASADENA,CA 91125, USA. NR 21 TC 10 Z9 10 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 1993 VL 105 IS 5 BP 1855 EP 1859 DI 10.1086/116559 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KZ644 UT WOS:A1993KZ64400018 ER PT J AU GOMEZ, M HARTMANN, L KENYON, SJ HEWETT, R AF GOMEZ, M HARTMANN, L KENYON, SJ HEWETT, R TI ON THE SPATIAL-DISTRIBUTION OF PRE-MAIN-SEQUENCE STARS IN TAURUS SO ASTRONOMICAL JOURNAL LA English DT Article ID MAGNETIC-FIELD STRUCTURE; AURIGA DARK CLOUDS; MOLECULAR CLOUD; DENSE CORES; SOLAR NEIGHBORHOOD; PERSEUS; COMPLEX AB We derive characteristic properties of the nonrandom spatial distribution of pre-main-sequence stars in the Taurus-Auriga molecular cloud by applying several different statistical techniques. We find that a power-law form for the two-point angular correlation function (with index - 1.2) reproduces the overall shape of the actual pre-main-sequence distribution in Taurus at small angular scales (approximately 0.3-degrees). This result is consistent with the existence of real clustering in the T Tauri distribution. With the aid of the nearest-neighbor distribution technique, we determine a median projected separation of approximately 0.3 pc for young stars in this cloud, even after eliminating close pairs with separations less than 20'' (approximately 3000 AU at the distance of Taurus) from our sample. This separation is only slightly larger than the typical size of a dense molecular core (approximately 0.1 pc), which suggests that ''isolated'' star formation does not occur in low-density star-forming regions like Taurus. We find similar properties for the nearest-neighbor distributions in other star-forming regions, such as Lupus, Chamaeleon T1, rho Ophiuchi, Orion, NGC 7000/IC 5070, and NGC 2264. Our analysis suggests that even ultimately single stars typically form with a relatively close companion. Multiple star formation inside elongated molecular cloud cores may provide a natural mechanism for this result. We also identify six statistically significant clumps or groups of stars in Taurus with projected radii of approximately 0.5-1 pc. These small groups appear distributed over the molecular cloud and harbor approximately 15 stellar systems each. The internal velocity dispersions in these groups are approximately 0. 5-1 km s-1 for a mean stellar lifetime of approximately 10(6) yr if they are not gravitationally bound. RP GOMEZ, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 50 TC 205 Z9 205 U1 0 U2 2 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 1993 VL 105 IS 5 BP 1927 EP 1937 DI 10.1086/116567 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KZ644 UT WOS:A1993KZ64400026 ER PT J AU DAVIES, MB RUFFERT, M BENZ, W MULLER, E AF DAVIES, MB RUFFERT, M BENZ, W MULLER, E TI A COMPARISON BETWEEN SPH AND PPM - SIMULATIONS OF STELLAR COLLISIONS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE HYDRODYNAMICS; METHODS, NUMERICAL; STARS, EVOLUTION STARS, KINEMATICS ID 3-DIMENSIONAL HYDRODYNAMICAL SIMULATIONS; SN-1987A; STARS AB A full 3D implementation of the smoothed particle hydrodynamics method (SPH) is compared to the 3D Eulerian piecewise parabolic method (PPM). Both codes were used to simulate a collision between a 0.5M. main-sequence star (modelled as a n = 3/2 polytrope) and a white dwarf star of equal mass (treated as a point mass). The encounter was simulated 6 times with SPH (the number of particles ranging between 2900 and 27 000) and twice with PPM (using 64(3) and 128(3) cartesian zones). A multiple grid implementation of the PPM code was also employed (5 nested grids of 32(3) zones each). Our results show that the key factor determining the overall result of the collision is the form of the potential well of the point mass. Depending on the exact numerical smoothing of the well, different trajectories, amounts of mass accretion and maximum temperatures are obtained. Once both codes are run with the same point mass potential, the global values (e.g. total energy, angular momentum, center of mass trajectory, etc.) are in good agreement. However the results differ in the values of local quantities like density distribution in the immediate vicinity of the point mass, and in the envelope structure. The choice of an impartial test problem is difficult, since advantages and disadvantages of both methods are largely mutually exclusive. For the modeling of stellar collisions, SPH and PPM produce results that compare quite favorably. Hence, given that both schemes are fundamentally different, we assume that common features are physical in nature and not numerical. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. MAX PLANCK INST ASTROPHYS, W-8046 GARCHING, GERMANY. UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85724 USA. NR 22 TC 22 Z9 22 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD MAY PY 1993 VL 272 IS 2 BP 430 EP 441 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LC646 UT WOS:A1993LC64600011 ER PT J AU MAY, J BRONFMAN, L ALVAREZ, H MURPHY, DC THADDEUS, P AF MAY, J BRONFMAN, L ALVAREZ, H MURPHY, DC THADDEUS, P TI A DEEP CO SURVEY OF THE 3RD GALACTIC QUADRANT SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article DE SURVEYS; GALAXY-STRUCTURE; RADIO LINES-MOLECULAR-INTERSTELLAR; INTERSTELLAR MEDIUM-CLOUDS ID SOUTHERN MILKY-WAY; MOLECULAR CLOUDS; SOLAR CIRCLE; IRAS SOURCES; CALIBRATION AB We present a new survey of the third galactic quadrant in the J = 1 - 0 transition line of CO. With an angular resolution of 8.8' and a rms noise temperature of 0.10 K, this survey has allowed the detection of weak emission from distant molecular clouds, 12 - 18 kpc from the galactic center, previously undetected in a low resolution survey of this region done with the same telescope (May et al. 1988). Owing to the warping of the outer Galaxy, the coverage follows a strip inclined to the galactic plane covering at least 3-degrees in latitude between longitudes 210-degrees and 270-degrees, but only 2-degrees between 194-degrees and 210-degrees. The results of the survey are presented in the form of a full set of latitude-velocity and longitude-velocity contour diagrams for each observed longitude and latitude, respectively. Spatial maps, obtained by integrating the CO over the spectral range where emission was detected, -19 to 110 km s-1, summarize the survey for comparison with continuum data (gamma-ray, infrared, and radio). C1 OBSERV CARNEGIE INST WASHINGTON,PASADENA,CA 91101. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MAY, J (reprint author), UNIV CHILE,DEPT ASTRON,CASILLA 36-D,SANTIAGO,CHILE. RI Bronfman, Leonardo/H-9544-2013 OI Bronfman, Leonardo/0000-0002-9574-8454 NR 19 TC 21 Z9 22 U1 0 U2 0 PU EDITIONS PHYSIQUE PI LES ULIS CEDEX PA Z I DE COURTABOEUF AVE 7 AV DU HOGGAR, BP 112, 91944 LES ULIS CEDEX, FRANCE SN 0365-0138 J9 ASTRON ASTROPHYS SUP JI Astron. Astrophys. Suppl. Ser. PD MAY PY 1993 VL 99 IS 1 BP 105 EP 165 PG 61 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LC840 UT WOS:A1993LC84000006 ER PT J AU CORNWELL, TJ NARAYAN, R AF CORNWELL, TJ NARAYAN, R TI IMAGING WITH ULTRA-RESOLUTION IN THE PRESENCE OF STRONG SCATTERING SO ASTROPHYSICAL JOURNAL LA English DT Article DE SCATTERING; TECHNIQUES, INTERFEROMETRIC; TELESCOPES ID BROADENED IMAGE; COHERENCE; SHAPE AB When there is random scattering between a source and an imaging telescope or interferometer, it is known that the angular resolution that can be attained with a long exposure observation is below the ideal limit. Techniques such as speckle and self-calibration permit the use of short exposure data to restore the full resolution of the instrument. We show in this Letter that, under certain circumstances involving very strong scattering, short exposure data can actually be used to enhance the angular resolution to well beyond the ideal limit. Schematic designs for an interferometer to make use of this effect are presented. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP CORNWELL, TJ (reprint author), NATL RADIO ASTRON OBSERV,POB 0,SOCORRO,NM 87801, USA. OI Narayan, Ramesh/0000-0002-1919-2730 NR 14 TC 6 Z9 6 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 1993 VL 408 IS 1 BP L69 EP L72 DI 10.1086/186833 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KY811 UT WOS:A1993KY81100018 ER PT J AU FANNING, TG SEUANEZ, HN FORMAN, L AF FANNING, TG SEUANEZ, HN FORMAN, L TI SATELLITE DNA-SEQUENCES IN THE NEW-WORLD PRIMATE CEBUS-APELLA (PLATYRRHINI, PRIMATES) SO CHROMOSOMA LA English DT Article ID ALPHOID DNA; TANDEM ARRAYS; LONG; CHROMOSOMES; STABILITY; GENOME AB Two satellite DNAs, designated CapA and CapB, were isolated from the neotropical primate, Cebus apella. The satellites exhibit nonoverlapping distributions on C. apella chromosomes. CapA is a major component of interstitial regions of constitutive heterochromatin, a very large block of heterochromatin comprising most of the long arm of chromosome 11, and some telomeres. The CapA monomer has a length of about 1500 bp and appears recently to have undergone an amplification episode in the C. apella genome. CapA-like sequences are probably present in members of the family Cebidae (to which C. apella belongs), but not in members of the family Callitrichidae (marmosets). CapB sequences can be detected at the centromeres of many C. apella chromosomes, and similar sequences are present in all neotropical primates. The 342 bp CapB monomer shares 60%-64% sequence identity with several alpha satellite sequences of human origin. Because of its structure, sequence, and location, it appears that CapB is the New World primate homolog of Old World primate alpha satellite DNA. C1 UNIV FED RIO DE JANEIRO,INST NACL CANC,DEPT GENET,GENET SECT,RIO JANEIRO,BRAZIL. SMITHSONIAN INST,NATL ZOOL PK,DEPT ZOOL RES,WASHINGTON,DC 20008. RP FANNING, TG (reprint author), AFIP,DEPT CELLULAR PATHOL,WASHINGTON,DC 20306, USA. NR 25 TC 19 Z9 19 U1 0 U2 1 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0009-5915 J9 CHROMOSOMA JI Chromosoma PD MAY PY 1993 VL 102 IS 5 BP 306 EP 311 DI 10.1007/BF00661273 PG 6 WC Biochemistry & Molecular Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Genetics & Heredity GA LB423 UT WOS:A1993LB42300002 PM 8325162 ER PT J AU EBERHARD, WG AF EBERHARD, WG TI COPULATORY COURTSHIP AND GENITAL MECHANICS OF 3 SPECIES OF MACRODACTYLUS (COLEOPTERA SCARABAEIDAE MELOLONTHINAE) SO ETHOLOGY ECOLOGY & EVOLUTION LA English DT Article DE COPULATORY COURTSHIP; CRYPTIC FEMALE CHOICE; SEXUAL SELECTION; GENITALIC EVOLUTION; SPECIES-SPECIFIC CHARACTERS AB Female Macrodactylus costulatus, sericinus, and sylphis mated repeatedly while feeding on flowers and fruits as they matured eggs. Courtship in all species occurred both prior to and following intromission, with most courtship being performed after the male had achieved intromission. Females often prevented males from mounting, and often prevented mounted males from achieving intromission. They also probably often prevented male genitalia from penetrating past the vulva, even after they had allowed them into the genital chamber. Males at least sometimes pushed forcefully at structures both on the surface of the female and within her reproductive tract. Copulation probably involved a combination of force and persuasion. It often failed to result in complete transfer of sperm. Males displayed striking virtuosity in both the morphology and behavior of their genitalia, which assumed at least four different morphological configurations. At least five and perhaps up to eight different functions were performed by male genitalia. Small sacs near the tips of the male parameres were probably used by males as ''foot-in-the-door'' devices to gain access to the female's genital chamber, while the spiney collar and tongue may have helped open the vulva to allow deeper penetration. The energetic and persistent courtship which occurred after intromission was achieved may function at least partly to induce the female to allow the male to reach the deeper stage of penetration necessary for spermatophore formation, and perhaps to permit transfer of sperm to her spermathecal duct. Male courtship behavior included movements of his head, vibration and sweeping movements of his middle legs, rubbing with his abdominal bristles against the female's elytra, strong substrate vibrations of unknown origin in the male's body, and tapping and stroking with his genitalia on the external surface of the female's abdomen while he held her with his specialized front legs. Pairings in the field lasted up to several days, but there was no sign of size biases in either paired males or females. Males were more susceptible to predation by a common predator than were females when beetles were paired. RP EBERHARD, WG (reprint author), UNIV COSTA RICA,SMITHSONIAN TROP RES INST,SAN JOSE,COSTA RICA. NR 0 TC 24 Z9 27 U1 0 U2 8 PU UNIV FIRENZE ETHOLOGY ECOLOGY & EVOLUTION PI FLORENCE PA ATTN: PROF. F. DESSI-FULGHERI VIA ROMANA 17, 50125 FLORENCE, ITALY SN 0394-9370 J9 ETHOL ECOL EVOL JI Ethol. Ecol. Evol. PD MAY PY 1993 VL 5 IS 1 BP 19 EP 63 PG 45 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA LL104 UT WOS:A1993LL10400002 ER PT J AU WOOD, JA HASHIMOTO, A AF WOOD, JA HASHIMOTO, A TI MINERAL EQUILIBRIUM IN FRACTIONATED NEBULAR SYSTEMS SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID TEMPERATURE PHASE-EQUILIBRIA; EARLY SOLAR-SYSTEM; THERMODYNAMIC PROPERTIES; ISOTOPIC ANOMALIES; CHONDRITES; ORIGIN; CONDENSATION; CHONDRULES; METEORITES; HYPOTHESIS AB We investigated the equilibrium mineral assemblages in chemically fractionated nebular systems, using a computer routine that finds the set of minerals and gases which minimizes the Gibbs free energy of a system with stipulated elemental abundances. Diagrams are presented showing the equilibrium mineralogy, as a function of temperature (400-2300 K), for unfractionated solar material and five fractionated systems. The fractionated systems were defined by mixing, in various proportions, the following four volatility components that solar material can be divided into: refractory dust, carbonaceous matter, ices, and H-2 gas. Dust enrichment is seen to increase temperatures of condensation/evaporation and the Fe2+ content of mafic minerals and to permit existence of stable melt phases. Enrichment of dust and organic matter produces mineral assemblages that are similar in many ways to those of enstatite chondrites, but with mafic minerals that are far more reduced (Fe2+-poor) than those in primitive enstatite chondrites. Enrichment of dust, organics, and ices leads to highly ferrous mineralogies even at the highest temperatures but does not predict the stability of hydrous phases above approximately 450 K. RP WOOD, JA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 66 TC 130 Z9 130 U1 1 U2 8 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD MAY PY 1993 VL 57 IS 10 BP 2377 EP 2388 DI 10.1016/0016-7037(93)90575-H PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA LE469 UT WOS:A1993LE46900019 ER PT J AU PIPERNO, DR PEARSALL, DM AF PIPERNO, DR PEARSALL, DM TI PHYTOLITHS IN THE REPRODUCTIVE STRUCTURES OF MAIZE AND TEOSINTE - IMPLICATIONS FOR THE STUDY OF MAIZE EVOLUTION SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE PHYTOLITHS; MAIZE EVOLUTION; TEOSINTE EXPLOITATION ID ZEA-DIPLOPERENNIS; INFLORESCENCE; CULTIVATION; WILD; GRAMINEAE; GRASSES; ECUADOR; ORIGIN C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV MISSOURI,DEPT ANTHROPOL AMER ARCHAEOL,COLUMBIA,MO 65211. RP PIPERNO, DR (reprint author), UNIV PENN,UNIV MUSEUM,MASCA,33RD & SPRUCE ST,PHILADELPHIA,PA 19104, USA. NR 35 TC 48 Z9 50 U1 0 U2 5 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD MAY PY 1993 VL 20 IS 3 BP 337 EP 362 DI 10.1006/jasc.1993.1021 PG 26 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA LD979 UT WOS:A1993LD97900005 ER PT J AU SEARS, TJ RADFORD, HE MOORE, MA AF SEARS, TJ RADFORD, HE MOORE, MA TI B-DIPOLE TRANSITIONS IN TRANS-HOCO OBSERVED BY FAR-INFRARED LASER MAGNETIC-RESONANCE SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID OH + CO; GROUND-STATE; SPECTRUM; HO2; HCO AB Far infrared laser magnetic resonance spectroscopy is used to measure components of 12 rotational transitions in the ground state of the HOCO radical. The transitions are all b-dipole in character in contrast to the a-dipole rotational spectrum previously reported [Radford, Wei, and Sears, J. Chem. Phys. 97, 3989 (1992)]. The new data determine the A rotational constant to high precision and allow the determination of several centrifugal distortion constants for the first time. The hyperfine coupling in the radical leads to observable splittings in several of the observed transitions and these are used to estimate two of the four expected nonzero hyperfine parameters in the radical. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP SEARS, TJ (reprint author), BROOKHAVEN NATL LAB, DEPT CHEM, UPTON, NY 11973 USA. RI Sears, Trevor/B-5990-2013 OI Sears, Trevor/0000-0002-5559-0154 NR 24 TC 43 Z9 43 U1 1 U2 4 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD MAY 1 PY 1993 VL 98 IS 9 BP 6624 EP 6631 DI 10.1063/1.465098 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA LA763 UT WOS:A1993LA76300004 ER PT J AU WILCZYNSKI, W MCCLELLAND, BE RAND, AS AF WILCZYNSKI, W MCCLELLAND, BE RAND, AS TI ACOUSTIC, AUDITORY, AND MORPHOLOGICAL DIVERGENCE IN 3 SPECIES OF NEOTROPICAL FROG SO JOURNAL OF COMPARATIVE PHYSIOLOGY A-SENSORY NEURAL AND BEHAVIORAL PHYSIOLOGY LA English DT Article DE AMPHIBIAN; ACOUSTIC COMMUNICATION; LARYNX; EAR; BASILAR PAPILLA; ADVERTISEMENT CALL ID HYLA-MICROCEPHALA; VOCAL BEHAVIOR; LEOPARD FROG; TREEFROG; CALL; COMMUNICATION; RECOGNITION; EBRACCATA; MIDBRAIN AB Advertisement calls, auditory tuning, and larynx and ear morphology were examined in 3 neotropical frogs, Hyla microcephala, H. phlebodes and H. ebraccata, H. microcephala has the highest call dominant frequency (6.068 kHz) and basilar papilla tuning (5.36 kHz). H. phlebodes and H. ebraccata calls have lower dominant frequencies (3.832 and 3.197 kHz respectively) and basilar papilla tuning (2.79 and 2.56 kHz). The primary call notes of H. ebraccata are longer (181.6 ms) than those of H. microcephala (95.5 ms) or H. phlebodes (87.3 ms). Morphometric analysis suggests that temporal call features differ as laryngeal musculature changes, in the process changing the overall size of the larynx. The spectral aspects of the call differ as head size, and hence the size of its resonating and radiating structures, changes, modifying the dominant frequency of calls by accentuating their higher harmonics when head size decreases. Decreasing head size decreases the size of the middle and inner ear chambers, changing the mechanical tuning of the ear in the same direction as the change in dominant frequency. These changes result in divergent spectral-temporal characteristics of both the sending and receiving portions of the acoustic communication system underlying social behavior in these frogs. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP WILCZYNSKI, W (reprint author), UNIV TEXAS,DEPT PSYCHOL,AUSTIN,TX 78712, USA. FU NIMH NIH HHS [R01 MH45350] NR 56 TC 34 Z9 35 U1 0 U2 8 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0340-7594 J9 J COMP PHYSIOL A JI J. Comp. Physiol. A-Sens. Neural Behav. Physiol. PD MAY PY 1993 VL 172 IS 4 BP 425 EP 438 DI 10.1007/BF00213524 PG 14 WC Behavioral Sciences; Neurosciences; Physiology; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Physiology; Zoology GA LB024 UT WOS:A1993LB02400004 PM 8315606 ER PT J AU ALPERT, Y LANZEROTTI, LJ THOMSON, DJ MACLENNAN, CG WOLFE, A ERLANDSON, RE AF ALPERT, Y LANZEROTTI, LJ THOMSON, DJ MACLENNAN, CG WOLFE, A ERLANDSON, RE TI HYDROMAGNETIC BACKGROUND OF THE MAGNETOSPHERE AND GYRORESONANCE SWINGING OF A GIANT PC-2 WAVE EVENT SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ION BOUNCE WAVE; GENERATION; PULSATIONS; SPECTRA; PLASMA; PC1 AB The spectral and temporal characteristics of a ''giant'' Pc 2 (tau approximately 7 s) hydromagnetic wave event of duration approximately 110 s have been reanalyzed, as have the electromagnetic oscillations generated in the magnetosphere in an interval of about 45 min preceding and following the event. The event, which was recorded near local midnight at two mid-latitude locations, is, to the best of our knowledge, the largest such wave event reported to date. Previous analyses and interpretation of the event have centered on the bounce resonance generation of this packet of oscillations (Lanzerotti et al., 1986). The reexamination of the event, as well as other oscillations of the magnetoplasma, has caused us to identify six distinguishable spectral frequency bands which appear to encompass die Pc 2 wave packet and its evolution in time as well as to look at the development of the process as a whole. We present the details of these temporal and spectral studies and provide evidence that the Pc 2 event is probably produced by the gyroresonance swinging: amplification of the oscillatory magnetoplasma background in the frequency band approximately 0.1-0.2 Hz. The analysis suggests that the oscillatory background could be produced by impulse-like disturbances. The possible source(s) of such disturbances and their nature require further study. C1 JOHNS HOPKINS UNIV,APPL PHYS LAB,LAUREL,MD 20723. CUNY NEW YORK CITY TECH COLL,BROOKLYN,NY 11201. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP ALPERT, Y (reprint author), AT&T BELL LABS,600 MT AVE,POB 636,MURRAY HILL,NJ 07974, USA. NR 20 TC 2 Z9 2 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES JI J. Geophys. Res-Space Phys. PD MAY 1 PY 1993 VL 98 IS A5 BP 7571 EP 7584 DI 10.1029/92JA00985 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LB643 UT WOS:A1993LB64300006 ER PT J AU EBERHARD, WG AF EBERHARD, WG TI COPULATORY COURTSHIP AND MORPHOLOGY OF GENITALIC COUPLING IN 7 PHYLLOPHAGA SPECIES (COLEOPTERA, MELOLONTHIDAE) SO JOURNAL OF NATURAL HISTORY LA English DT Article DE COPULATION; BEETLES; COPULATORY COURTSHIP; GENITALIC EVOLUTION; PHYLLOPHAGA ID FEMALE CHOICE; BIOLOGY AB Males in six of seven species of phyllophaga perform apparent courtship behaviour during copulation. As predicted by the hypothesis that such copulatory courtship is under sexual selection by female choice, behavioural details differ between species. The modified male abdominal sternites, which rub against the female's pygidium during copulation and whose morphology also differs between species, and the flattened, setose tarsi of males of one species probably function as contact courtship devices during copulatory courtship. Observations of events inside copulating beetles were made through the semi-transparent abdominal sternites of females and male genitalia in three species. They revealed cryptic genitalic thrusting behaviour of male genitalia within the female which occurred even when there was little or no external movement of the male genitalia. Dissections of pairs frozen in copula demonstrated that males transfer large quantities of material to females during copulation that is not physically related to sperm transfer. The type of material varied between species. In at least two species most of the transfer apparently occurred after sperm transfer. The possibility that some male genitalic structures function as holdfasts and/or stimulatory devices was suggested by their positions relative to female structures, and/or their movements within the female. Portions of male genitalia with strong bristles tended to lie against setose or more heavily sclerotized portions of the female reproductive duct. Some portions of female genitalia which vary between species seem ill-designed to exclude the genitalia of cross-specific males. The female reproductive tract is partially everted during copulation in one species. C1 UNIV COSTA RICA,ESCUELA BIOL,CIUDAD UNIV,COSTA RICA. RP EBERHARD, WG (reprint author), UNIV COSTA RICA,SMITHSONIAN TROP RES INST,CIUDAD UNIV,COSTA RICA. NR 13 TC 31 Z9 33 U1 0 U2 10 PU TAYLOR & FRANCIS LTD PI LONDON PA ONE GUNDPOWDER SQUARE, LONDON, ENGLAND EC4A 3DE SN 0022-2933 J9 J NAT HIST JI J. Nat. Hist. PD MAY-JUN PY 1993 VL 27 IS 3 BP 683 EP 717 DI 10.1080/00222939300770401 PG 35 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA LL803 UT WOS:A1993LL80300014 ER PT J AU DONOGHUE, AM JOHNSTON, LA GOODROWE, KL OBRIEN, SJ WILDT, DE AF DONOGHUE, AM JOHNSTON, LA GOODROWE, KL OBRIEN, SJ WILDT, DE TI INFLUENCE OF DAY OF ESTRUS ON EGG VIABILITY AND COMPARATIVE EFFICIENCY OF INVITRO FERTILIZATION IN DOMESTIC CATS IN NATURAL OR GONADOTROPIN-INDUCED ESTRUS SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article ID CIRCULATING HORMONES; FOLLICULAR OOCYTES; EMBRYO DEVELOPMENT; OVARIAN ACTIVITY; SEXUAL-BEHAVIOR; SHEEP OOCYTES; SUPEROVULATION; ABNORMALITIES AB Thirty-six domestic cats received 100 iu hCG (i.m.) on day 1, 2 or 3 of a natural, behavioural oestrus. Twenty-two anoestrous cats were injected with 150 iu pregnant mares' serum gonadotrophin (PMSG; i.m.) followed 84 h later by 100 iu hCG. Twenty-four to 26 h after hCG, all cats were examined laparoscopically to determine the number of ovarian follicles and to recover follicular eggs. Mature eggs were cultured with conspecific spermatozoa and examined 30 h later for cleavage. Within the natural oestrus group, cats on day 1 produced fewer (P < 0.0.5) follicles and total eggs than females on day 2 or 3, and 88.9% of the day 1 eggs were degenerate or immature and unsuitable for in vitro fertilization (IVF). Although only 54.5% of the cats in the PMSG/hCG group exhibited overt oestrus, mean (+/-SEM) numbers of follicles (9.7 +/- 0.8) and oocytes recovered (8.7 +/- 0.8) were at least twofold greater (P < 0.001) than those measured in the natural oestrus group (3.7 +/- 0.6; 3.4 +/- 0.6, respectively) or subgroups on day 2 (3.7 +/- 0.4; 3.3 +/- 0.4) and day 3 (5.7 +/- 0.8; 5.3 +/- 0.8). Overall, the proportion of eggs cleaving in vitro was similar (P > 0.05) between the natural oestrus group (48.3%) and the PMSG/hCG group (50.9%), but the latter group produced more than twice the number of embryos per donor. Embryo quality was unaffected (P > 0.05) by day of hormone treatment, and more than 80% of all two-cell embryos were rated good-to-excellent quality. In summary, there is a temporal relationship between day of sexual receptivity and follicular egg viability in the domestic cat: eggs on the first day of oestrus are not optimally responsive to an LH-like stimulus. There is also no evidence that PMSG/hCG treatment compromises egg quality or subsequent fertilizability in vitro. On the contrary, use of these gonadotrophins markedly improves overall IVF efficiency by increasing the total number of high quality embryos produced. C1 SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008. NCI,FREDERICK CANC RES & DEV CTR,VIRAL CARCINOGENESIS LAB,FREDERICK,MD 21702. FU NICHD NIH HHS [HD 23583] NR 34 TC 17 Z9 19 U1 0 U2 3 PU J REPROD FERTIL INC PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE, ENGLAND CB5 8DT SN 0022-4251 J9 J REPROD FERTIL JI J. Reprod. Fertil. PD MAY PY 1993 VL 98 IS 1 BP 85 EP 90 PG 6 WC Reproductive Biology SC Reproductive Biology GA LH234 UT WOS:A1993LH23400011 PM 8345483 ER PT J AU CREW, SR AF CREW, SR TI THE GREAT MIGRATION IN HISTORICAL-PERSPECTIVE - NEW DIMENSIONS OF RACE, CLASS, AND GENDER - TROTTER,JW SO JOURNAL OF SOUTHERN HISTORY LA English DT Book Review RP CREW, SR (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU SOUTHERN HISTORICAL ASSN PI ATHENS PA UNIV GEORGIA HISTORY DEPT, ATHENS, GA 30602 SN 0022-4642 J9 J SOUTHERN HIST JI J. South. Hist. PD MAY PY 1993 VL 59 IS 2 BP 409 EP 410 DI 10.2307/2209852 PG 2 WC History SC History GA LB631 UT WOS:A1993LB63100078 ER PT J AU SCHOBER, UM CHRISTY, JH AF SCHOBER, UM CHRISTY, JH TI SAND DISPOSAL OF THE PAINTED GHOST CRAB OCYPODE-GAUDICHAUDII (DECAPODA, OCYPODIDAE) - A POSSIBLE ROLE IN COURTSHIP SO MARINE BIOLOGY LA English DT Article ID BRACHYURA; UCA AB In 1991/1992, we studied the sand disposal behavior of the painted ghost crabs Ocypode gaudichaudii on the Pacific coast of Panama. O. gaudichaudii either kick, dump or tamp sand they excavate from their burrows. Here we relate these three kinds of sand disposal to burrow structure and distribution, as well as to crab size and sex. Our objective was to determine whether tamping may be a male courtship signal. Burrows whose owners tamped sand were on average longer, deeper, and higher on the beach than were burrows whose owners kicked or dumped sand. Five burrow shapes were distinguished, with half-spiral and spiral shapes being most common among tamped burrows. All crabs excavated from tamped burrows were males. Tamped burrows peaked in abundance around full and new moons. These observations, together with what is known about mating and breeding behavior of other ghost crabs, suggest that tamping may be involved in O. gaudichaudii courtship. RP SCHOBER, UM (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 33 TC 12 Z9 14 U1 0 U2 7 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD MAY PY 1993 VL 116 IS 1 BP 53 EP 60 DI 10.1007/BF00350731 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA LG628 UT WOS:A1993LG62800007 ER PT J AU GUZMAN, HM HOLST, I AF GUZMAN, HM HOLST, I TI EFFECTS OF CHRONIC OIL-SEDIMENT POLLUTION ON THE REPRODUCTION OF THE CARIBBEAN REEF CORAL SIDERASTREA-SIDEREA SO MARINE POLLUTION BULLETIN LA English DT Article ID RED-SEA CORALS; SEXUAL REPRODUCTION; BUILDING CORALS; SPILL; GAMETOGENESIS; CONSEQUENCES; POPULATIONS; COMMUNITIES; RECRUITMENT; PATTERNS AB In 1986 a major oil spill in Panama polluted and killed extensive areas of coral reefs. Five years afterwards, reef areas are chronically threatened by oil and large amounts of sediments containing toxic hydrocarbons trapped in mangroves. Sublethal effects of oil on coral reproduction were evaluated 39 months after the spill using healthy and injured colonies of the reef-building coral Siderastrea siderea at heavily oiled and unoiled reefs. Number of reproductive colonies and number of gonads per polyp were not sensitive to level of oiling, but gonads were significantly larger at unoiled than oiled reefs during spawning periods. Colonies with recent injuries demonstrated a consistent decrease in fecundity relative to uninjured parts of the same colonies. Years after the spill, the increased number of injuries and associated reduction in colony size, and decreased size of gonads (eggs) on oiled reefs can reduce the number of reproductively viable colonies and gametes in coral populations, and ultimately reduce population survival. RP SMITHSONIAN TROP RES INST, POB 2072, BALBOA, PANAMA. NR 46 TC 56 Z9 60 U1 2 U2 50 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD MAY PY 1993 VL 26 IS 5 BP 276 EP 282 DI 10.1016/0025-326X(93)90068-U PG 7 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA LF396 UT WOS:A1993LF39600011 ER PT J AU FORGET, PM AF FORGET, PM TI POSTDISPERSAL PREDATION AND SCATTERHOARDING OF DIPTERYX-PANAMENSIS (PAPILIONACEAE) SEEDS BY RODENTS IN PANAMA SO OECOLOGIA LA English DT Article DE DIPTERYX-PANAMENSIS; DASYPROCTA-PUNCTATA; SCIURUS-GRANATENSIS; POSTDISPERSAL SEED PREDATION; SCATTERHOARDING ID SCHEELEA PALM SEEDS; POSTDISPERSAL PREDATION; NEOTROPICAL TREE; PARENT PALM; FOREST; SURVIVAL; MAMMALS; RECRUITMENT; DYNAMICS; DISTANCE AB In tropical rain forests of Central America, the canopy tree Dipteryx panamensis (Papilionaceae) fruits when overall fruit biomass is low for mammals. Flying and arboreal consumers feed on D. panamensis and drop seeds under the parent or disperse them farther away. Seeds on the ground attract many vertebrate seed-eaters, some of them potential secondary seed dispersers. The fate of seeds artificially distributed to simulate bat dispersal was studied in relation to fruitfall periodicity and the visiting frequency of diurnal rodents at Barro Colorado Island (BCI), Panama. The frequency of visits by agoutis is very high at the beginning of fruitfall, but in the area close (< 50 m) to fruiting trees (Dipteryx-rich area) it declines throughout fruiting, whereas it remains unchanged farther (> 50 m) away (Dipteryx-poor and Gustavia-rich area). Squirrels were usually observed in the Dipteryx-rich area. Along with intense post-dispersal seed predation by rodents in the Dipteryx-rich area, a significant proportion of seeds were cached by rodents in the Dipteryx-poor area. Post-dispersal seed predation rate was inversely related to hoarding rate. A significantly greater proportion of seeds was cached in March, especially more than 100 m from the nearest fruiting tree. This correlates with the mid-fruiting period, i.e. during the height of D. panamensis fruiting, when rodents seem to be temporarily satiated with the food supply at parent trees. Hoarding remained high toward April, i.e. late in the fruiting season of D. panamensis. Low survival of scatterhoarded seeds suggests that the alternative food supply over the animal's home-ranges in May June 1990 was too low to promote survival of cached seeds. Seedlings are assumed to establish in the less-used area of the rodents' home-range when overall food supply is sufficient to satiate post-dispersal predators. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RI Forget, Pierre-Michel/B-4355-2009 OI Forget, Pierre-Michel/0000-0002-9252-974X NR 57 TC 92 Z9 105 U1 1 U2 23 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD MAY PY 1993 VL 94 IS 2 BP 255 EP 261 DI 10.1007/BF00341325 PG 7 WC Ecology SC Environmental Sciences & Ecology GA LE061 UT WOS:A1993LE06100015 PM 28314040 ER PT J AU POST, RC AF POST, RC TI HUNTINGTON,HENRY,E. AND THE CREATION OF SOUTHERN CALIFORNIA - FRIEDRICKS,WB SO PACIFIC HISTORICAL REVIEW LA English DT Book Review RP POST, RC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0030-8684 J9 PAC HIST REV JI Pac. Hist. Rev. PD MAY PY 1993 VL 62 IS 2 BP 253 EP 255 PG 3 WC History SC History GA LL349 UT WOS:A1993LL34900021 ER PT J AU PENG, JS LI, GX AF PENG, JS LI, GX TI EFFECTS OF THE DIPOLE-DIPOLE INTERACTION ON DYNAMIC PROPERTIES AND ATOMIC COHERENT TRAPPING OF A 2-ATOM SYSTEM SO PHYSICAL REVIEW A LA English DT Article ID JAYNES-CUMMINGS MODEL; SIMPLE QUANTUM MODEL; 2 2-LEVEL ATOMS; REVIVAL PHENOMENON; COLLAPSE; CAVITY; FIELD; JUMPS AB We investigate the effect of the dipole-dipole interaction on the dynamic properties and the atomic coherent trapping of a two-identical-atom system in the presence of a laser field by means of quantum-electrodynamics theory. The influence of the dipole-dipole interaction on the collapses and revivals of the atomic population is revealed. The conditions of the atomic coherent trapping are given. A way to measure optically the coupling strength between the atoms is pointed out. We also show that the effect of the dipole-dipole interaction may be screened due to the coherent field in certain atomic superposition states. C1 HUAZHONG NORMAL UNIV,DEPT PHYS,WUHAN 430070,PEOPLES R CHINA. RP PENG, JS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138, USA. NR 31 TC 17 Z9 23 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAY PY 1993 VL 47 IS 5 BP 4212 EP 4218 DI 10.1103/PhysRevA.47.4212 PN B PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LB807 UT WOS:A1993LB80700022 ER PT J AU KOLBE, E LANGANKE, K KREWALD, S THIELEMANN, FK AF KOLBE, E LANGANKE, K KREWALD, S THIELEMANN, FK TI INELASTIC NEUTRINO SCATTERING ON NUCLEI AND NEUTRINO-NUCLEOSYNTHESIS SO PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS LA English DT Review ID II SUPERNOVAE; EMISSION; DECAY; MODEL AB Within the Continuum Random Phase Approximation we have calculated neutral current cross sections for various neutrino-induced particle reactions on selected nuclei. These cross sections are important for the neutrino-nucleosynthesis in explosive supernova burning. As a byproduct we find that neutrinos and antineutrinos excite parts of the giant dipole resonance differently, with scattering on O-16 showing the most noticeable deviations. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. FORSCHUNGSZENTRUM JULICH, FORSCHUNGSZENTRUM JULICH, INST KERNPHYS, W-5170 JULICH 1, GERMANY. RP CALTECH, WK KELLOGG RADIAT LAB, PASADENA, CA 91125 USA. OI Krewald, Siegfried/0000-0002-8596-8429 NR 27 TC 9 Z9 9 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-1573 EI 1873-6270 J9 PHYS REP JI Phys. Rep.-Rev. Sec. Phys. Lett. PD MAY PY 1993 VL 227 IS 1-5 BP 37 EP 46 DI 10.1016/0370-1573(93)90055-I PG 10 WC Physics, Multidisciplinary SC Physics GA LH206 UT WOS:A1993LH20600005 ER PT J AU THIELEMANN, FK BITOUZET, JP KRATZ, KL MOLLER, P COWAN, JJ TRURAN, JW AF THIELEMANN, FK BITOUZET, JP KRATZ, KL MOLLER, P COWAN, JJ TRURAN, JW TI OPERATION OF THE R-PROCESS AND COSMOCHRONOLOGY SO PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS LA English DT Review ID NEUTRON-RICH NUCLEI; DECAY HALF-LIVES; PROCESS NUCLEOSYNTHESIS; CHEMICAL EVOLUTION; GALAXY; ELEMENTS; SOLAR; MODEL; AGE; FORMULA AB The rapid neutron capture process produced about half of the heavy elements in nature beyond the Fe-peak. In the past quite a number of astrophysical sites have been suggested, but none of them has yet been uniquely identified. Without assuming a particular site or model, we deduce the conditions responsible for the production of r-process nuclei by making use of the following information: (1) the solar r-process abundances and (2) nuclear masses and beta decay half lives for nuclei far from stability - in particular experimental information near magic neutron numbers, which determines the shape of the r-process peaks. In addition, we review briefly galactic age determinations based on the long-lived r-process chronometer nuclei Th-232, U-235 and U-238. C1 ECOLE POLYTECH, F-91128 PALAISEAU, FRANCE. UNIV MAINZ, INST KERNCHEM, W-6500 MAINZ, GERMANY. UNIV OKLAHOMA, DEPT PHYS & ASTRON, NORMAN, OK 73019 USA. COLUMBIA UNIV, DEPT ASTRON, NEW YORK, NY 10027 USA. UNIV CHICAGO, DEPT ASTRON & ASTROPHYS, CHICAGO, IL 60637 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. NR 64 TC 19 Z9 19 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-1573 EI 1873-6270 J9 PHYS REP JI Phys. Rep.-Rev. Sec. Phys. Lett. PD MAY PY 1993 VL 227 IS 1-5 BP 269 EP 281 DI 10.1016/0370-1573(93)90072-L PG 13 WC Physics, Multidisciplinary SC Physics GA LH206 UT WOS:A1993LH20600022 ER PT J AU CAMERON, AGW THIELEMANN, FK COWAN, JJ AF CAMERON, AGW THIELEMANN, FK COWAN, JJ TI S-PROCESS AND R-PROCESS CONTRIBUTIONS TO EXTINCT RADIOACTIVITIES SO PHYSICS REPORTS-REVIEW SECTION OF PHYSICS LETTERS LA English DT Review ID PROCESS NUCLEOSYNTHESIS AB There is now evidence, ranging in quality from very strong to marginal, for the existence in early solar system material of ten radionuclides with mean lives long enough for them to be incorporated live in our planetary system but not long enough to be live at the present time. Of these ten, one (Pu-244) is unquestionably an r-process product, and four (Cs-135, Pd-107, I-129, and Hf-182) might in principle have been made by either the r-process or the s-process. One of us has constructed a model for the history of the local part of the galaxy into which the abundances of the ten extinct nuclides can be fitted. The purpose of the present paper is to explain in greater detail the reasoning that has led to the assignment of I-129 to the r-process and the assignment of the others to the s-process. These latter assignments do not correspond to the traditional assignments of these nuclides as primarily r-process products. It is shown that most of the so-called r-process isobars in the solar system abundance table can have s-process contributions in lower mass AGB stars where peak neutron number densities of 3 x 10(9) to 3 x 10(10) cm-3 are expected during helium shell flashes. C1 COLUMBIA UNIV,DEPT ASTRON,NEW YORK,NY 10027. UNIV OKLAHOMA,DEPT PHYS & ASTRON,NORMAN,OK 73019. RP CAMERON, AGW (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 20 TC 18 Z9 18 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-1573 J9 PHYS REP JI Phys. Rep.-Rev. Sec. Phys. Lett. PD MAY PY 1993 VL 227 IS 1-5 BP 283 EP 291 DI 10.1016/0370-1573(93)90073-M PG 9 WC Physics, Multidisciplinary SC Physics GA LH206 UT WOS:A1993LH20600023 ER PT J AU OFTEDAL, OT BOWEN, WD BONESS, DJ AF OFTEDAL, OT BOWEN, WD BONESS, DJ TI ENERGY-TRANSFER BY LACTATING HOODED SEALS AND NUTRIENT DEPOSITION IN THEIR PUPS DURING THE 4 DAYS FROM BIRTH TO WEANING SO PHYSIOLOGICAL ZOOLOGY LA English DT Article ID TOTAL-BODY WATER; CYSTOPHORA-CRISTATA; ISOTOPE-DILUTION; ELEPHANT SEAL; GROWTH; MILK; ENERGETICS; HYDROGEN; ANIMALS; FLUX AB Hooded seals (Cystophora cristata) have a lactation period of 4 d. The rate of milk energy transfer must be very high to ensure that pups are weaned with sufficient energy reserves to withstand the lengthy postweaning fast. Milk energy transfer was measured by isotope dilution (n = 6), and energy deposition was assayed by chemical analysis of pups at birth (n = 4) and weaning (n = 5). Estimates of body water content obtained by isotope dilution and direct analysis were not significantly different. Water constituted only 71.7% +/- 0.50% (SE) of lean body mass at birth, indicating developmental maturity. Newborn pups were also high in fat (14.0% +/- 0.78%) and energy (10.1 +/- 0.25 MJ/kg). Pups consumed 7.52 +/- 0.469 kg/d milk containing 187 +/- 11.6 MJ/d. Total milk and energy yields were estimated as 30.1 kg and 746 MJ. Pups deposited 88% of ingested fat, 41% of protein, and 84% of energy. Of the weight gain, 82% was fat. The energy content of pups increased nearly fourfold from birth to weaning, but protein content increased by only 11%. At weaning, the energy content of the pup was similar, relative to maternal metabolic size (17.7 MJ/kg0.75), to that in other species with longer lactation periods. We conclude that extreme abbreviation of lactation is feasible as a reproductive strategy in the hooded seal because (1) most of the growth of the lean body and 27% of the energy deposition in pups occur in utero, (2) females produce large amounts of high-fat milk, and (3) the pups are very efficient at converting milk fat to stored lipids. C1 BEDFORD INST OCEANOG, DIV MARINE FISH, DARTMOUTH B24 4A2, NS, CANADA. RP SMITHSONIAN INST, DEPT ZOOL RES, NATL ZOOL PK, WASHINGTON, DC 20008 USA. RI Bowen, William/D-2758-2012 NR 64 TC 68 Z9 68 U1 0 U2 8 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0031-935X J9 PHYSIOL ZOOL JI Physiol. Zool. PD MAY-JUN PY 1993 VL 66 IS 3 BP 412 EP 436 PG 25 WC Physiology; Zoology SC Physiology; Zoology GA LJ923 UT WOS:A1993LJ92300008 ER PT J AU SANDNESS, KL GREEN, JR AF SANDNESS, KL GREEN, JR TI LINES OF ARRESTED GROWTH IN LONG BONES OF PREHISTORIC AND HISTORIC NEBRASKA NATIVE-AMERICANS SO PLAINS ANTHROPOLOGIST LA English DT Note DE PALEOPATHOLOGY; HARRIS LINES; DIET; DISEASE; OMAHA ID AGE AB Radiographs of long bones from prehistoric (AD 1000-1400) and historic (AD 1780-1840) north-eastern Nebraska Native American skeletal series were examined for radiopaque lines (harris lines, growth arrest lines) transversing the distal or proximal ends of individual tibiae and femora. Of the four sites represented, samples from the Woodland site 25DX4 (ca. AD 1000) exhibit the highest frequency of lines. Samples from the St. Helena phase site 25DK13 (AD 1200-1400) show the next highest frequency and those from historic sites 25DK2 and 25DK10 (AD 1780-1840) have the lowest occurrence of lines. There are statistically significant differences between the Woodland samples and those from the later prehistoric and historic contexts. No significant difference could be determined between the 25DK13 samples and those from historic contexts, although a trend toward decreasing number of growth arrest lines is noted. Changing levels of stress related to shifts in subsistence strategies and the onset of epidemic disease are suggested as factors in the decreasing occurrence of lines in the later skeletal series. Lead poisoning is also discussed as a possible contributor to line formation in historic individuals. C1 UNIV NEBRASKA,DEPT ANTHROPOL,LINCOLN,NE 68588. RP SANDNESS, KL (reprint author), SMITHSONIAN INST,DEPT ANTHROPOL,WASHINGTON,DC 20560, USA. NR 28 TC 3 Z9 3 U1 1 U2 2 PU PLAINS ANTHROPOLOGICAL SOC PI LINCOLN PA 410 WEDGEWOOD DRIVE, LINCOLN, NE 68510 SN 0032-0447 J9 PLAINS ANTHROPOL JI Plains Anthropol. PD MAY PY 1993 VL 38 IS 143 BP 211 EP 216 PG 6 WC Anthropology SC Anthropology GA LF524 UT WOS:A1993LF52400009 ER PT J AU JACOB, J DRAKE, BG AF JACOB, J DRAKE, BG TI LONG-TERM CO2 ENRICHMENT EFFECTS ON THE RUBISCO CONTENT AND ACTIVITY IN 2 FIELD-GROWN C3 PLANTS SO PLANT PHYSIOLOGY LA English DT Meeting Abstract C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER SOC PLANT PHYSIOLOGISTS PI ROCKVILLE PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 SN 0032-0889 J9 PLANT PHYSIOL JI Plant Physiol. PD MAY PY 1993 VL 102 IS 1 SU S BP 46 EP 46 PG 1 WC Plant Sciences SC Plant Sciences GA LD890 UT WOS:A1993LD89000236 ER PT J AU LOZHKIN, AV ANDERSON, PM EISNER, WR RAVAKO, LG HOPKINS, DM BRUBAKER, LB COLINVAUX, PA MILLER, MC AF LOZHKIN, AV ANDERSON, PM EISNER, WR RAVAKO, LG HOPKINS, DM BRUBAKER, LB COLINVAUX, PA MILLER, MC TI LATE QUATERNARY LACUSTRINE POLLEN RECORDS FROM SOUTHWESTERN BERINGIA SO QUATERNARY RESEARCH LA English DT Article ID ALASKA C1 UNIV WASHINGTON,QUARTERNARY RES CTR,AK-60,SEATTLE,WA 98195. OHIO STATE UNIV,BYRD POLAR RES CTR,COLUMBUS,OH 43210. UNIV ALASKA,ALASKA QUARTERNARY CTR,FAIRBANKS,AK 99775. UNIV WASHINGTON,COLL FOREST RESOURCES,AR-10,SEATTLE,WA 98195. SMITHSONIAN TROP RES INST,APO,MIAMI,FL 34002. UNIV CINCINNATI,DEPT BIOL SCI,CINCINNATI,OH 45221. RP LOZHKIN, AV (reprint author), RUSSIAN ACAD SCI,NE INTERDISCIPLINARY RES INST,16 PORTOVAYA ST,MAGADAN 685000,RUSSIA. NR 46 TC 79 Z9 83 U1 0 U2 4 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0033-5894 J9 QUATERNARY RES JI Quat. Res. PD MAY PY 1993 VL 39 IS 3 BP 314 EP 324 DI 10.1006/qres.1993.1038 PG 11 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA LA952 UT WOS:A1993LA95200006 ER PT J AU ADAMS, RM AF ADAMS, RM TI SMITHSONIAN HORIZONS SO SMITHSONIAN LA English DT Editorial Material RP ADAMS, RM (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOCIATES PI WASHINGTON PA 900 JEFFERSON DRIVE, WASHINGTON, DC 20560 SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAY PY 1993 VL 24 IS 2 BP 12 EP 12 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA LA656 UT WOS:A1993LA65600001 ER PT J AU CANTINO, PD ABUASAB, MS AF CANTINO, PD ABUASAB, MS TI A NEW LOOK AT THE ENIGMATIC GENUS WENCHENGIA (LABIATAE) SO TAXON LA English DT Article AB The phylogenetic position of Wenchengia is considered in the light of new data on its pollen morphology and leaf epidermal anatomy. The pollen is tricolpate, tectate-perforate, supra-reticulate and has simple columellae. Leaves are hypostomatic, with mainly diacytic and diallelocytic stomata. Wenchengia appears to be most closely related to Ajuga, Cymaria, or Acrymia. A position close to Scutellaria, Tinnea, and Renschia is only slightly less parsimonious. Although Wenchengia was originally segregated as a monotypic subfamily, assignment to Ajugoideae or Scutellarioideae may be more consistent with a phylogenetic classification of the family. C1 SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. RP CANTINO, PD (reprint author), OHIO UNIV,DEPT ENVIRONM & PLANT BIOL,ATHENS,OH 45701, USA. NR 18 TC 5 Z9 5 U1 0 U2 1 PU INT ASSN PLANT TAXONOMY PI BERLIN PA BOTANISCHER GARTEN & MUSEUM KONIGIN-LUISSE-STRASSE 6-8, W-1000 BERLIN, GERMANY SN 0040-0262 J9 TAXON JI Taxon PD MAY PY 1993 VL 42 IS 2 BP 339 EP 344 DI 10.2307/1223142 PG 6 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA LE154 UT WOS:A1993LE15400003 ER PT J AU NARAYAN, R POPHAM, R AF NARAYAN, R POPHAM, R TI HARD X-RAYS FROM ACCRETION DISK BOUNDARY-LAYERS SO NATURE LA English DT Article ID T-TAURI STARS; CATACLYSMIC VARIABLES; EMISSION; MODEL; SPECTRUM AB ACCRETION disks1,2 are found in many astrophysical objects, ranging from newly formed stars and mass-transferring binary systems to quasars and other active galactic nuclei. An important feature of accretion disks is the boundary layer-the interface between the disk and the accreting objects-where up to half the accretion luminosity may be liberated. The lack of a satisfactory description of the flow and thermal structure of this layer has long been a handicap when modelling disk spectra. Here we report numerical solutions of a model of thin accretion disks around a central white dwarf which includes a self-consistent description of the boundary layer. We find two distinct kinds of solution depending on the mass accretion rate M. At high rates, we find optically thick boundary layers whose radial width and peak temperature decrease with decreasing M, but when the accretion rate falls below a critical value, the boundary layer becomes optically thin, and the width and temperature increase dramatically. Our results provide an explanation for the hard X-rays observed3 in cataclysmic variables, particularly at low M. It should be possible to extend our analysis to other accretion-disk systems. RP NARAYAN, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 20 TC 121 Z9 121 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD APR 29 PY 1993 VL 362 IS 6423 BP 820 EP 822 DI 10.1038/362820a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA KZ563 UT WOS:A1993KZ56300048 ER PT J AU STELBOVICS, AT KUMAR, M WILLIAMS, JF AF STELBOVICS, AT KUMAR, M WILLIAMS, JF TI COMMENT ON ANGULAR-CORRELATIONS FROM COHERENT EXCITATION OF THE N=3 LEVELS OF ATOMIC-HYDROGEN SO JOURNAL OF PHYSICS B-ATOMIC MOLECULAR AND OPTICAL PHYSICS LA English DT Letter ID 32DJ STATES; ELECTRON-IMPACT AB Several errors in the theory of the angular correlations dealing with the electron-impact excitation of hydrogen atoms to n = 3 levels and with the detection of the cascade Lyman-alpha photon in coincidence with the scattered electron are noted and corrected. In one case, a state multipole, derived from measurements of the circular polarization of the photon, has to be substantially readjusted. C1 MURDOCH UNIV,CTR ATOM MOLEC & SURFACE PHYS,SCH MATH & PHYS SCI,MURDOCH,WA 6150,AUSTRALIA. UNIV WESTERN AUSTRALIA,CTR ATOM MOLEC & SURFACE PHYS,DEPT PHYS,NEDLANDS,WA 6009,AUSTRALIA. RP STELBOVICS, AT (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,ITAMP,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 5 TC 4 Z9 4 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0953-4075 J9 J PHYS B-AT MOL OPT JI J. Phys. B-At. Mol. Opt. Phys. PD APR 28 PY 1993 VL 26 IS 8 BP L237 EP L241 DI 10.1088/0953-4075/26/8/005 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA LE976 UT WOS:A1993LE97600005 ER PT J AU KENYON, SJ AF KENYON, SJ TI STRUCTURE AND EVOLUTION OF SINGLE AND BINARY STARS - DELOORE,CWH, DOOM,C SO SCIENCE LA English DT Book Review RP KENYON, SJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD APR 23 PY 1993 VL 260 IS 5107 BP 569 EP 570 DI 10.1126/science.260.5107.569 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA KY504 UT WOS:A1993KY50400045 PM 17830440 ER PT J AU WHITMORE, BC GILMORE, DM JONES, C AF WHITMORE, BC GILMORE, DM JONES, C TI WHAT DETERMINES THE MORPHOLOGICAL FRACTIONS IN CLUSTERS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERING; GALAXIES, FUNDAMENTAL PARAMETERS ID DENSITY RELATION; COMPACT-GROUPS; VIRGO CLUSTER; RICH CLUSTERS; DISK GALAXIES; EVOLUTION; ROTATION; SPIRALS AB A reexamination of Dressler's sample of nearly 6000 galaxies in 55 clusters shows that the morphology-clustercentric radius relation is more fundamental than the morphology-local density relation. This conclusion is supported by improved correlations when the clustercentric radius is used as the independent parameter, and by a comparison of galaxies with the same normalized clustercentric radii but different values of the local density. The morphology-radius relation, when normalized by a characteristic cluster radius, R(c)opt, does not vary as a function of the number density within 0.5 Mpc, N0.5, the X-ray luminosity, L(x), or the velocity dispersion of the cluster, V(disp). This surprising result means that only one parameter is needed to determine the morphological fractions in clusters, namely R/R(c)opt. The elliptical fraction in the outer regions of clusters is relatively constant for all types of clusters, with a slight rise from about 10% in the outermost region to about 16% at R/R(c)opt = 1. For radii smaller than R/R(c)opt = 1 (generally about 0.5 Mpc for most clusters) the elliptical fraction rises rapidly, reaching values of 60%-70% near the center of the cluster. The S0 fraction rises moderately as the center is approached, and then falls sharply within about 0.2 Mpc of the center. The spiral fraction falls moderately as the clustercentric radius decreases and then falls rapidly near the center. The spiral fraction is essentially zero at the cluster center, even though spirals dominate everywhere else in the universe. These results indicate that some property of the cluster center plays the key role in determining the morphological fractions in clusters, and suggests the possibility that a destructive mechanism is controlling the morphological fractions rather than a formation mechanism. Using this basic idea as a starting point we developed the following simple model. The three basic assumptions are (1) the intrinsic morphological mix of galaxies is EASO + S + 1) = 10%/90%, (2) elliptical galaxies form first, followed by the cluster collapse, S0 galaxies, and finally spiral and irregular galaxies, and (3) during the cluster collapse, galaxies which are still protogalactic clouds of gas are destroyed, and the gas from these failed galaxies is added to the intracluster medium. The destruction of the late-forming spiral and SO protogalaxies near the cluster centers results in the increase in the elliptical fraction. This simple model can explain a wide range of observations. Besides explaining the morphological fractions, it also suggests that roughly half of the intracluster gas resulted from '' failed '' galaxies. The model is also consistent with the tidal radii that would be imposed by the mean tidal field of the clusters. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,SMITHSONIAN ASTROPHYS OBSERV,CAMBRIDGE,MA 02138. RP WHITMORE, BC (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 61 TC 241 Z9 241 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 1993 VL 407 IS 2 BP 489 EP 509 DI 10.1086/172531 PN 1 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KX399 UT WOS:A1993KX39900005 ER PT J AU VANDERMAREL, RP FRANX, M AF VANDERMAREL, RP FRANX, M TI A NEW METHOD FOR THE IDENTIFICATION OF NON-GAUSSIAN LINE-PROFILES IN ELLIPTIC GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ELLIPTIC AND LENTICULAR, CD; GALAXIES, KINEMATICS AND DYNAMICS; LINE, PROFILES ID DIFFERENTIAL POPULATION SYNTHESIS; VELOCITY DISPERSIONS; SURFACE PHOTOMETRY; SYSTEMS; KINEMATICS; SPECTRA; FAMILY; MODELS AB It is usually assumed that the line profiles (i.e., the distributions of stars over line-of-sight velocities) of elliptical galaxies have Gaussian shapes, characterized by a line strength gamma, mean radial velocity V, and velocity dispersion sigma. We relax this unnecessarily restrictive assumption and propose a decomposition of the line profile into orthogonal functions: the Gauss-Hermite series. This series naturally leads to two extra parameters that measure deviations of the line profile from a Gaussian: a parameter h3 measuring asymmetric deviations and a parameter h4 measuring symmetric deviations. Model calculations for the outer parts of spherical galaxies yield line profiles that can deviate significantly from Gaussians. Even for models with only mild velocity dispersion anisotropy the rms deviations from a Gaussian can be of order 10%. Approximating these line profiles by Gaussians yields systematic errors in the estimates of the mean radial velocity and velocity dispersion of 10% or more. The new method is used to derive line profiles for the elliptical galaxies IC 1459, NGC 1374, and NGC 4278. All three galaxies have asymmetric line profiles on the major axis, similar to those found earlier in galaxies with kinematically distinct cores. In addition we find evidence for symmetric deviations from a Gaussian. By fitting Gaussians to these asymmetric line profiles the amplitude of the rotation curve can be overestimated by 30% or more. The results for h3 and h4 are not strongly dependent on the spectral resolution of the observations. The results confirm the notion that elliptical galaxies have complex structures, due to their complex formation history. It is expected that accurate measurements of line profiles will provide additional constraints on models of galaxy structure and formation. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP VANDERMAREL, RP (reprint author), STERREWACHT LEIDEN,POSTBUS 9513,2300 RA LEIDEN,NETHERLANDS. NR 36 TC 526 Z9 527 U1 1 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 1993 VL 407 IS 2 BP 525 EP 539 DI 10.1086/172534 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KX399 UT WOS:A1993KX39900008 ER PT J AU SMITH, RC KIRSHNER, RP BLAIR, WP LONG, KS WINKLER, PF AF SMITH, RC KIRSHNER, RP BLAIR, WP LONG, KS WINKLER, PF TI OPTICAL EMISSION-LINE PROPERTIES OF M33 SUPERNOVA-REMNANTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ABUNDANCES; GALAXIES, INDIVIDUAL (M33); H-II REGIONS; NEBULAE, SUPERNOVA REMNANTS ID H-II-REGIONS; GALACTIC ABUNDANCE GRADIENT; LARGE MAGELLANIC CLOUD; X-RAY-EMISSION; NOVA REMNANTS; SPIRAL GALAXIES; DIAGNOSTIC DIAGRAMS; THEORETICAL-MODELS; SHOCK-WAVES; RESOLUTION AB We have obtained spectra of the 42 supernova remnants (SNRs) and remnant candidates identified in the recent survey of the inner portion of M33. Relative fluxes for the important diagnostic emission lines in the red portion of the optical spectrum (6200-7500 angstrom) are reported. We have confirmed that all the candidate SNRs have [S II]/Halpha ratios greater-than-or-equal-to 0.4, the canonical dividing line between SNR emission and emission from the photoionized gas in H II regions and planetary nebulae. Significant [O I] emission, another distinguishing characteristic of shocked gas, is also seen in the majority of the remnants. We find little evidence of emission-line variation with SNR diameter, unlike that reported in previous SNR samples. Using published grids of shock models, we derive abundances and abundance gradients in the interstellar gas in M33. While the oxygen abundances and gradient derived agree (to within the rather large errors) with those derived from H II region studies, the nitrogen abundances and gradient show the same offset as previously noted in studies of other galaxies. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. JOHNS HOPKINS UNIV,CTR ASTROPHYS SCI,BALTIMORE,MD 21218. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. MIDDLEBURY COLL,DEPT PHYS,MIDDLEBURY,VT 05753. RP SMITH, RC (reprint author), CERRO TOLOLO INTERAMER OBSERV,CASILLA 603,LA SERENA 1353,CHILE. NR 70 TC 54 Z9 54 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 1993 VL 407 IS 2 BP 564 EP 578 DI 10.1086/172538 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KX399 UT WOS:A1993KX39900012 ER PT J AU SUNYAEV, RA MARKEVITCH, M PAVLINSKY, M AF SUNYAEV, RA MARKEVITCH, M PAVLINSKY, M TI THE CENTER OF THE GALAXY IN THE RECENT PAST - A VIEW FROM GRANAT SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXY, CENTER; ISM, INDIVIDUAL (SGR A, SGR B2); X-RAYS, GALAXIES ID 6.7-KEV IRON LINE; X-RAY; GALACTIC-CENTER; EMISSION AB We present 15' resolution images of the extended source (approximately 1.degrees5) in the center of our Galaxy made with the ART-P telescope onboard Granat, in the energy bands 2.5-5 keV, 5-8.5 keV, and, for the first time, in the harder 8.5-22 keV interval. In the 2.5-8.5 keV band, we see a source of roughly the same shape as that found by Spartan 1, Spacelab 2, and Ginga. At higher energies, this source appears much more elongated parallel to the Galactic plane and has some features in common with the map of the molecular gas clouds. This leads us to suggest that part of the observed X-ray flux (at least at higher energies) may be X-rays from nearby compact sources, Thomson-scattered by dense molecular gas. The scattered X-ray flux from such gas which resides in this region, illuminated by the presently observed nearby X-ray sources, is expected to be more than 0.1 of the observed hard X-ray flux from the diffuse source, the uncertainty arising mainly from contradictory estimates of the molecular gas mass. Also, it is not unlikely that the nearby sources have been brighter in the past. Whether or not the flux we observed is due to Thomson scattering, we find that the Galactic center has not been much brighter in X-rays during the past several hundred years. Moreover, if there is a supermassive black hole in the Galactic nucleus, it has not emitted at the level of its Eddington luminosity for even a day over the last 400 yr. Under the simple assumption of bremsstrahlung emission from a hot gas, the average temperature of the diffuse source is found to be kT(e) = 15(-5)+10 keV (1 sigma errors), kT(e) > 8 keV at the 95% confidence level. At the position of the Sgr B2 molecular cloud, the measured temperature is greater than 15 keV at the 95% confidence level. If the harder energy emission is due to Thompson scattering, the component emitting in the 6.7 keV line need not be so hot. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP SUNYAEV, RA (reprint author), ACAD SCI,INST SPACE RES,PROFSOYUZNAYA 84-32,MOSCOW 117810,RUSSIA. NR 26 TC 139 Z9 139 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 1993 VL 407 IS 2 BP 606 EP 610 DI 10.1086/172542 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KX399 UT WOS:A1993KX39900016 ER PT J AU KENYON, SJ LIVIO, M MIKOLAJEWSKA, J TOUT, CA AF KENYON, SJ LIVIO, M MIKOLAJEWSKA, J TOUT, CA TI ON SYMBIOTIC STARS AND TYPE IA SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, GENERAL; STARS, EVOLUTION; SUPERNOVAE, GENERAL ID ACCRETING WHITE-DWARFS; SPACE DENSITY; EVOLUTION; BINARIES; PROGENITORS; PERIOD AB We examine the possibility that symbiotic stars-wide binaries containing a red giant and a white dwarf-produce a significant fraction of Type Ia supernovae (SN Ia). These binaries probably cannot account for SN Ia events if the white dwarf mass must evolve to the Chandrasekhar limit during the expected lifetime of the red giant primary star. However, symbiotic binaries are good candidates for helium detonation supernovae in low-mass white dwarfs. If helium detonations can produce the majority of SN Ia events, then symbiotic stars might account for a large fraction of Type Ia supernovae. C1 TECHNION ISRAEL INST TECHNOL,DEPT PHYS,IL-32000 HAIFA,ISRAEL. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. NICOLAUS COPERNICUS ASTRON CTR,PL-00716 WARSAW,POLAND. UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 0HA,ENGLAND. RP KENYON, SJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 46 TC 52 Z9 52 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 1993 VL 407 IS 2 BP L81 EP L84 DI 10.1086/186811 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KX400 UT WOS:A1993KX40000011 ER PT J AU HERKEN, G AF HERKEN, G TI GENIUS IN THE SHADOWS - A BIOGRAPHY OF SZILARD,LEO - THE MAN BEHIND THE BOMB - LANOUETTE,W, SILARD,B SO NATURE LA English DT Book Review RP HERKEN, G (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,DEPT SPACE HIST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD APR 15 PY 1993 VL 362 IS 6421 BP 661 EP 661 DI 10.1038/362661a0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA KX438 UT WOS:A1993KX43800065 ER PT J AU CRUTCHER, RM TROLAND, TH GOODMAN, AA HEILES, C KAZES, I MYERS, PC AF CRUTCHER, RM TROLAND, TH GOODMAN, AA HEILES, C KAZES, I MYERS, PC TI OH ZEEMAN OBSERVATIONS OF DARK CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, CLOUDS; ISM, MAGNETIC FIELDS; ISM, MOLECULES ID MAGNETIC INTERSTELLAR CLOUDS; MOLECULAR CLOUDS; ISOTHERMAL CLOUDS; STAR FORMATION; NONHOMOLOGOUS CONTRACTION; INTERCLOUD MEDIUM; FIELD STRENGTHS; EQUILIBRIA; EVOLUTIONS; TAURUS AB We have made measurements with the Green Bank 43 m telescope of the Zeeman effect in the 1665 and 1667 MHz lines of OH toward dark clouds. The typical 1 sigma sensitivity was 3 muG. The only certain detection of a magnetic field was toward B1, for which we measured a line-of-sight component Absolute value of B cos theta = - 19.1 +/- 3.9 muG. Comparison with our earlier measurement of the field toward B1 with the Arecibo telescope provided evidence for a 40% enhancement in field strength between the molecular envelope and core of the B1 cloud, which is consistent with quasi-static contraction of the cloud driven by ambipolar diffusion. Because the Zeeman effect is only sensitive to the line-of-sight component of the magnetic field, a statistical analysis of the detection and upper limits was necessary. This analysis indicated that the total (not line-of-sight) field strength was typically Absolute value of B almost-equal-to 16 muG toward the central regions of dark clouds sampled by the Green Bank beam (for which A(v) almost-equal-to 5 mag and n(H) is similar to 10(3) cm-3), which implied that the central regions were approximately magnetically critical. The data were found to be consistent with the hypotheses that (1) dark clouds are in approximate virial equilibrium between magnetic and gravitational energy and (2) the supersonic line widths observed in dark clouds are the result of MHD motions such as Alfven waves. The data were also consistent with detailed physical models of initially magnetically subcritical clouds evolving on the ambipolar diffusion time scale. C1 OBSERV PARIS, F-92195 MEUDON, FRANCE. UNIV KENTUCKY, DEPT PHYS & ASTRON, LEXINGTON, KY 40506 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV CALIF BERKELEY, DEPT ASTRON, BERKELEY, CA 94720 USA. RP UNIV ILLINOIS, DEPT ASTRON, URBANA, IL 61801 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 39 TC 121 Z9 121 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 1993 VL 407 IS 1 BP 175 EP 184 DI 10.1086/172503 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KV285 UT WOS:A1993KV28500018 ER PT J AU HARTMANN, L KENYON, SJ CALVET, N AF HARTMANN, L KENYON, SJ CALVET, N TI THE EXCESS INFRARED-EMISSION OF HERBIG AE/BE STARS - DISKS OR ENVELOPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; CIRCUMSTELLAR MATTER; STARS, EMISSION-LINE, BE; STARS, PRE-MAIN-SEQUENCE ID T-TAURI STARS; YOUNG STELLAR OBJECTS; POLYCYCLIC AROMATIC-HYDROCARBONS; VISUAL REFLECTION NEBULAE; ORION POPULATION STARS; ACCRETION DISKS; INTERSTELLAR DUST; LINE FORMATION; SMALL GRAINS; EVOLUTION AB We suggest that the near-infrared emission of many Herbig Ae/Be stars arises in surrounding dusty envelopes, rather than circumstellar disks. Hillenbrand et al. and Lada & Adams showed that circumstellar disk models which reproduce the approximately 3 mum peaks in the near-infrared spectral energy distributions of Ae/Be stars must have high accretion rates, and must either be transparent in their inner regions, or have physical inner disk ''holes.'' However, we show that disks around Ae/Be stars are likely to remain optically thick at the required accretion rates. Alternatively, the assumption of a physical hole in the disk implies either that large amounts of material pile up at approximately 10 stellar radii or that approximately 90% of the accretion luminosity escapes detection. To avoid these difficulties we propose that the infrared excesses of many Ae/Be stars originate in surrounding dust nebulae instead of circumstellar disks. These dust envelopes could be associated with the primary star or a nearby companion star. One picture supposes that the near-infrared emission of the envelope is enhanced by the same processes that produce anomalously strong continuum emission at temperatures approximately 1000 K in reflection nebulae surrounding hot stars. This near-infrared emission could be due to small grains transiently heated by ultraviolet photons. Some Ae/Be stars show evidence for the 3.3-3.6 mum emission features seen in reflection nebulae around hot stars, which lends further support to this suggestion. Given the difficulties of applying circumstellar disk models to Ae/Be stars, dusty nebula hypotheses deserve further consideration. C1 CTR INVEST ASTRON, MERIDA 5101A, VENEZUELA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 77 TC 134 Z9 135 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 1993 VL 407 IS 1 BP 219 EP 231 DI 10.1086/172507 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KV285 UT WOS:A1993KV28500022 ER PT J AU FRANX, M AF FRANX, M TI KINEMATICS OF AN E+A GALAXY IN ABELL-665 AT Z=0.18 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, EVOLUTION; GALAXIES, KINEMATICS AND DYNAMICS; GALAXIES, PHOTOMETRY ID CLUSTERS; EVOLUTION; PHOTOMETRY; DISTANCES; REDSHIFT AB The first profiles of rotational velocity and velocity dispersion are presented of a blue ''Butcher-Oemler'' galaxy in an intermediate-redshift cluster, Abell 665, at z = 0.18. A deep, high spectral resolution spectrum shows that the galaxy rotates rapidly, with an observed rotation speed of 180 km s-1. A lower resolution spectrum clearly shows that the galaxy has two population components, a young component resembling an A star spectrum, and an old component resembling a K star spectrum. This galaxy is therefore similar to ''E + A'' galaxies discovered previously by Dressler & Gunn in intermediate-redshift clusters. The luminosity profiles and kinematics of the two components are quite similar. The younger component is possibly more extended, and may be rotating faster in the center. This blue galaxy shows a large residual from the Faber-Jackson relation for the red galaxies in the same cluster. If it were an ordinary elliptical, it would be too bright by 2.2 +/- 0.5 mag in the I band. This is much larger than can be explained by the contribution of the young component. The Tully-Fisher relation implies a much smaller discrepancy of 0.3 +/- 0.3 mag. All the data are consistent with the hypothesis that the E + A galaxy is a disk galaxy, which is evolving into a cluster spiral or an SO galaxy with low star formation rate at z = 0. There appear to be many possible counterparts in a nearby rich cluster like Coma. C1 UNIV ARIZONA,SMITHSONIAN INST,MULTIPLE MIRROR TELESCOPE,TUCSON,AZ 85721. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 23 TC 52 Z9 52 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 1993 VL 407 IS 1 BP L5 EP L8 DI 10.1086/186792 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KV287 UT WOS:A1993KV28700002 ER PT J AU PRESS, WH AF PRESS, WH TI SUPERCOMPUTING AND THE TRANSFORMATION OF SCIENCE - KAUFMANN,WJ, SMARR,LL SO NATURE LA English DT Book Review RP PRESS, WH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 1 TC 0 Z9 0 U1 1 U2 1 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD APR 8 PY 1993 VL 362 IS 6420 BP 507 EP 507 DI 10.1038/362507a0 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA KW453 UT WOS:A1993KW45300039 ER PT J AU EMMONS, LH AF EMMONS, LH TI ON THE IDENTITY OF ECHIMYS-DIDELPHOIDES DESMAREST, 1817 (MAMMALIA, RODENTIA, ECHIMYIDAE) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB Two early names for species of the genus Echimys (Makalata), E. didelphoides and Loncheres obscura, were erroneously assigned to the genus Mesomys by Tate (1935). One of these, didelphoides, is the oldest name for the red-nosed tree rats currently known as Makalata armata. RP EMMONS, LH (reprint author), SMITHSONIAN INST,MRC 108,WASHINGTON,DC 20560, USA. NR 16 TC 12 Z9 13 U1 0 U2 0 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD APR 8 PY 1993 VL 106 IS 1 BP 1 EP 4 PG 4 WC Biology SC Life Sciences & Biomedicine - Other Topics GA KX034 UT WOS:A1993KX03400001 ER PT J AU YENER, KA VANDIVER, PB AF YENER, KA VANDIVER, PB TI TIN PROCESSING AT GOLTEPE, AN EARLY BRONZE-AGE SITE IN ANATOLIA SO AMERICAN JOURNAL OF ARCHAEOLOGY LA English DT Review ID TAURUS MOUNTAINS; METALLURGY; BEGINNINGS; BOLKARDAG AB This paper presents the archaeological contexts and results of analyses of slags, surface residues, and earthenware refractories from the third-millennium B.C. site of Goltepe in south-central Turkey. These materials are only part of a workshop/habitation assemblage at the site, which also includes ore nodules, multifaceted molds, and metal fragments as well as groundstone tools utilized in ore dressing and beneficiation. Twenty-four ceramic fragments of bowl-shaped crucibles were analyzed as a representative sample from some 250 examples excavated in the 1990 season. Analysis suggests the intentional production of tin metal by reduction firing of tin oxide (cassiterite, SnO2) in crucibles. Tin oxide was identified on the interior surfaces of the crucible fragments by x-ray fluorescence, x-ray diffraction, scanning electron microscopy coupled with energy dispersive x-ray analysis, and wavelength dispersive microprobe analysis. The results of these tests have a direct bearing on the question of tin sources in ancient Anatolia. RP YENER, KA (reprint author), SMITHSONIAN INST, CONSERVAT ANALYT LAB, WASHINGTON, DC 20560 USA. NR 142 TC 39 Z9 39 U1 1 U2 4 PU ARCHAEOLOGICAL INST AMERICA PI BOSTON PA 656 BEACON STREET, BOSTON, MA 02215 USA SN 0002-9114 J9 AM J ARCHAEOL JI Am. J. Archaeol. PD APR PY 1993 VL 97 IS 2 BP 207 EP 238 DI 10.2307/505657 PG 32 WC Archaeology SC Archaeology GA KY247 UT WOS:A1993KY24700002 ER PT J AU WASHBURN, WE AF WASHBURN, WE TI SMITH GOES TO TOKYO - JAPANESE CINEMA UNDER THE AMERICAN OCCUPATION, 1945-1952 - HIRANO,K SO AMERICAN STUDIES INTERNATIONAL LA English DT Book Review RP WASHBURN, WE (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU GEORGE WASHINGTON UNIV PI WASHINGTON PA AMERICAN STUDIES PROGRAM, WASHINGTON, DC 20052 SN 0003-1321 J9 AM STUD INT JI Am. Stud. Int. PD APR PY 1993 VL 31 IS 1 BP 134 EP 135 PG 2 WC History SC History GA LA700 UT WOS:A1993LA70000025 ER PT J AU GERNSTEIN, JM AF GERNSTEIN, JM TI MISTER - THE TRAINING OF AN AVIATION CADET IN WORLD-WAR-II - FLETCHER,E SO AMERICAN STUDIES INTERNATIONAL LA English DT Book Review RP GERNSTEIN, JM (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU GEORGE WASHINGTON UNIV PI WASHINGTON PA AMERICAN STUDIES PROGRAM, WASHINGTON, DC 20052 SN 0003-1321 J9 AM STUD INT JI Am. Stud. Int. PD APR PY 1993 VL 31 IS 1 BP 151 EP 152 PG 2 WC History SC History GA LA700 UT WOS:A1993LA70000052 ER PT J AU PELETIER, RF CHRISTODOULOU, DM AF PELETIER, RF CHRISTODOULOU, DM TI A PHOTOMETRIC AND DYNAMIC STUDY OF THE HELIX GALAXY NGC-2685 SO ASTRONOMICAL JOURNAL LA English DT Article ID POLAR-RING GALAXIES; PREFERRED ORBIT PLANES; RAPIDLY ROTATING STARS; ELLIPTIC GALAXIES; GAS DISKS; GRAVITATIONAL-FIELD; TRIAXIAL GALAXIES; VERSATILE METHOD; S0 GALAXIES; DARK HALO AB We present optical and near-infrared surface photometry of the Helix galaxy NGC 2685 and its two rings. We detected the inner (''polar'') ring in the near-infrared J-band and found that its colors are consistent with a normal initial mass function and an age of at most 5-6 Gyr. The inner ring is almost as red as the central galaxy suggesting that it is a long-lived structure. The central galaxy may be either an SO or an E6/E7 galaxy and has a reddened nucleus. We have constructed gas-dynamical models of the inner self-gravitating ring in a variety of potentials and searched for long-lived models of both rings. These models indicate that the overall potential is either generally oblate-like triaxial or prolate-like triaxial in shape. Based on an analysis of the physical mechanism which can produce such a two-ring structure, we believe that the prolate-like triaxial model is the best current model. This model predicts that both rings achieve very long-lived states within only approximately 20 inner-ring rotation periods after the accretion of gas into the galaxy's potential. This time scale is in good agreement with the determined upper limit for the age of the inner ring. C1 EUROPEAN SO OBSERV, W-8046 GARCHING, GERMANY. UNIV VIRGINIA, DEPT ASTRON, CHARLOTTESVILLE, VA 22903 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RI Peletier, Reynier/B-9633-2012 NR 53 TC 22 Z9 24 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD APR PY 1993 VL 105 IS 4 BP 1378 EP 1391 DI 10.1086/116517 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU572 UT WOS:A1993KU57200012 ER PT J AU PETERSON, RC CALDWELL, N AF PETERSON, RC CALDWELL, N TI STELLAR VELOCITY DISPERSIONS OF DWARF ELLIPTIC GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article ID PRECISION RADIAL-VELOCITIES; VIRGO CLUSTER; SURFACE PHOTOMETRY; FAINT GIANTS; LOCAL GROUP; SPECTROSCOPY; STARS; MASS; DYNAMICS; NGC-205 AB We present new measurements of the central stellar velocity dispersions (sigma) of dwarf elliptical galaxies (dE's), most of them of the nucleated variety. The data consist of photon counting spectra taken at the MMT with spectral resolution of 12 and 32 km s-1 and CCD data from CTIO and KPNO at 8 and 18 km s-1 (FWHM). The measured dispersions range from 14 to 39 km-1, and are lower than previous measurements done at more coarse resolution by about 50%. M/L ratios are derived for the galaxies. These are not unusually high (1-7, in solar units), but the change in M/L with luminosity for all dE galaxies confirms a prediction made by Dekel and Silk [ApJ, 303, 39 (1986)] (M/L approximately L-0.40+/-0.06) as does the observed relation between L and velocity dispersion (L approximately sigma5.6+/-0.9). We use the data to investigate the fundamental plane for dE's. A limited sample for which complete data exist (L, R(e), S(e), and sigma) indicates the galaxies are a one parameter family, i.e., a single parameter accurately predicts the three other structural parameters. However, a larger photometric data set (for which a are mostly unknown) indicates that the dwarfs require two parameters, mainly to explain the large low surface brightness galaxies. We attribute that poor correlation of color with structural parameters to real variations in the stellar population of dE's. C1 SMITHSONIAN INST,FL WHIPPLE OBSERV,AMADO,AZ 85645. NR 45 TC 71 Z9 72 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 1993 VL 105 IS 4 BP 1411 EP 1419 DI 10.1086/116520 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU572 UT WOS:A1993KU57200015 ER PT J AU PROSSER, CF AF PROSSER, CF TI THE OPEN CLUSTER IC-4665 SO ASTRONOMICAL JOURNAL LA English DT Article ID BINARY FREQUENCY; INTERNAL MOTIONS; SPECTRAL TYPES; TIME-SERIES; M-DWARFS; IC 4665; PHOTOMETRY; PLEIADES; PRAESEPE; MEMBERS AB The results of a combined astrometric, photometric, and spectroscopic program to identify members of the open cluster IC 4665 are presented. Numerous new proper motion/photometric candidate members and at least 23 M dwarfs with Halpha emission have been identified. A reanalysis of IC 4665's age using different methods yields conflicting results ranging from approximately 3 X 10(7) yr to the age of the Pleiades. This study provides a list of candidate cluster members in the intermediate and low-mass regime of this cluster. Future spectroscopic observations of these candidates should eventually identify true cluster members. The results of new echelle observations of some candidates and the photometric monitoring of one apparent cluster member are given in an appendix. RP PROSSER, CF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,MS-66,CAMBRIDGE,MA 02138, USA. NR 42 TC 20 Z9 20 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 1993 VL 105 IS 4 BP 1441 EP 1454 DI 10.1086/116522 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU572 UT WOS:A1993KU57200017 ER PT J AU KENYON, SJ HARTMANN, L GOMEZ, M CARR, JS TOKUNAGA, A AF KENYON, SJ HARTMANN, L GOMEZ, M CARR, JS TOKUNAGA, A TI RNO 1B/1C - A DOUBLE FU ORIONIS SYSTEM SO ASTRONOMICAL JOURNAL LA English DT Article ID YOUNG STELLAR OBJECTS; Z-CANIS MAJORIS; T-TAURI STARS; MOLECULAR CLOUD; DISK ACCRETION; DENSE CORES; OUTFLOWS; SPECTRA; EVOLUTION; EMISSION AB We present infrared imaging and spectroscopic data of the RNO 1 region in the L1287 molecular cloud. Both RNO 1B and RNO 1C show the strong 2.3 mum CO absorption bands observed in the pre-mainsequence FU Orionis variables (FUors). These results confirm Staude & Neckel's [ApJ, 400, 556 (1992)] identification of RNO 1B as a FUor from optical spectra; its nearby (6'' separation), heavily extincted companion-RNO 1C-also appears to be a FUor. The combined light of RNO 1B/1C has a spectral energy distribution similar to the embedded FUor V1735 Cyg (Elias 1-12). Over half of the known FUors now appear deeply embedded within dusty molecular gas, which suggests they have ages of roughly 1-3 X 10(5) yr. Our JHK imaging observations exhibit extended near-IR emission along the axis of the molecular outflow from RNO 1B/1C, with morphology similar to the extended I-band emission discovered by Staude & Neckel (1992). These observations and the spatial coincidence of the outflow center with RNO 1B/1C suggest one-perhaps both-of these objects drives the outflow. We show that the FUor wind can power this outflow-and the outflow in L1551 IRS5-if a young star spends roughly 5% of its pre-main-sequence lifetime as a FUor; this duty cycle agrees very well with the time needed to fill its circumstellar disk between eruptions given estimated infall rates. C1 OHIO STATE UNIV,DEPT ASTRON,COLUMBUS,OH 43210. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. RP KENYON, SJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Kenyon, Scott/0000-0003-0214-609X NR 61 TC 53 Z9 54 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 1993 VL 105 IS 4 BP 1505 EP 1510 DI 10.1086/116529 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU572 UT WOS:A1993KU57200024 ER PT J AU PELETIER, RF AF PELETIER, RF TI THE STELLAR CONTENT OF ELLIPTIC GALAXIES - OPTICAL AND INFRARED COLOR PROFILES OF M32 AND NGC-205 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE GALAXIES, DWARF ELLIPTICALS; GALAXIES, ELLIPTICALS; GALAXIES, INDIVIDUAL, M-32; GALAXIES, INDIVIDUAL, NGC-205; GALAXIES, STELLAR CONTENT OF; INFRARED RADIATION ID CCD SURFACE PHOTOMETRY; POPULATIONS; SPECTROSCOPY; PARAMETERS; GRADIENTS; SYSTEM; ORIGIN; LAW AB We have obtained high quality surface photometry of the two brightest companiom galaxies of M 31 in optical and infrared colours. We find that in M 32 all colours, as well as the CO band, do not depend on radius from the center. This is consistent with profiles in the Mg2 index available for this galaxy in the literature, but not in other, mostly weaker, lines. In this respect M 32 follows the trend for compact elliptical galaxies, which contrary to giant ellipticals in general do not display any colour gradients. Since all compact ellipticals are companions to brighter galaxies and are tidally truncated we presume that the tidal interaction must be responsible for the removal of the interstellar material at a certain epoch, so that all star formation stopped. In NGC 205 we find a very blue center and colours that get redder slowly when going outward. The colour gradient reverses sign at almost-equal-to 60''. Because of the presence of very young stars near the center we attribute the gradient in the inner areas to a difference in age. Optical and optical-infrared gradients are consistent with being caused by metallicity or age. C1 EUROPEAN SO OBSERV, W-8046 GARCHING, GERMANY. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RI Peletier, Reynier/B-9633-2012 NR 50 TC 75 Z9 75 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 1993 VL 271 IS 1 BP 51 EP 64 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU738 UT WOS:A1993KU73800010 ER PT J AU ALBERDI, A KRICHBAUM, TP MARCAIDE, JM WITZEL, A GRAHAM, DA INOUE, M MORIMOTO, M BOOTH, RS RONNANG, BO COLOMER, F ROGERS, AEE ZENSUS, JA READHEAD, ACS LAWRENCE, CR VERMEULEN, R BARTEL, N SHAPIRO, II BURKE, BF AF ALBERDI, A KRICHBAUM, TP MARCAIDE, JM WITZEL, A GRAHAM, DA INOUE, M MORIMOTO, M BOOTH, RS RONNANG, BO COLOMER, F ROGERS, AEE ZENSUS, JA READHEAD, ACS LAWRENCE, CR VERMEULEN, R BARTEL, N SHAPIRO, II BURKE, BF TI 1ST 7-MM VLBI OBSERVATIONS OF THE PECULIAR SUPERLUMINAL RADIO-SOURCE 4C-39.25 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE INTERFEROMETRY; JETS OF QUASARS ID ANGULAR RESOLUTION; 4C 39.25; MOTION; 3C273; CORE AB On sub-milliarcsecond to milliarcsecond scales the quasar 4C 39.25 consists of two ''stationary'' jet components a and c between which a component b is moving superluminally eastward towards a. From global VLBI observations at 7 mm we have obtained the first image of 4C 39.25 at this wavelength. The high angular resolution of 7 mm-VLBI maps allows us to follow the motion of b towards a to separations not resolvable by VLBI-observations at longer wavelengths. The present observations also confirm the existence of a new jet component d detected recently with VLBI at 1.3 cm wavelength. The component is located approximately 2.7 mas west of a and seems to have an inverted spectrum between 1.3 cm and 7 mm. We suggest that d is either the ''core'' of 4C 39.25 or is a recently ejected new jet component with a time-evolving spectrum. C1 MAX PLANCK INST RADIOASTRON, W-5300 BONN 1, GERMANY. UNIV VALENCIA, VALENCIA, SPAIN. NOBEYAMA RADIO OBSERV, NOBEYAMA, JAPAN. ONSALA SPACE OBSERV, ONSALA, SWEDEN. HAYSTACK OBSERV, NEROC, WESTFORD, MA USA. NATL RADIO ASTRON OBSERV, SOCORRO, NM 87801 USA. CALTECH, PASADENA, CA 91125 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. YORK UNIV, N YORK M3J 1P3, ONTARIO, CANADA. MIT, CAMBRIDGE, MA 02139 USA. RP ALBERDI, A (reprint author), INST ASTROFIS ANDALUCIA, APARTADO 3004, E-18080 GRANADA, SPAIN. NR 34 TC 15 Z9 15 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 1993 VL 271 IS 1 BP 93 EP 100 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU738 UT WOS:A1993KU73800015 ER PT J AU BAUDRY, A MENTEN, KM WALMSLEY, CM WILSON, TL AF BAUDRY, A MENTEN, KM WALMSLEY, CM WILSON, TL TI VLA OBSERVATIONS OF THE 8 GHZ ROTATIONALLY EXCITED OH LINES TOWARD W3(OH) SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE H-II REGIONS; MASERS; EXCITATION; OH; STAR FORMATION; W3(OH) ID H-II REGIONS; VLBI SYNTHESIS OBSERVATIONS; MASER EMISSION; W3 OH; RESOLUTION MAPS; SHELL STRUCTURE; 4765 MHZ; DISCOVERY; AMMONIA; STARS AB The 2pi1/2, J = 3/2 and J = 5/2 main lines of OH and the continuum, at 8 GHz, have been mapped toward W3(OH) with an angular resolution of 0.3'' and a resolution of 0.45-0.47 km s-1. The continuum maps produced in conjunction with each spectral line map were combined. In addition to the four previously found continuum features, we have tentatively detected a new weak, unresolved source. This coincides with a weak 1.7 GHz OH maser, about 7'' NE of W3(OH). The 2pi1/2, J = 3/2, F = 2-2 and F = 1-1 main lines at 7820 and 7762 MHz, respectively, are found in absorption toward the western part of W3(OH), and both show a clumpy structure. There is a weak emission feature at 7820 MHz, about 0.5'' NE of the northern absorption clump. The 2pi1/2, J = 5/2, F = 2-2 main line, at 8136 MHz, shows only absorption, while the F = 3-3 main line, at 8190 MHz, is present in weak emission; this emission overlaps the 7820 MHz emission region. The flux density of the F = 3-3 line has been redetermined with the 100-m telescope; this line is not polarized, and there has been no significant change in properties since 1988. There are deviations from LTE excitation for these lines; comparisons with OH excitation models are made. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. MAX PLANCK INST RADIOASTRON, W-5300 BONN 1, GERMANY. RP OBSERV BORDEAUX, BP 89, F-33270 FLOIRAC, FRANCE. NR 36 TC 26 Z9 26 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 1993 VL 271 IS 2 BP 552 EP 563 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KY482 UT WOS:A1993KY48200027 ER PT J AU WRIGHT, MCH ISHIZUKI, S TURNER, JL HO, PTP LO, KY AF WRIGHT, MCH ISHIZUKI, S TURNER, JL HO, PTP LO, KY TI HETEROGENOUS ARRAY OBSERVATIONS OF IC-342 - THE CO ISOTOPIC RATIO SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (IC-342); GALAXIES, ISM; GALAXIES, KINEMATICS AND DYNAMICS; ISM, MOLECULES ID CLUMPY MOLECULAR GAS; IC 342; WARM; DISTRIBUTIONS; EMISSION; GALAXIES; NUCLEUS; DISKS AB We present images of the (CO)-C-13 and (CO)-C-12 J = 1-0 emission from the nuclear region of the galaxy IC 342 with 3'' resolution. The images were obtained by combining data from the BIMA, OVRO, and Nobeyama millimeter arrays. The data processing using the MIRIAD software is described in some detail. The (CO)-C-12 and (CO)-C-13 images are very similar in appearance with an average (CO)-C-12/(CO)-C-13 ratio of approximately 9 over the central arcminute. The molecular gas forms two spiral features with a number of prominent peaks which are also seen in HCN emission. The (CO)-C-12/(CO)-C-13 line ratio varies from 3 to 24 with peaks at the position of the thermal continuum where the gas is heated by the star formation, and further out in the spiral features where the gas density is reduced. The molecular emission peaks correspond to molecular clouds with diameters 20-50 pc and masses approximately 10(6) M.. The total molecular mass within the central arcminute is 4.4 x 10(7) MD. The CO emission peaks lic between the more diffuse (CO)-C-12 emission and the peak Halpha emission. This can be understood as due to compression of the gas by a density wave with the CO peaks tracing the dense cloud cores. C1 NOBEYAMA RADIO OBSERV, MINAMISA KU, NAGANO 38413, JAPAN. UNIV CALIF LOS ANGELES, DEPT ASTRON, LOS ANGELES, CA 90024 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV ILLINOIS, DEPT ASTRON, URBANA, IL 61801 USA. RP WRIGHT, MCH (reprint author), UNIV CALIF BERKELEY, RADIO ASTRON LAB, BERKELEY, CA 94720 USA. NR 23 TC 21 Z9 21 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 1993 VL 406 IS 2 BP 470 EP 476 DI 10.1086/172458 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU607 UT WOS:A1993KU60700012 ER PT J AU GREENHILL, LJ MORAN, JM REID, MJ MENTEN, KM HIRABAYASHI, H AF GREENHILL, LJ MORAN, JM REID, MJ MENTEN, KM HIRABAYASHI, H TI MICROARCSECOND PROPER MOTIONS OF EXTRAGALACTIC WATER-VAPOR MASERS IN M33 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ASTROMETRY; GALAXIES, ISM; GALAXIES, INDIVIDUAL (M33); H-II REGIONS; ISM, INDIVIDUAL (IC 133); MASERS ID DISTANCES; HYDROGEN AB We present a second-epoch spectral line VLBI synthesis map of the H2O Maser associated with the H II region IC 133 in the galaxy M33. This map is about 2.5 times more sensitive than the earlier one. Thirty-two spatially distinct maser features have been identified, and we have discovered a second center of maser activity within the IC 133 complex, IC 133 West, which is displaced almost-equal-to 0.3 (1 pc at a nominal distance of 720 kpc) from IC 133 Main. The most blueshifted maser features are located in IC 133 West, which may mark the location of a separate star forming region. Comparing the two available maps of IC 133, we have estimated the right ascension components of proper motion over a period of 479 days for five maser features to accuracies of between 7 and 16 muas. The dispersions in transverse and radial velocities for the maser features are consistent with the accepted distance to M33 of 720 kpc, where the data admit a fractional uncertainty in distance of 50%. Our result represents the first successful measurements of proper motions in an extragalactic H2O maser source and demonstrate the feasibility of making such measurements in other galaxies. Improvements in this technique may make it important for the estimation of extragalactic distances. C1 NOBEYAMA RADIO OBSERV,MINAMISA KU,NAGANO 38413,JAPAN. RP GREENHILL, LJ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 18 TC 30 Z9 30 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 1993 VL 406 IS 2 BP 482 EP 488 DI 10.1086/172460 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU607 UT WOS:A1993KU60700014 ER PT J AU GOODMAN, AA BENSON, PJ FULLER, GA MYERS, PC AF GOODMAN, AA BENSON, PJ FULLER, GA MYERS, PC TI DENSE CORES IN DARK CLOUDS .8. VELOCITY-GRADIENTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, CLOUDS; ISM, KINEMATICS AND DYNAMICS; ISM, MOLECULES; STARS, FORMATION ID ELONGATED CYLINDRICAL CLOUDS; ROTATING INTERSTELLAR CLOUDS; H-II REGIONS; ISOTHERMAL CLOUDS; MOLECULAR CLOUDS; STAR FORMATION; PROTOSTELLAR FORMATION; AMBIPOLAR DIFFUSION; POLYTROPIC CLOUDS; MAGNETIC BRAKING AB We present an analysis of motions consistent with uniform rotation in dense cores (density greater than or similar to 10(4) cm-3; size approximately 0.1 pc). Twenty-nine of the 43 cores studied have a statistically significant gradient. The detected gradients range in magnitude from 0.3 to 4 km s-1 pc-1, corresponding to 2 x 10(-3) < beta < 1.4, with typical values beta approximately 0.02, where beta is the ratio of rotational to gravitational energy. Some gradients are spatially continuous and are consistent with uniform rotation, but other apparent gradients are caused by clump-clump motion, or sharp localized gradients, within a map. The motions in L1495, B217, L1251, L43, B361, and L1551 are discussed in detail. In L1551, the residuals of the fit to the NH3 velocity field indicate an outflow from IRS 5 in the same direction as the CO outflow. Gradient ofientation appears to be preserved over a range of density, as evidenced by comparing results for NH3 to fits of (CO)-O-18 and CS maps. There appears to be no correlation between the inferred rotation axis and the orientation of elongated cores, a result consistent with the relatively small energy of rotation in these regions. The magnitude of the velocity gradient in a core has no relation to the absence or presence of an associated young stellar object. We find that the specific angular momentum, J/M, scales roughly as R3/2, where R represents the diameter of the FWHM intensity contour in a map. This relationship between specific angular momentum and cloud size can be understood if (a) cores are in approximate virial equilibrium, (b) line width scales as cloud size roughly according to DELTAnu is-proportional-to R1/2, and (c) beta is roughly constant (i.e., independent of R) over the range of scales studied. C1 UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. WELLESLEY COLL,WHITIN OBSERV,DEPT ASTRON,WELLESLEY,MA 02181. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 NR 75 TC 462 Z9 462 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 1993 VL 406 IS 2 BP 528 EP 547 DI 10.1086/172465 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU607 UT WOS:A1993KU60700019 ER PT J AU KOCHANEK, CS AF KOCHANEK, CS TI SOME IMPLICATIONS OF PSR 1259-63 SO ASTROPHYSICAL JOURNAL LA English DT Article DE BINARIES, ECLIPSING; PULSARS, INDIVIDUAL (PSR 1259-63); STARS, EMISSION-LINE, BE; STARS, MASS LOSS ID ECLIPSING MILLISECOND PULSAR; RAY TRANSIENT A0538-66; TIDAL CAPTURE; STELLAR WIND; UBV PHOTOMETRY; BINARY PULSAR; MODEL; STARS; EVOLUTION; EMISSION AB We estimate that the binary PSR 1259 - 63 consists of a M(ns) = 1.4 M. neutron star orbiting a M* = 20 M. Be star with orbital inclination sin (i) greater than or similar to 0.9 and pulsar period derivative P congruent-to 10(-15). Oscillations of the Be star excited by the close pericentric passages of the neutron star may produce an orbital period derivative of P0 approximately 10(-6), although the number is exponentially sensitive to the ratio of the stellar and pericentric radii. The tidally induced oscillations of the star can be detected as photometric fluctuations larger than 0.001 mag if P0 greater than or similar to 10(-8). The mass flux in the Be star wind is between 0.1 less than or similar to M8nu3 less than or similar to 1 where nu = 10(3)vu3 km s-1 is the wind velocity and M = 10(-8) M8 M. yr-1 is the mass flux. The upper limit is set by the observed limits on variations in the dispersion measure, and the lower limit is required for a reasonable stellar wind to produce the observed eclipse of the pulsar by free-free absorption. The existence of a coherent stellar wind to produce the absorption means that less than epsilon(c) less than or similar to 10(-2) M8nu3(-1)P-15(-1) of the pulsar spin-down energy can be coupled to the stellar wind for a pulsar spin-down rate of P = 10(-15) P15. If accretion onto neutron stars prevents pulsed radio emission, then the coupling must be greater than epsilon(c) greater than or similar to 10(-6) M8nu3(-3)P-15(-1) to prevent accretion in the range where the radio pulsar is seen. The neutron star disrupts part of the Be star disk during each pericentric encounter leading to dramatic variations in the emission-line profiles, particularly on the blueshifted side of the line. Except when the neutron star passes through the Be star's disk, this system should be a poor X-ray source, probably dominated by the coronal X-ray emission from the Be star. During the passage through the Be star disk the X-ray luminosity should approach levels typical of massive X-ray binaries for a period of about one week. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,DEPT ASTRON MS51,CAMBRIDGE,MA 02138. RP KOCHANEK, CS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 54 TC 27 Z9 27 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 1993 VL 406 IS 2 BP 638 EP 650 DI 10.1086/172475 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU607 UT WOS:A1993KU60700029 ER PT J AU ABADASIMON, M LECACHEUX, A BASTIAN, TS BOOKBINDER, JA DULK, GA AF ABADASIMON, M LECACHEUX, A BASTIAN, TS BOOKBINDER, JA DULK, GA TI THE SPECTRUM AND VARIABILITY OF RADIO-EMISSION FROM AE AQUARII SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; BINARIE, GENERAL; NOVAE, CATACLYSMIC VARIABLES; RADIO CONTINUUM, STARS; STARS, INDIVIDUAL (AE AQUARII) ID CATACLYSMIC VARIABLES; RAPID OSCILLATIONS; OBLIQUE ROTATOR; FLARES AB We report the first detections of the magnetic cataclysmic variable AE Aquarii at millimeter wavelengths. AE Aqr was detected at a wavelength lambda = 3.4 mm on five independent observing runs by the interferometer on the Plateau de Bure, France. It was also detected by the Caltech Submillimeter Observatory on Mauna Kea at a wavelength lambda = 1.25 mm. Both of these observations were accompanied by contemporaneous microwave observations at the Very Large Array. We use these data to show that (1) the time-averaged spectrum is generally well fitted by a power law S(nu) is-proportional-to nu(alpha), where alpha almost-equal-to 0.35-0.60, and (2) the power law extends to millimeter wavelengths-i.e., the spectral turnover is at a frequency higher than 240 GHz. We suggest that the spectrum is consistent with that expected from a superposition of flarelike events where the frequency distribution of initial flux density is a power law f(S0) is-proportional-to S-0(-epsilon) with index epsilon almost-equal-to 1.8. Within the context of this model, the high turnover frequency of the radio spectrum implies magnetic field strengths in excess of 250 G in the source. The observed properties of AE Aqr are compared to those of a related class of objects, the low-mass X-ray binaries. C1 NATL RADIO ASTRON OBSERV,SOCORRO,NM 87801. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV COLORADO,DEPT ASTROPHYS PLANETARY & ATMOSPHER SCI,BOULDER,CO 80303. RP ABADASIMON, M (reprint author), OBSERV PARIS,CNRS,URA 324,F-92190 MEUDON,FRANCE. NR 17 TC 36 Z9 36 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 1993 VL 406 IS 2 BP 692 EP 700 DI 10.1086/172479 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU607 UT WOS:A1993KU60700033 ER PT J AU BARSONY, M CHANDLER, CJ AF BARSONY, M CHANDLER, CJ TI THE CIRCUMSTELLAR DENSITY DISTRIBUTION OF L1551NE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, JETS AND OUTFLOWS; ISM, MAGNETIC FIELDS; STARS, FORMATION; STARS, INDIVIDUAL (L1551NE); STARS, PRE-MAIN-SEQUENCE ID STAR FORMATION; OBJECTS AB We report the results of submillimeter photometry and 800 mum mapping of L1551NE, the second brightest Class I source in the Taurus dark clouds. Simultaneous modeling of the continuum spectrum and the azimuthally averaged 800 mum radial profile of L1551NE indicates a circumstellar envelope with a rather shallow density gradient [rho(r) is-proportional-to r-1/2]. Such shallow density gradients, although unexpected theoretically, have now been found around a number of other low-mass young stellar objects. We suggest that the magnetic fields in these sources may play a role in determining the observed density distributions. C1 CALTECH,OWENS VALLEY RADIO OBSERV,PASADENA,CA 91125. RP BARSONY, M (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,MS-78,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 25 TC 29 Z9 29 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 1993 VL 406 IS 2 BP L71 EP & DI 10.1086/186789 PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU611 UT WOS:A1993KU61100008 ER PT J AU BLOEMHOF, EE AF BLOEMHOF, EE TI DIAGONALIZATION OF THE VELOCITY VARIANCE COVARIANCE-MATRIX AS A DIAGNOSTIC OF MASER PROPER MOTIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE H-II REGIONS; ISM, INDIVIDUAL, W3(OH); ISM, KINEMATICS AND DYNAMICS; MASERS; METHODS, MISCELLANEOUS ID RESOLUTION MAPS; DISTANCES AB A new computational technique is presented for analyzing the velocity fields mapped by VLBI (very long baseline interferometry) proper-motion studies of astrophysical masers. Such studies, despite yielding kinematic information of great detail on unprecedented spatial scales, generally cannot determine the absolute motions of maser spots through the sky, or with respect to other nearby objects. The resulting ambiguity hinders physical interpretation, but can be partially overcome by constructing and diagonalizing the velocity variance/covariance matrix (VVCM) for a set of relative maser motions. Applied to the OH masers in W3(OH), VVCM diagonalization provides strong support for the cometary bow-shock model. RP BLOEMHOF, EE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 14 TC 10 Z9 10 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 1993 VL 406 IS 2 BP L75 EP L78 DI 10.1086/186790 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU611 UT WOS:A1993KU61100009 ER PT J AU SODERBLOM, DR STAUFFER, JR HUDON, JD JONES, BF AF SODERBLOM, DR STAUFFER, JR HUDON, JD JONES, BF TI ROTATION AND CHROMOSPHERIC EMISSION AMONG F-DWARFS, G-DWARFS, AND K-DWARFS OF THE PLEIADES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Review DE OPEN CLUSTERS AND ASSOCIATIONS, INDIVIDUAL (PLEIADES); STARS, CHROMOSPHERES; STARS, LATE-TYPE; STARS, ROTATION ID SOLAR-TYPE STARS; MAIN-SEQUENCE STARS; LOW-MASS STARS; T-TAURI STARS; H-ALPHA EMISSION; CA-II H; SPECTROSCOPIC BINARY GLIESE-268; X-RAY SURVEY; MAGNETIC ACTIVITY; EVOLUTIONARY MODELS AB We report and discuss high-resolution echelle spectra of more than 100 F, G, and K dwarfs in the Pleiades. Comparisons of the profiles of Halpha and the Ca II infrared triplet to chromospherically inactive field stars allow us to measure chromospheric activity in these stars, and we have determined v sin i values to a limit of 7 km s-1. We have combined these new observations with published data and have conducted a census to assess the state of our knowledge of Pleiades solar-type stars. After allowing for a patch of heavy reddening in the southwest part of the cluster, consistent dereddened colors are determined from the available photometry and temperatures are derived. Rotation is fully resolved in the Pleiades for stars more massive than the Sun, but for less massive stars there are still too many upper limits to v sin i to determine the underlying, intrinsic distribution of rotation. Over the entire mass range we consider (1.4 greater than or similar to M / M. greater than or similar to 0.6), no single value can characterize rotation at any one mass because the spread is too large. Most G and K dwarfs in the Pleiades rotate slowly (v sin i less than or similar to 10 km s-1), but approximately 20% of the stars are ultrafast rotators (UFRs) with v sin i greater than or similar to 30 km s-1. That fraction of UFRs is independent of color, and the highest rotation rates are found among the K dwarfs. The surfaces of the many slowly rotating solar-type stars in the Pleiades are already rotating at or near the rate of stars of the same mass in the Hyades. That means that the dominant aspect of the evolution of rotation from the age of the Pleiades to the Hyades is convergence in rotation. Among the F dwarfs, the degree of convergence is about a factor of 5, but among the K stars it is at least a factor of 20. We argue that this convergence, as well as the large number of slow rotators at 1.0 M. suggests that the convective envelopes and radiative cores of these Pleiads are rotationally decoupled, with later replenishment of angular momentum to the envelope. The Pleiades also shows a broad range in the strength of chromospheric emission (CE) at any one color. CE depends on both mass and rotation, but, once the rotation is normalized to an index akin to the Rossby number, rotation and activity are well correlated. Most G and K dwarfs in the Pleiades show Halpha and the infrared triplet in absorption, with filling in of the line cores. Some stars show overt Halpha emission comparable in strength and profile to the weaker T Tauri stars, and a few even show overt emission at the infrared triplet. We have also found three G dwarfs with peculiar Halpha profiles whose rotation rates substantially exceed those seen previously in the Pleiades among stars of their color. These stars show very broad wings to their Halpha emission profiles, suggesting that the emission arises over a broad range of height in the stars' atmospheres. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV CALIF SANTA CRUZ,BOARD STUDIES ASTRON & ASTROPHYS,LICK OBSERV,SANTA CRUZ,CA 95064. RP SODERBLOM, DR (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 152 TC 203 Z9 203 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 1993 VL 85 IS 2 BP 315 EP 346 DI 10.1086/191767 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU132 UT WOS:A1993KU13200005 ER PT J AU EMLEN, ST AF EMLEN, ST TI ETHICS AND EXPERIMENTATION - HARD CHOICES FOR THE FIELD ORNITHOLOGIST SO AUK LA English DT Note ID LANGURS PRESBYTIS-ENTELLUS; JACANA JACANA-SPINOSA; INFANTICIDE; ANIMALS; RAJASTHAN C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP EMLEN, ST (reprint author), CORNELL UNIV,NEUROBIOL & BEHAV SECT,ITHACA,NY 14853, USA. NR 21 TC 10 Z9 10 U1 1 U2 5 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 SN 0004-8038 J9 AUK JI AUK PD APR PY 1993 VL 110 IS 2 BP 406 EP 409 PG 4 WC Ornithology SC Zoology GA MC017 UT WOS:A1993MC01700031 ER PT J AU WASSER, SK NORTON, G AF WASSER, SK NORTON, G TI BABOONS ADJUST SECONDARY SEX-RATIO IN RESPONSE TO PREDICTORS OF SEX-SPECIFIC OFFSPRING SURVIVAL SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article ID MIKUMI-NATIONAL-PARK; LOCAL RESOURCE COMPETITION; PAPIO-CYNOCEPHALUS; MORTALITY; SELECTION; TANZANIA AB Most theories of sex ratio adjustment assume that parents will adjust the sex ratio of births (secondary sex ratio) in a manner that maximizes offspring reproductive success (as long as this does not jeopardize parental reproductive success). Survival to maturity is typically the largest component of variance in offspring reproductive success. This should make environmental predictors of sex-specific offspring survival strong predictors of secondary sex ratio adjustment. We tested this survivorship maximization hypothesis for secondary sex ratio adjustment using data from a 17-year demographic study of 315 yellow baboon infants at Mikumi National Park, Tanzania. Sex differences were found in the degree to which several social and ecological conditions affected infant survival to 1 year. Female, but not male, infant survival was inversely correlated with birth order and the proportion of infant females in their birth cohort. Male, but not female, infant survival was inversely correlated with the amount of rainfall early in the year (January) and the proportion of infant males in their birth cohort; male survival also was positively correlated with maternal dominance rank. The consistency and timing of these effects across years suggested that such information was, in fact, available to females around the time of conception. Most importantly, social and ecological conditions that predicted improved survivorship of a given sex also were positively correlated with production of that sex. Early births were female-biased; and low January rainfall was correlated with a male-biased sex ratio, becoming increasingly female-biased as January rainfall increased. However, no sex ratio effects were correlated with maternal rank. Data supported the hypothesis that females adjusted secondary sex ratio in a manner that maximized sex-specific infant survival. This hypothesis also offered a plausible explanation for some of the contradictory data that have arisen from studies of maternal rank effects on sex ratio both within and between species. C1 SMITHSONIAN INST,RES CTR,FRONT ROYAL,VA 22630. UNIV CAMBRIDGE,DEPT ZOOL,CAMBRIDGE,ENGLAND. RP WASSER, SK (reprint author), SMITHSONIAN INST,DEPT ANIM HLTH & CONSERVAT,NATL ZOOL PK,FRONT ROYAL,VA 22630, USA. NR 30 TC 37 Z9 38 U1 2 U2 11 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD APR PY 1993 VL 32 IS 4 BP 273 EP 281 PG 9 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA KX458 UT WOS:A1993KX45800007 ER PT J AU STRONG, MT AF STRONG, MT TI 2 OVERLOOKED SPECIES OF BULBOSTYLIS (CYPERACEAE) FROM SOUTH-AMERICA SO BRITTONIA LA English DT Article DE CLASSIFICATION; CYPERACEAE; SOUTH-AMERICA; BULBOSTYLIS AB New species combinations are made in Bulbostylis, B. schomburgkiana and B. truncata from South America. A description, illustration, SEM photo of the fruit (achene), and comparison to related taxa are provided for each species. RP STRONG, MT (reprint author), SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 SN 0007-196X J9 BRITTONIA JI Brittonia PD APR-JUN PY 1993 VL 45 IS 2 BP 162 EP 168 DI 10.2307/2807501 PG 7 WC Plant Sciences SC Plant Sciences GA LD955 UT WOS:A1993LD95500008 ER PT J AU DORR, LJ BARRIE, FR AF DORR, LJ BARRIE, FR TI TYPIFICATION OF THE LINNAEAN NAMES IN PYROLA (ERICACEAE, PYROLOIDEAE) SO BRITTONIA LA English DT Article DE ERICACEAE; PYROLOIDEAE; PYROLA; CHIMAPHILA; MONESES; ORTHILIA; LINNAEUS AB Lectotypes are designated for four of the six Linnaean names in Pyrola. The names are applied now to species of Chimaphila, Moneses, Orthilia, and Pyrola (Ericaceae, Pyroloideae). C1 SMITHSONIAN INST,DEPT BOT,WASHINGTON,DC 20560. NR 0 TC 1 Z9 1 U1 0 U2 1 PU NEW YORK BOTANICAL GARDEN PI BRONX PA PUBLICATIONS DEPT, BRONX, NY 10458 SN 0007-196X J9 BRITTONIA JI Brittonia PD APR-JUN PY 1993 VL 45 IS 2 BP 177 EP 180 DI 10.2307/2807504 PG 4 WC Plant Sciences SC Plant Sciences GA LD955 UT WOS:A1993LD95500011 ER PT J AU RYAN, MJ RAND, AS AF RYAN, MJ RAND, AS TI SPECIES RECOGNITION AND SEXUAL SELECTION AS A UNITARY PROBLEM IN ANIMAL COMMUNICATION SO EVOLUTION LA English DT Article DE FEMALE CHOICE; MATE RECOGNITION; MATING PREFERENCES; PHYSAELAEMUS-PUSTULOSUS; SEXUAL SELECTION; SPECIES RECOGNITION ID FEMALE MATE CHOICE; PHYSALAEMUS-PUSTULOSUS; SENSORY EXPLOITATION; MATING PREFERENCES; FROG; ORTHOPTERA; EVOLUTION; TETTIGONIIDAE; TREEFROGS; HYLIDAE AB We investigated patterns of mating call preference and mating call recognition by examining phonotaxis of female tungara frogs, Physalaemus pustulosus, in response to conspecific and heterospecific calls. There are four results: females always prefer conspecific calls; most heterospecific calls do not elicit phonotaxis; some heterospecific calls do elicit phonotaxis and thus are effective mate recognition signals; and females prefer conspecific calls to which a component of a heterospecific call has been added to a normal conspecific call. We use these data to illustrate how concepts of species recognition and sexual selection can be understood in a unitary framework by comparing the distribution of signal traits to female preference functions. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP RYAN, MJ (reprint author), UNIV TEXAS,DEPT ZOOL,AUSTIN,TX 78712, USA. NR 39 TC 322 Z9 332 U1 4 U2 70 PU SOC STUDY EVOLUTION PI LAWRENCE PA 810 E 10TH STREET, LAWRENCE, KS 66044 SN 0014-3820 J9 EVOLUTION JI Evolution PD APR PY 1993 VL 47 IS 2 BP 647 EP 657 DI 10.2307/2410076 PG 11 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA KZ712 UT WOS:A1993KZ71200021 ER PT J AU DRUCKER, S COOKSY, AL KLEMPERER, W AF DRUCKER, S COOKSY, AL KLEMPERER, W TI SPECTROSCOPIC CHARACTERIZATION OF THE LOWEST PI AND SIGMA BENDING STATES OF ARHCN SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID INFRARED-LASER SPECTROSCOPY; AR-HCL; VANDERWAALS MOLECULE; STARK SPECTROSCOPY; ELECTRIC-RESONANCE; VIBRATIONAL-STATES; SUPERSONIC JET; SPECTRUM; MICROWAVE; DYNAMICS AB The lowest excited bending states, SIGMA1 and PI1, of the ArHCN complex have been measured by millimeter-wave electric resonance optothermal spectroscopy. The principal molecular constants determined for the SIGMA1 state are v0 = 164 890.790(12) MHz; B = 1958-8571(37) MHz; D = -0.075 23(29) MHz; eq(aa)Q = 0.825(27) MHz; and mu(a) = -0.521(30) D. For the PI1 state, the constants are nu0 = 181 984.4126(47) MHz; B = 2031.3624(17) MHz; D = 0.153 35(16) MHz; eq(aa)Q = 0.904(11) MHz; and mu(a) = 0.273 02(63) D. The leading SIGMA1-PI1 coupling constants are the Coriolis coefficient beta0 = 1016.998 (13) MHz and the transition dipole moment mu(b) = 2.2535(57) D. The rotational constants for the two bending states indicate that the average separation between the argon and the HCN center of mass contracts by roughly 0.5 angstrom compared to the linear ground state. This is consistent with the nearly T-shaped average geometry for each state established by analysis of the dipole moments and quadrupole coupling constants. Agreement between this work and prior theory confirms attribution of the anomalous distortion and isotope effects in the ground state to extreme angular-radial coupling. The relative sign of the dipole moments for the SIGMA1 and PI1 states is resolved in this work, allowing an unambiguous interpretation of the angular information. Assuming Laguerre angular distributions, we obtain that the SIGMA1 state wave function has a maximum at an angle of 108-degrees with a halfwidth of 49-degrees, and that the PI1 state maximum is at 80-degrees with a halfwidth of 37-degrees. This estimate for the SIGMA1 state angular distribution indicates that although the state is not antilinear (ArNCH), as was expected, it does approach this configuration. The PI1 state is nearly a free rotor eigenstate, showing that the angular part of the potential surface near 90-degrees is extremely flat. The combined data from the ground, PI1, and PI1 states reflect virtually the entire angular coordinate along the radial minimum of the potential, and should provide a reliable benchmark for ab initio potential energy surfaces for ArHCN near the bottom of the well. We compare the data to predictions from available C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP DRUCKER, S (reprint author), HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138, USA. NR 56 TC 34 Z9 34 U1 1 U2 4 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD APR 1 PY 1993 VL 98 IS 7 BP 5158 EP 5183 DI 10.1063/1.464918 PG 26 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA KV997 UT WOS:A1993KV99700004 ER PT J AU MONTALI, RJ SCANGA, CA PERNIKOFF, D WESSNER, DR WARD, R HOLMES, KV AF MONTALI, RJ SCANGA, CA PERNIKOFF, D WESSNER, DR WARD, R HOLMES, KV TI A COMMON-SOURCE OUTBREAK OF CALLITRICHID HEPATITIS IN CAPTIVE TAMARINS AND MARMOSETS SO JOURNAL OF INFECTIOUS DISEASES LA English DT Note AB Callitrichid hepatitis (CH) is a highly fatal, emerging arenavirus disease of captive South American marmosets and tamarins (Callitrichidae), including the endangered golden lion tamarin. A common-source outbreak of CH in golden lion tamarins and pygmy marmosets at a US zoo resulted from a single feeding of the primates with newborn mice inapparently infected with lymphocytic choriomeningitis virus (LCMV). Isolates from livers of mice and primates were related to isolates from previous CH outbreaks and to laboratory strains of LCMV by serology and nucleic acid hybridization, and 2 surviving animals developed antibody to other LCMV(CH) isolates and to laboratory strains of LCMV. Thus, LCMV, an arenavirus prevalent in wild mice in the US, can cause sporadic fatal hepatic disease in primates. Exposure of humans to wild or laboratory mice or to marmosets and tamarins that are infected with wild-type strains of LCMV poses the danger of serious disease. C1 UNIFORMED SERV UNIV HLTH SCI,BETHESDA,MD 20814. FT WORTH ZOOL PK,ANIM HLTH SECK,FT WORTH,TX. RP MONTALI, RJ (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT PATHOL,WASHINGTON,DC 20008, USA. FU NIAID NIH HHS [AI-27203] NR 15 TC 26 Z9 27 U1 0 U2 5 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0022-1899 J9 J INFECT DIS JI J. Infect. Dis. PD APR PY 1993 VL 167 IS 4 BP 946 EP 950 PG 5 WC Immunology; Infectious Diseases; Microbiology SC Immunology; Infectious Diseases; Microbiology GA KU086 UT WOS:A1993KU08600023 PM 8450260 ER PT J AU FLINT, OS MASTELLER, EC AF FLINT, OS MASTELLER, EC TI EMERGENCE COMPOSITION AND PHENOLOGY OF TRICHOPTERA FROM A TROPICAL RAIN-FOREST STREAM AT EL-VERDE, PUERTO-RICO SO JOURNAL OF THE KANSAS ENTOMOLOGICAL SOCIETY LA English DT Article ID CADDISFLIES AB An emergence trap operated over a small mountain stream in Puerto Rico collected 2561 specimens of Trichoptera in a 12 month period. Sixteen species were collected, with a single species, Cariboptila orophila, comprising 78.2% of the emergence. Females made up 5 8% of the catch, although this varied somewhat depending on the taxon. There was a pronounced minimum in the emergence pattern in June and July with a secondary drop in November. The average annual rainfall pattern offers no clear correlation with emergence, but the November drop might have been correlated with a sharp peak in rainfall in October of 1990. There does seem to be some seasonality in flight periods of some species, but the more abundant species were present year round. C1 PENN STATE UNIV,BEHREND COLL,ERIE,PA 16563. RP FLINT, OS (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,WASHINGTON,DC 20560, USA. NR 10 TC 7 Z9 7 U1 0 U2 0 PU KANSAS ENTOMOLOGICAL SOC PI LAWRENCE PA PO BOX 368, LAWRENCE, KS 66044 SN 0022-8567 J9 J KANSAS ENTOMOL SOC JI J. Kans. Entomol. Soc. PD APR PY 1993 VL 66 IS 2 BP 140 EP 150 PG 11 WC Entomology SC Entomology GA MF538 UT WOS:A1993MF53800002 ER PT J AU MONFORT, SL SCHWARTZ, CC WASSER, SK AF MONFORT, SL SCHWARTZ, CC WASSER, SK TI MONITORING REPRODUCTION IN CAPTIVE MOOSE USING URINARY AND FECAL STEROID METABOLITES SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Article ID WHITE-TAILED DEER; OVARIAN-FUNCTION; EXCRETED STEROIDS; PREGNANCY; PROGESTERONE; PLASMA AB Because repeated capture, restraint, and blood sampling generally are impractical strategies for monitoring reproductive status in wildlife species, noninvasive methods for tracking reproductive activity have become increasingly important. Thus, we used radioimmunoassay (RIA) of urinary pregnanediol-3alpha-glucuronide (PdG), estrogen conjugates, and fecal progesterone and estradiol to assess estrous cycles and pregnancy in captive moose (Alces alces). Using urinary PdG, we identified distinct reproductive cycles that began during October, and estrus behavior that coincided with nadirs in PdG excretion. Although PdG increased up to 5-fold over cycling levels during pregnancy, concentrations were variable making pregnancy diagnosis equivocal using this method. Estrogen conjugates were not useful for monitoring estrous cyclicity; however, during the final month of gestation urinary estrogen conjugate levels increased from <5 ng/mg creatinine (Cr) to >50 ng/mg Cr making this a useful method for definitive late pregnancy detection. To establish a simple pregnancy test, we evaluated estradiol and progesterone in feces (1-6 samples/individual) collected over a 2-year interval from 16 moose of various age, gender, and physiological (pregnant vs. nonpregnant) classifications. Using fecal progesterone and blind tests, technicians correctly identified pregnancy status in 22 of 26 (85%) cases with 3 false positive and 1 equivocal diagnosis; fecal estradiol proved less effective (15/26) (58%) for accurately diagnosing pregnancy. These methods provide the potential to monitor reproductive activity in both captive and free-living moose. C1 SMITHSONIAN INST,NATL ZOOL PK,CONSERVAT & RES CTR,FRONT ROYAL,VA 22630. ALASKA DEPT FISH & GAME,MOOSE RES CTR,SOLDOTNA,AK 99669. RP MONFORT, SL (reprint author), SMITHSONIAN INST,NATL ZOOL PK,DEPT ANIM HLTH,FRONT ROYAL,VA 22630, USA. NR 17 TC 40 Z9 45 U1 3 U2 13 PU WILDLIFE SOC PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814-2197 SN 0022-541X J9 J WILDLIFE MANAGE JI J. Wildl. Manage. PD APR PY 1993 VL 57 IS 2 BP 400 EP 407 DI 10.2307/3809440 PG 8 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA LA012 UT WOS:A1993LA01200027 ER PT J AU ROBERTSON, DR SCHOBER, UM BRAWN, JD AF ROBERTSON, DR SCHOBER, UM BRAWN, JD TI COMPARATIVE VARIATION IN SPAWNING OUTPUT AND JUVENILE RECRUITMENT OF SOME CARIBBEAN REEF FISHES SO MARINE ECOLOGY PROGRESS SERIES LA English DT Article ID GREAT-BARRIER-REEF; PHYTOPLANKTON PRODUCTION; CORAL REEFS; MARINE FISH; MORTALITY; POPULATIONS; LARVAE; DAMSELFISH; STRATEGIES; SETTLEMENT AB It is generally accepted that the intensity of recruitment of pelagic young of temperate marine fishes is determined primarily by events that affect young as larvae, and that pelagic processes substantially increase variation in recruitment over the level expected from variation in spawning output alone. Spawning and recruitment of 6 species of Caribbean damselfishes were monitored monthly at a site in Panama for 1 to 3 yr (1983 to 1987) and 7 to 10 yr (1980 to 1989), respectively. Intermensual variation in recruitment strength exceeded corresponding variation in spawning output by average factors of at least 1.5 to 3.0 (and perhaps as much as 4 to 20) among those species. Serial changes in seasonally-adjusted monthly spawning output and 'resultant' recruitment strength were not correlated in any species. Thus, regardless of whether or not local populations are self-recruiting, pelagic processes evidently do largely control, and substantially enhance, short-term variability in recruitment strength in these fishes. Interannual variation in recruitment was low in all but one species, in which it also exceeded variation in spawning. Thus control of variation in recruitment strength by short-term pelagic processes had little or no net effect on interannual variation in recruitment in most cases. Interspecific differences in recruitment seasonality and in levels of variation in mensual and annual recruitment strength (but not mensual and annual spawning output) indicate that pelagic processes affect recruitment of some of these closely related species to different degrees and in different temporal patterns. RP SMITHSONIAN TROP RES INST, UNIT 0948, BALBOA, PANAMA. NR 49 TC 43 Z9 43 U1 0 U2 7 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0171-8630 EI 1616-1599 J9 MAR ECOL PROG SER JI Mar. Ecol.-Prog. Ser. PD APR PY 1993 VL 94 IS 2 BP 105 EP 113 DI 10.3354/meps094105 PG 9 WC Ecology; Marine & Freshwater Biology; Oceanography SC Environmental Sciences & Ecology; Marine & Freshwater Biology; Oceanography GA LB331 UT WOS:A1993LB33100001 ER PT J AU LOIZEAU, JL STANLEY, DJ AF LOIZEAU, JL STANLEY, DJ TI PETROLOGICAL STATISTICAL APPROACH TO INTERPRET RECENT AND SUBRECENT LAGOON SUBFACIES, IDKU, NILE DELTA OF EGYPT SO MARINE GEOLOGY LA English DT Article ID QUATERNARY STRATIGRAPHY; HOLOCENE SEQUENCES; EVOLUTION; SEDIMENTOLOGY; DEPOSITS; HARBOR; SYSTEM AB An approach combining petrology and statistics (cluster analysis) is developed to better distinguish a series of subfacies in surficial and short core samples from Idku lagoon in the northwestern Nile delta, Egypt. The method integrates lithology, physical and biogenic structures, grain size, and composition of the sand-size fraction. Seven lithofacies, eight grain-size types and six clusters reveal comparable geographic distributions that are a direct response to geomorphic setting and depositional processes, both of which have been modified by man. Although positioned in an arid setting and affected by anthropogenic factors (land reclamation, pollutants), regional subfacies distribution patterns in Idku lagoon are largely a function of the spatial configuration of freshwater-dominated to brackish to higher salinity-dominated (near inlet) zones typical of lagoons receiving significant freshwater input. Within Idku, a northern depositional province near the inlet and along the coastal sand barrier is defined by associations of terrigenous and coarse-grained sediment types. A southern province, bounded by lagoon margins and marshes, is characterized by finer-grained sediment types, with a high biogenic content, recording lower energy levels. The petrological-statistical approach is used to identify and interpret lagoon subfacies in older (to > 6000 years B.P.) core sections in ldku region and in former Abu Qir lagoon. Additionally, cluster analysis serves to determine specific lagoon subfacies from hand samples alone, whether from surface grabs or cores; this is based on a comparison of lithofacies and clusters determined for surficial and short core samples in the ldku region. To test the method, a separate cluster analysis, also using surficial and short core samples, was used to define Manzala lagoon subfacies in the northeastern Nile delta. Results are generally comparable to those obtained in the ldku study, and show a close relation among Manzala lagoon subfacies, geomorphic configuration and depositional processes. The petrological-statistical method could be applied to other regions, and also to the geological record. C1 UNIV GENEVA,INST F A FOREL,CH-1290 VERSOIX,SWITZERLAND. SMITHSONIAN INST,MEDITERRANEAN BASIN PROGRAM,WASHINGTON,DC 20560. OI Loizeau, Jean-Luc/0000-0002-0611-0388 NR 66 TC 16 Z9 16 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0025-3227 J9 MAR GEOL JI Mar. Geol. PD APR PY 1993 VL 111 IS 1-2 BP 55 EP 81 DI 10.1016/0025-3227(93)90188-2 PG 27 WC Geosciences, Multidisciplinary; Oceanography SC Geology; Oceanography GA LB416 UT WOS:A1993LB41600005 ER PT J AU EVERETT, RA RUIZ, GM AF EVERETT, RA RUIZ, GM TI COARSE WOODY DEBRIS AS A REFUGE FROM PREDATION IN AQUATIC COMMUNITIES - AN EXPERIMENTAL TEST SO OECOLOGIA LA English DT Review DE COARSE WOODY DEBRIS; HABITAT STRUCTURE; PALAEMONETES; REFUGE; RISK OF PREDATION ID SALMON ONCORHYNCHUS-KISUTCH; JUVENILE BROWN SHRIMP; PENAEUS-AZTECUS IVES; GRASS SHRIMP; HABITAT USE; PALAEMONETES-PUGIO; FISH PREDATION; PREY RELATIONSHIPS; SEAGRASS MEADOWS; MANGROVE FORESTS AB This study demonstrates experimentally that coarse woody debris (CWD) can provide refuge from predation in aquatic habitats. In the Rhode River subestuary of Chesapeake Bay, Maryland, (USA), we (1) measured the abundance of CWD, (2) examined the utilization of CWD by mobile epibenthic fish and crustaceans, and (3) tested experimentally the value of CWD as a refuge from predation. CWD was the dominant above-bottom physical structure in shallow water, ranging in size from small branches (< 2 cm diameter) to fallen trees (> 50 cm diameter). In response to experimental additions of CWD, densities of common epibenthic species (Callinectes sapidus, Fundulus heteroclitus, Fundulus majalis, Gobiosoma bosc, Gobiesox strumosus, Palaemonetes pugio, and Rithropanopeus harrisii) increased significantly compared to control sites without CWD. In laboratory experiments, grass shrimp (P. pugio) responded to predatory fish (F. heteroclitus and Micropogonias undulatus) by utilizing shelter at CWD more frequently than in the absence of fish. Access to CWD increased survivorship of grass shrimp in laboratory and field experiments. These experimental results (1) support the hypothesis, commonly proposed but untested for freshwater habitats, that CWD can provide a refuge from predation for epibenthic fish and invertebrates and (2) extend the recognized functional importance of CWD in freshwater to estuarine and marine communities. We hypothesize that CWD is an especially important refuge habitat in the many estuarine and freshwater systems for which alternative physical structure (e.g., vegetation or oyster reefs) are absent or in low abundance. RP EVERETT, RA (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGWATER,MD 21037, USA. OI Ruiz, Gregory/0000-0003-2499-441X NR 126 TC 149 Z9 157 U1 4 U2 44 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD APR PY 1993 VL 93 IS 4 BP 475 EP 486 DI 10.1007/BF00328954 PG 12 WC Ecology SC Environmental Sciences & Ecology GA KW414 UT WOS:A1993KW41400003 PM 28313814 ER PT J AU SADEGHPOUR, HR DALGARNO, A AF SADEGHPOUR, HR DALGARNO, A TI DOUBLE PHOTOIONIZATION OF MOLECULAR-HYDROGEN SO PHYSICAL REVIEW A LA English DT Note ID HELIUM AB The cross section for two-electron photoionization of the hydrogen molecule by high-energy photons is predicted in the nonrelativistic dipole approximation to be 2.25% of the cross section for single photoionization. RP SADEGHPOUR, HR (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 20 TC 17 Z9 17 U1 0 U2 6 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD APR PY 1993 VL 47 IS 4 BP R2458 EP R2459 PN A PG 2 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA KW308 UT WOS:A1993KW30800010 ER PT J AU BERMINGHAM, E LESSIOS, HA AF BERMINGHAM, E LESSIOS, HA TI RATE VARIATION OF PROTEIN AND MITOCHONDRIAL-DNA EVOLUTION AS REVEALED BY SEA-URCHINS SEPARATED BY THE ISTHMUS OF PANAMA SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE SPECIATION; MOLECULAR EVOLUTION; MOLECULAR CLOCK; ISOZYMES; POPULATION GENETICS ID MOLECULAR CLOCK; BIOCHEMICAL EVOLUTION; SYSTEMATICS; PACIFIC; AMERICAN; ORIGIN AB Acceptance of the rough constancy of rates of molecular evolution, averaged over tens of millions of years, is widely used to date the splitting between taxa. However, for the study of speciation a hypothesis of rough constancy over tens of millions of years is of little use. In order to date the splitting of congeneric species within defined ranges of uncertainty, we need to know the variation of evolutionary rates over shorter periods of time. Such estimates of uncertainty are particularly useful if they apply to techniques of molecular comparisons that lend themselves to the assessment of intraspecific variation. We have measured protein divergence by electrophoresis and mitochondrial DNA differentiation by restriction fragment length polymorphism analysis in three pairs of sea urchin species believed to have resulted from the simultaneous fragmentation of ranges of marine species by the emergence of the Isthmus of Panama, about 3 million years ago. Transisthmian isozyme divergence in these pairs varies by an order of magnitude; mitochondrial DNA divergence, on the other hand, is equivalent in all pairs, suggesting that this molecule, assayed by endonucleases, can provide fairly accurate estimates of times since separation in the 3-million-year range. C1 SMITHSONIAN TROP RES INST,BALBOA,PORTUGAL. NR 33 TC 107 Z9 109 U1 2 U2 6 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 1 PY 1993 VL 90 IS 7 BP 2734 EP 2738 DI 10.1073/pnas.90.7.2734 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA KV975 UT WOS:A1993KV97500038 PM 8096641 ER PT J AU TORRES, G MAZEH, T LATHAM, DW STEFANIK, RP AF TORRES, G MAZEH, T LATHAM, DW STEFANIK, RP TI THE SEMIREGULAR VARIABLE FS COMAE - EVIDENCE FOR RADIAL OSCILLATIONS SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID STARS AB We present newly obtained radial-velocity measurements of the semiregular variable FS Comae, together with available photoelectric data and visual brightness estimates. Both the light variations in the V band and the radial velocities show a similar periodicity of about 55 days, with a phase lag of approximately 40 days between the two. These observations strongly suggest radial pulsation as the mechanism driving the variations. There is evidence that both the photometric period and the spectroscopic period are variable over long time scales. C1 TEL AVIV UNIV,SACKLER FAC EXACT SCI,SCH PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. RP TORRES, G (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 27 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD APR PY 1993 VL 105 IS 686 BP 360 EP 366 DI 10.1086/133162 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KY948 UT WOS:A1993KY94800005 ER PT J AU RODRIGUEZ, LF MARTI, J CANTO, J MORAN, JM CURIEL, S AF RODRIGUEZ, LF MARTI, J CANTO, J MORAN, JM CURIEL, S TI POSSIBLE RADIO SPECTRAL INDEXES FROM INHOMOGENEOUS FREE-FREE SOURCES SO REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA LA English DT Article DE H-II REGIONS; RADIATION MECHANISM; RADIATIVE TRANSFER ID CIRCUMSTELLAR DISKS; ENVELOPES AB Radio sources with large negative indices (alpha < -0.1, where the spectral index alpha is defined by S(nu) is-proportional-to nu(alpha)) have been found in regions of star formation. In this paper, we explore whether these spectral indices could be obtained from sources of free-free emission with ad hoc electron density and temperature distributions. We find that, if only free-free emission and absorption are involved, the spectral index will always be alpha greater-than-or-equal-to -0.1 regardless of the source characteristics. Finally, we explore the possibility that the large negative spectral indices could be produced by dust absorption. However, the very high column densities required lead us to conclude that the large negative indices found in these peculiar sources are more naturally explained in terms of optically thin synchrotron emission. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV BARCELONA,DEPT ASTRON & METEOROL,E-08028 BARCELONA,SPAIN. RP RODRIGUEZ, LF (reprint author), NATL AUTONOMOUS UNIV MEXICO,INST ASTRON,APARTADO POSTAL 70-264,MEXICO CITY 04510,DF,MEXICO. NR 16 TC 28 Z9 28 U1 0 U2 0 PU UNIV NACIONAL AUTONOMA MEXICO, INST DE ASTRONOMIA PI MEXICO CITY PA APDO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 0185-1101 J9 REV MEX ASTRON ASTR JI Rev. Mex. Astron. Astrofis. PD APR PY 1993 VL 25 IS 1 BP 23 EP 29 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA LC907 UT WOS:A1993LC90700003 ER PT J AU NEUFELD, MJ AF NEUFELD, MJ TI A NATION OF FLIERS - GERMAN AVIATION AND THE POPULAR IMAGINATION - FRITZSCHE,P SO TECHNOLOGY AND CULTURE LA English DT Book Review RP NEUFELD, MJ (reprint author), SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,DEPT AERONAUT,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD APR PY 1993 VL 34 IS 2 BP 440 EP 441 DI 10.2307/3106562 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA LH981 UT WOS:A1993LH98100028 ER PT J AU KIRBY, KP AF KIRBY, KP TI ELECTRON-SPIN EFFECTS IN ASTROCHEMISTRY SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 28 PY 1993 VL 205 BP 2 EP PHYS PN 2 PG 0 WC Chemistry, Multidisciplinary SC Chemistry GA KQ983 UT WOS:A1993KQ98300608 ER PT J AU MECKLENBURG, MF TUMOSA, CS AF MECKLENBURG, MF TUMOSA, CS TI COMPUTER MODELING OF THE EFFECTS OF TEMPERATURE AND RELATIVE-HUMIDITY ON STRESSES IN THE LAYERS OF CULTURAL MATERIALS SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract C1 SMITHSONIAN INST,CAL,MSC,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 SN 0065-7727 J9 ABSTR PAP AM CHEM S JI Abstr. Pap. Am. Chem. Soc. PD MAR 28 PY 1993 VL 205 BP 124 EP PMSE PN 2 PG 0 WC Chemistry, Multidisciplinary SC Chemistry GA KQ983 UT WOS:A1993KQ98301465 ER PT J AU ANDRE, P WARDTHOMPSON, D BARSONY, M AF ANDRE, P WARDTHOMPSON, D BARSONY, M TI SUBMILLIMETER CONTINUUM OBSERVATIONS OF RHO OPHIUCHI-A - THE CANDIDATE PROTOSTAR VLA-1623 AND PRESTELLAR CLUMPS SO ASTROPHYSICAL JOURNAL LA English DT Review DE ISM, INDIVIDUAL (VLA 1623); ISM, JETS AND OUTFLOWS; RADIO CONTINUUM, STARS; STARS, INDIVIDUAL (RHO OPHIUCHI-A); STARS, PRE-MAIN-SEQUENCE ID FAR-INFRARED OBSERVATIONS; YOUNG STELLAR OBJECTS; CO LINE FORMATION; DENSE CORES; DARK-CLOUD; CIRCUMSTELLAR DISKS; STAR FORMATION; MOLECULAR OUTFLOWS; IRAS OBSERVATIONS; EXCITING SOURCE AB We have mapped the submillimeter continuum emission from the rich star-forming core, rho Oph A, at 3.50, 450, 800, and 1300 mum using the JCMT and IRAM 30 m telescopes. In addition to the diffuse emission from the cloud core itself, these observations reveal four well-defined clumps, which, surprisingly, are barely visible in the single-dish molecular maps obtained so far in this region. The gas may have partially frozen out onto the dust grains, due to low temperature and/or high density in the clumps. We discuss the possibility that these clumps are prestellar or extremely young, low-mass protostars. One of them coincides with the (centimeter) radio source VLA 1623 which drives one of the youngest and best collimated CO bipolar flows known to date. Supplementing our JCMT measurements with stringent upper limits obtained at all four IRAS bands by maximum entropy deconvolution of the raw IRAS data, we show that VLA 1623 is a highly obscured (A(V) greater than or similar to 1000) young stellar object (YSO) with a remarkably low bolometric luminosity (L(bol) less than or similar to 1 L.) and dust temperature (T(d) less than or similar to 20 K). Its spectral energy distribution is well fitted by a single modified blackbody from dust at 15-20 K with an opacity index beta = 1.5. This indicates a mass of circumstellar material M(C) approximately 0.6 M. and a bolometric luminosity L(bol) approximately 1 L.. Our submillimeter observations resolve a nearly spherical dust envelope around VLA 1623, of FWHM size almost-equal-to 2000 AU roughly independent of wavelength. This suggests that the bulk of the circumstellar mass of VLA 1623 is distributed in an '' apple-like '' structure rather than a disk. Detailed, spherical modeling of this dust structure, using the radiative transfer code of Wolfire & Cassinelli, shows the spectral energy distribution and submillimeter intensity profiles of VLA 1623 can be fitted simultaneously by a 1 L. internal source surrounded by a circumstellar envelope with a surprisingly shallow density distribution [rho(r) is-proportional-to r-0.5]. The remarkably cold temperature, high internal obscuration, and relatively massive circumstellar structure of VLA 1623 all point to an extremely young object, perhaps a true protostar. We compare VLA 1623 with a few other very young embedded sources similarly characterized by very low values of the ratio L(bol)/L(submm), and suggest that these objects define an entirely new class of YSOs, which we call ''Class 0'' to indicate their extreme youth. Although these strong submillimeter YSOs are invisible in the near- and mid-IR, they are already powering highly collimated outflows (opening angles < 30-degrees) with great efficiency (L(flow)/L(bol) up to approximately 50%). This may indicate that the outflow phenomenon starts earlier than previously thought in (proto)stellar evolution, i.e., prior to the near-IR Class I phase as in the scheme devised by Lada. C1 CTR ETUD SACLAY,SERV ASTROPHYS,F-91191 GIF SUR YVETTE,FRANCE. MULLARD RADIO ASTRON OBSERV,CAVENDISH LAB,CAMBRIDGE CB3 0HE,ENGLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP ANDRE, P (reprint author), NATL RADIO ASTRON OBSERV,949 N CHERRY AVE,TUCSON,AZ 85721, USA. NR 104 TC 846 Z9 849 U1 1 U2 9 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 1993 VL 406 IS 1 BP 122 EP 141 DI 10.1086/172425 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KT453 UT WOS:A1993KT45300014 ER PT J AU FONTENLA, JM AVRETT, EH LOESER, R AF FONTENLA, JM AVRETT, EH LOESER, R TI ENERGY-BALANCE IN THE SOLAR TRANSITION REGION .3. HELIUM EMISSION IN HYDROSTATIC, CONSTANT-ABUNDANCE MODELS WITH DIFFUSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE DIFFUSION; LINE, FORMATION; SUN, TRANSITION REGION; SUN, UV RADIATION ID THERMAL CONDUCTION; QUIET SUN; CHROMOSPHERE; DISTRIBUTIONS; EQUATIONS; CORONA AB In our previous papers we described the mathematical formalism and the computed results for energy-balance hydrostatic models of the solar transition region. This region, characterized by a steep temperature gradient, is the interface between hot coronal material at 10(6) K and much cooler chromospheric material having temperatures at or below 10(4) K, and forms a narrow emission rim observed at the solar limb. In our model calculations we balance the radiative losses from the transition region with the total energy downflow at each depth in the atmosphere. The models include a detailed treatment of particle diffusion (in this case described by the ambipolar diffusion velocity), including the resulting departures from local ionization equilibrium and the transport of ionization energy. Our previous calculations of the hydrogen spectra agree reasonably well with the observed Lyalpha and Lybeta line intensities and profiles and account for the observed spatial variations of these lines. In this paper we discuss in some detail the limitations of the hydrostatic and one-dimensional assumptions used. Then we analyze the determination of helium emission when diffusion is included. We use transport coefficients estimated from kinetic theory to determine the helium departures from local ionization balance. We calculate the helium spectra for each of our models (A, C, F, and P) and evaluate the role of helium in the energy transport. Also, we investigate the effects of coronal illumination on the structure of the transition region and upper chromosphere, and show how coronal illumination affects various EUV lines and the He I 10830 angstrom line. Comparing with both absolute intensities and detailed line profiles, we show that our models are consistent not only with the observed hydrogen spectra but also with the available helium spectra. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP UNIV ALABAMA, HUNTSVILLE, AL 35899 USA. NR 40 TC 436 Z9 440 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAR 20 PY 1993 VL 406 IS 1 BP 319 EP 345 DI 10.1086/172443 PN 1 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KT453 UT WOS:A1993KT45300032 ER PT J AU YOSHINO, K ESMOND, JR FREEMAN, DE PARKINSON, WH AF YOSHINO, K ESMOND, JR FREEMAN, DE PARKINSON, WH TI MEASUREMENTS OF ABSOLUTE ABSORPTION CROSS-SECTIONS OF OZONE IN THE 185-NM TO 254-NM WAVELENGTH REGION AND THE TEMPERATURE-DEPENDENCE SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID HERZBERG CONTINUUM; 205-240 NM; OXYGEN; SPECTROMETER AB Laboratory measurements of the relative absorption cross sections of ozone at temperatures 195, 228 and 295 K have been made throughout the 185 to 254 nm wavelength region. The absolute absorption am sections at the same temperatures have been measured at several discrete wavelengths in the 185 to 250 nm region. The absolute cross sections of ozone have been used to put the relative cross sections on a firm absolute basis throughout the 185 to 255 nm region. These recalibrated cross sections are slightly lower than those of L. T. Molina and M.J. Molina (Journal of Geophysical Research 91, 1450, 1986), but the differences are within a few percent and would not be significant in atmospheric applications. RP YOSHINO, K (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GRADEN ST,CAMBRIDGE,MA 02138, USA. NR 18 TC 36 Z9 36 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD MAR 20 PY 1993 VL 98 IS D3 BP 5205 EP 5211 DI 10.1029/93JD00028 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA KU069 UT WOS:A1993KU06900028 ER PT J AU KOCHANEK, CS AF KOCHANEK, CS TI ANALYTIC RESULTS FOR THE GRAVITATIONAL LENS STATISTICS OF SINGULAR ISOTHERMAL SPHERES IN GENERAL COSMOLOGIES SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE COSMOLOGY-OBSERVATIONS; COSMOLOGY-THEORY; GRAVITATIONAL LENSING; RADIO CONTINUUM-GALAXIES ID ELLIPTICAL POTENTIAL WELLS; GALAXIES; DISTRIBUTIONS; CONSTANT; LIMITS AB The natural cosmological distance for the analysis of gravitational lens statistics with a singular isothermal sphere model for the lens potential is the proper motion distance. By using the proper motion distance we derive analytic expressions for the cross-sections, averages of the image separations, and averages of the distances to the lens for both point-like and resolved sources that depend only on the total density of the cosmological model and the proper motion distance to the source. The ratio of the square of the mean image separation to the mean square image separation for the lenses in a survey is a robust measure of survey completeness. The test shows that the sample of lenses in the Snapshot lens survey of bright quasars is complete within the limits of statistical errors, while the sample of lenses in the MIT-Greenbank radio survey for gravitational lenses is only 50 per cent complete. In a complete sample, the mean and mean square image separations can be used to estimate the velocity dispersion scale of galaxies. The Snapshot survey sample shows that the velocity dispersion scale of L* galaxies is in the range 240 km s-1 less than or similar sigma* less than or similar 310 km s- 1 and the uncertainty is comparable to the uncertainties from dynamical studies. The probability of lensing extended radio sources discriminates more strongly between low-density universes and the Einstein-de Sitter model than does the probability of lensing unresolved sources such as quasars. RP KOCHANEK, CS (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,DEPT ASTRON MS-51,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 34 TC 33 Z9 34 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAR 15 PY 1993 VL 261 IS 2 BP 453 EP 463 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KR176 UT WOS:A1993KR17600023 ER PT J AU MORGAN, JD KUTZELNIGG, W AF MORGAN, JD KUTZELNIGG, W TI HUND RULES, THE ALTERNATING RULE, AND SYMMETRY HOLES SO JOURNAL OF PHYSICAL CHEMISTRY LA English DT Article ID SINGLET; ENERGY AB We review attempts to explain Hund's first rule, that a triplet state should lie below a singlet state of the same configuration, as a consequence of the ''Fermi hole' in the triplet state electron-electron distribution function. After describing the failure of such attempts, and reviewing the types of exceptions to Hund's first rule, we examine the ''alternating rule'', which accounts for most of the known exceptions. We show that the alternating rule is associated with whether the parity of the two-electron wave function is natural or unnatural. We show that whereas in the case of natural parity the triplet correlation function has a broad Fermi hole and the singlet correlation function does not, in the case of unnatural parity the singlet correlation function has a quartic ''symmetry hole'' that i:s even broader than the quadratic Fermi hole of the triplet correlation function. Thus this more general perspective provides a relationship between the ordering of singlet/triplet energy levels and the breadth of their respective symmetry holes. We argue that although the breadth of symmetry holes cannot be said to cause the ordering of singlet/triplet energy levels, both phenomena are consequences of factors of (-1)S+L+l1+l2 in the construction of the properly antisymmetrized eigenfunctions of spin and angular variables; hence the two phenomena are closely associated, although neither is the cause of the other. C1 HARVARD UNIV,DEPT CHEM,CAMBRIDGE,MA 02138. RUHR UNIV BOCHUM,LEHRSTUHL THEORET CHEM,W-4630 BOCHUM,GERMANY. UNIV DELAWARE,DEPT PHYS & ASTRON,NEWARK,DE 19716. RP MORGAN, JD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 45 TC 36 Z9 36 U1 0 U2 7 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 SN 0022-3654 J9 J PHYS CHEM-US JI J. Phys. Chem. PD MAR 11 PY 1993 VL 97 IS 10 BP 2425 EP 2434 DI 10.1021/j100112a051 PG 10 WC Chemistry, Physical SC Chemistry GA KT155 UT WOS:A1993KT15500051 ER PT J AU GOMEZ, DO MARTENS, PCH GOLUB, L AF GOMEZ, DO MARTENS, PCH GOLUB, L TI NORMAL INCIDENCE X-RAY TELESCOPE POWER SPECTRA OF X-RAY-EMISSION FROM SOLAR ACTIVE REGIONS .1. OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; SUN, ACTIVITY; TURBULENCE ID CORONA; FIELDS AB We use the very high resolution images of coronal active regions obtained by the Normal Incidence X-Ray Telescope to search for features of magnetohydrodynamic (MHD) fluctuations. By Fourier analyzing these images we find a broad-band, isotropic, power-law spectrum for the spatial distribution of soft X-ray intensities. The presence of a broad-band spectrum indicates that magnetic structures of all sizes are present, at least down to the resolution limit of the instrument, which is approximately 0''75. From a sample of topologically different active regions, we obtain power spectra for their X-ray intensities which falls off with increasing wavenumber as k-3. C1 LOCKHEED PALO ALTO RES LABS,SOLAR & ASTROPHYS LAB 9130252,PALO ALTO,CA 94304. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP GOMEZ, DO (reprint author), UNIV HAWAII,INST ASTRON,2680 WOODLAWN DR,HONOLULU,HI 96822, USA. OI Gomez, Daniel/0000-0002-4935-4358 NR 20 TC 23 Z9 23 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 1993 VL 405 IS 2 BP 767 EP & DI 10.1086/172405 PN 1 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KP612 UT WOS:A1993KP61200034 ER PT J AU GOMEZ, DO MARTENS, PCH GOLUB, L AF GOMEZ, DO MARTENS, PCH GOLUB, L TI NORMAL INCIDENCE X-RAY TELESCOPE POWER SPECTRA OF X-RAY-EMISSION FROM SOLAR ACTIVE REGIONS .2. THEORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; SUN, ACTIVITY; TURBULENCE ID DIMENSIONAL MAGNETOHYDRODYNAMIC TURBULENCE; CORONAL LOOPS; MAGNETIC-FIELDS; DISSIPATION AB In a previous paper, we used the very high resolution images of coronal active regions obtained by the Normal Incidence X-Ray Telescope to study the size distribution of X-ray-emitting structures. A Fourier analysis of these images showed a broad-band, isotropic, power-law spectrum for the spatial distribution of soft X-ray intensities. The presence of a broad-band spectrum indicates that magnetic structures of all sizes are present, at least down to the resolution limit of the instrument, which is about 3/4''. In the present paper, we present a model that relates the basic features of coronal magnetic fluctuations to the subphotospheric hydrodynamic turbulence that generates them. The main result of this paper is that from this model we obtain a theoretical power spectrum for the X-ray intensity, which falls off with increasing wavenumber as k-3, fitting remarkably well the observed spectra that we obtained from a sample of topologically different active regions. We speculate that the nonlinear interactions of these externally driven fluctuations will contribute to establish a magnetohydrodynamic turbulent regime in the corona. We suggest that the bulk of the energy delivered to the corona from footpoint motions directly cascades down to very microscopic length scales, where it efficiently dissipates and heats the plasma. However, since the wavenumber range associated with the cascade and dissipation regions are still beyond present-day spatial resolution limits, the presence of a turbulent regime cannot be observationally confirmed. C1 LOCKHEED PALO ALTO RES LABS,SOLAR & ASTROPHYS LAB 9130252,PALO ALTO,CA 94304. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP GOMEZ, DO (reprint author), UNIV HAWAII,INST ASTRON,2680 WOODLAWN DR,HONOLULU,HI 96822, USA. OI Gomez, Daniel/0000-0002-4935-4358; Golub, Leon/0000-0001-9638-3082 NR 44 TC 12 Z9 12 U1 0 U2 2 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 1993 VL 405 IS 2 BP 773 EP 781 DI 10.1086/172406 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KP612 UT WOS:A1993KP61200035 ER PT J AU KIMURA, M LANE, NF DALGARNO, A DIXSON, RG AF KIMURA, M LANE, NF DALGARNO, A DIXSON, RG TI RATE COEFFICIENTS FOR MOMENTUM-TRANSFER, CHARGE-TRANSFER, AND RADIATIVE ASSOCIATION PROCESSES IN COLLISIONS OF H+ WITH HE BELOW 10(5)K SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC PROCESSES; MOLECULAR PROCESSES ID ENERGIES AB The charge-transfer and momentum-transfer cross sections for protons in collisions with helium are calculated at relative energies up to 5 keV. Rate coefficients are presented for temperatures up to 10(5) K. Charge transfer is more rapid than radiative association at temperatures above 7500 K. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. YALE UNIV,DEPT PHYS,NEW HAVEN,CT 06520. NR 10 TC 23 Z9 23 U1 0 U2 3 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 10 PY 1993 VL 405 IS 2 BP 801 EP 802 DI 10.1086/172410 PN 1 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KP612 UT WOS:A1993KP61200039 ER PT J AU MITROVICA, JX PELTIER, WR AF MITROVICA, JX PELTIER, WR TI PRESENT-DAY SECULAR VARIATIONS IN THE ZONAL HARMONICS OF EARTHS GEOPOTENTIAL SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID DEEP MANTLE VISCOSITY; GLACIAL-ISOSTATIC-ADJUSTMENT; GLOBAL SEA-LEVEL; PLEISTOCENE DEGLACIATION; GRAVITY-FIELD; LAGEOS; CONSTRAINT; ROTATION; ACCELERATION; ANOMALIES AB We develop a new formalism for the prediction of secular variations in the gravitational potential field of a spherically symmetric, self-gravitating, (Maxwell) viscoelastic planetary model subjected to an arbitrary surface load which may include a gravitationally self-consistent ocean loading component. The theory is applied to generate the most accurate predictions to date, of the present-day secular variations in the zonal harmonics of the geopotential (the so-called J(l) for degree l) arising as a consequence of the late Pleistocene glacial cycles. In this respect, we use the very recent ICE-3G reconstruction of the last late Pleistocene deglaciation event (Tushingham and Peltier, 1991). A comparison of these predictions with those generated using simplified disk models of the ice sheets, which have been used in all previous studies of the J(l) harmonics (l > 2), indicates that the disk model approximation introduces unacceptably large errors at all spherical harmonic degrees except perhaps l = 2. Predictions have also been made using a eustatic loading approximation (also used in previous studies) in place of a gravitationally self-consistent ocean loading component, and we have found that the resulting discrepancy is largest at degrees 2, 8 and 10. In the case of J2, the magnitude of the error incurred using the eustatic approximation can be as large as order 10-15% of the predicted value. We have attributed this discrepancy to the present day net flux of water away from the equatorial regions arising from the remnant present-day adjustment associated with the late Pleistocene glacial cycles. The effect represents a heretofore unrecognized contribution to the J(l) harmonics, or alternatively the nontidal acceleration of Earth's axial rate of rotation. In terms of the latter, the maximum anomaly in the length of day is approximately 1.7 mus/yr. We also consider the sensitivity of the J(l) data to variations in the radial mantle viscosity profile by using a suite of forward calculations and an examination of Frechet kernels. The theory required for the computation of those kernels is described hemin. We find that the radial variation in sensitivity can be a strong function of the viscosity model used in the calculations. For models with a uniform upper mantle viscosity (v(UM)) of 10(21) Pa s, forward predictions of the J(l) harmonics exhibit a pronounced peak when a wide enough range of lower mantle viscosities (v(LM) are considered (we denote the v(LM) value at this peak as v(LM). At the lowest degrees (l less-than-or-equal-to 4), Frechet kernels computed for a series of increasing v(LM) values (10(21) Pa s less-than-or-equal-to v(LM) < 10(23) Pa s) indicate a migration of the dominant sensitivity of the J(l) data to variations in viscosity from regions below approximately 1200 km depth (for v(LM) less-than-or-equal-to v(LM)) to regions above this depth in the lower mantle (for v(LM) greater-than-or-equal-to v(LM)l). The sensitivity of the J(l) data to variations in the viscosity profile in the shallowest parts of the lower mantle, for the case v(LM) greater-than-or-equal-to v(LM)l is also reflected in a set of forward calculations described herein. As an example, J(l) predictions made using Earth models in which the viscosity above 1200 km depth is constrained to be 10(21) Pa s, do not exhibit the multiple solutions characteristic of the v(UM) = 10(21) Pa s calculations. The same is true of Earth models in which the upper mantle viscosity is weakened an order of magnitude to 10(20) Pa s. The theory described herein is also applied to compute the J(l) signal (l less-than-or-equal-to 10) arising from the retreat of small ice sheets and glaciers described by Meier (1984) and also from any potential variations in the mass of the Antarctic and Greenland ice sheets. The present day J(l) signal due to the late Pleistocene glacial cycles dominates the signal from Meier's sources at all degrees except l = 3. In contrast, the J(l) signal arising from mass variations in the Antarctic and Greenland ice sheets is potentially comparable to the former. A comparison of observational constraints on the J(l) data with predictions of the postglacial rebound signal described in this paper, in order to infer mantle rheology, cannot proceed until constraints are placed on the present-day mass flux of these large polar ice sheets. We show that the constraints required are weakest at degrees l = 2 and 4. Finally, we outline a potentially important procedure for incorporating predictions of the J(l) signal due to the late Pleistocene glacial cycles and Meier's sources, with an observational constraint on the J2 datum, to yield bounds on the present-day net mass flux from the Antarctic and Greenland ice sheets. A rigorous application of this procedure must wait until observational constraints on J2 are reestablished in the literature. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MITROVICA, JX (reprint author), UNIV TORONTO,DEPT PHYS,TORONTO M5S 1A7,ONTARIO,CANADA. RI Peltier, William/A-1102-2008 NR 51 TC 67 Z9 70 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD MAR 10 PY 1993 VL 98 IS B3 BP 4509 EP 4526 DI 10.1029/92JB02700 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA KQ873 UT WOS:A1993KQ87300031 ER PT J AU HERRE, EA AF HERRE, EA TI POPULATION-STRUCTURE AND THE EVOLUTION OF VIRULENCE IN NEMATODE PARASITES OF FIG WASPS SO SCIENCE LA English DT Article ID COEVOLUTION; SELECTION AB It is often assumed that parasitic and disease-producing organisms tend to evolve benign relationships with their hosts over time. In contrast, theoretical arguments suggest that increased opportunities for parasite transmission will promote the evolution of increased virulence. The natural history of species-specific nematodes that parasitize fig-pollinating wasps permits the testing of these predictions in natural populations. For 11 species of Panamanian fig wasps, those species characterized by population structures that result in increased opportunities for parasite transmission harbor more virulent species of nematodes. In addition, differences in population structure are also associated with differences in other intra- and interspecific phenomena, including sex ratios among the fig wasp species, the degree of tension in the wasp-fig mutualism, and lethal combat among the males of parasitic wasps. RP HERRE, EA (reprint author), SMITHSONIAN TROP RES INST,APARTADO 2072,BALBOA,PANAMA. NR 25 TC 275 Z9 280 U1 6 U2 104 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAR 5 PY 1993 VL 259 IS 5100 BP 1442 EP 1445 DI 10.1126/science.259.5100.1442 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA KP978 UT WOS:A1993KP97800033 PM 17801279 ER PT J AU MCCORRISTON, J AF MCCORRISTON, J TI THE ORIGINS OF AGRICULTURE - AN INTERNATIONAL PERSPECTIVE - COWAN,CW, WATSON,PJ SO SCIENCE LA English DT Book Review RP MCCORRISTON, J (reprint author), SMITHSONIAN INST,DEPT ANTHROPOL,WASHINGTON,DC 20560, USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD MAR 5 PY 1993 VL 259 IS 5100 BP 1473 EP 1474 DI 10.1126/science.259.5100.1473 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA KP978 UT WOS:A1993KP97800046 PM 17801283 ER PT J AU LO, KY BACKER, DC KELLERMANN, KI REID, M ZHAO, JH GOSS, WM MORAN, JM AF LO, KY BACKER, DC KELLERMANN, KI REID, M ZHAO, JH GOSS, WM MORAN, JM TI HIGH-RESOLUTION VLBA IMAGING OF THE RADIO-SOURCE SGR-A-ASTERISK AT THE GALACTIC-CENTER SO NATURE LA English DT Article AB THE compact non-thermal radio source at the Galactic Centre, known as Sgr A*, may mark the location of a massive black hole1,2. Here we present images of Sgr A* with milliaresecond resolution obtained by using five telescopes of the partially completed Very Long Baseline Array (VLBA) in conjunction with a few additional telescopes. The image of Sgr A* at a wavelength of 3.6 cm confirms almost exactly the elliptical gaussian model that has been proposed on the basis of previous, more sparse data3,4. The source size at 1.35 cm wavelength is 2.4 +/- 0.2 mas, similar to previous results3,5. At both wavelengths, the radio source is smooth, without detectable fine structure. These observations, along with other recent results6, support the suggestion7 that the radio emission from Sgr A* is strongly scattered by electron-density fluctuations along the line of sight. On the assumption8 that the emission is due to a black hole accreting stellar winds from massive stars in the central 0.5 pc, the observations are consistent with a black-hole mass of less than or similar to 2 x 10(6) M.. C1 UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. NATL RADIO ASTRON OBSERV,CHARLOTTESVILLE,VA 22903. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NATL RADIO ASTRON OBSERV,SOCORRO,NM 87801. RP LO, KY (reprint author), UNIV ILLINOIS,DEPT ASTRON,1002 W GREEN ST,URBANA,IL 61801, USA. NR 28 TC 32 Z9 33 U1 2 U2 2 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD MAR 4 PY 1993 VL 362 IS 6415 BP 38 EP 40 DI 10.1038/362038a0 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA KP976 UT WOS:A1993KP97600051 ER PT J AU MERRILL, WL AF MERRILL, WL TI HALF OF THE WORLD - BODY AND COSMOS IN OTOMI RITUALS - SPANISH - GALINIER,J SO AMERICAN ANTHROPOLOGIST LA English DT Book Review RP MERRILL, WL (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER ANTHROPOLOGICAL ASSOC PI ARLINGTON PA 4350 NORTH FAIRFAX DRIVE SUITE 640, ARLINGTON, VA 22203 SN 0002-7294 J9 AM ANTHROPOL JI Am. Anthropol. PD MAR PY 1993 VL 95 IS 1 BP 224 EP 224 DI 10.1525/aa.1993.95.1.02a00810 PG 1 WC Anthropology SC Anthropology GA KU108 UT WOS:A1993KU10800081 ER PT J AU DILLENBURG, LR WHIGHAM, DF TERAMURA, AH FORSETH, IN AF DILLENBURG, LR WHIGHAM, DF TERAMURA, AH FORSETH, IN TI EFFECTS OF VINE COMPETITION ON AVAILABILITY OF LIGHT, WATER, AND NITROGEN TO A TREE HOST (LIQUIDAMBAR-STYRACIFLUA) SO AMERICAN JOURNAL OF BOTANY LA English DT Article ID NUTRIENT AVAILABILITY; ROOT COMPETITION; GROWTH; PINE AB Competitive effects of vines on their tree hosts are well documented, but the mechanisms involved in these interactions are poorly understood. The objectives of this study were to measure the effects of below- and/or aboveground competition from the vines Lonicera japonica and Parthenocissus quinquefolia on availability of light, water, and nitrogen to the host tree Liquidambar styraciflua, and to examine the relationship between resource availability and tree growth. Light penetration through tree canopies, pre-dawn leaf water potential, and leaf nitrogen concentration were used as predictors of light, water, and nitrogen availability to the tree, respectively. Vine presence significantly reduced light penetration through the tree canopies, but this reduction was not clearly related to the growth responses of trees. Vines did not reduce the pre-dawn leaf water potential of competing trees, which was consistently above -0.5 MPa for the duration of the study. Leaf nitrogen concentration of trees, on the other hand, was significantly reduced by belowground competition with L. japonica. The positive correlation between the annual average leaf nitrogen concentration and tree diameter growth suggested that competition for nitrogen mediated the effects of belowground competition of vines on tree growth. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. UNIV MARYLAND,DEPT BOT,COLL PK,MD 20742. RI Rebello Dillenburg, Lucia /D-9120-2013; OI Whigham, Dennis/0000-0003-1488-820X NR 48 TC 52 Z9 55 U1 3 U2 17 PU BOTANICAL SOC AMER INC PI COLUMBUS PA OHIO STATE UNIV-DEPT BOTANY 1735 NEIL AVE, COLUMBUS, OH 43210 SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD MAR PY 1993 VL 80 IS 3 BP 244 EP 252 DI 10.2307/2445347 PG 9 WC Plant Sciences SC Plant Sciences GA KT073 UT WOS:A1993KT07300002 ER PT J AU HORTON, JO AF HORTON, JO TI THE ADVENTURES OF AMOS-N-ANDY, A SOCIAL-HISTORY OF AN AMERICAN PHENOMENON - ELY,MP SO AMERICAN QUARTERLY LA English DT Book Review C1 SMITHSONIAN INST,WASHINGTON,DC 20560. RP HORTON, JO (reprint author), GEORGE WASHINGTON UNIV,WASHINGTON,DC 20052, USA. NR 1 TC 1 Z9 1 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4319 SN 0003-0678 J9 AM QUART JI Am. Q. PD MAR PY 1993 VL 45 IS 1 BP 166 EP 170 DI 10.2307/2713058 PG 5 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA KR808 UT WOS:A1993KR80800008 ER PT J AU BEDINI, SA AF BEDINI, SA TI FROM PLEASURE AND PROFIT TO SCIENCE AND SECURITY - LENOIR,ETIENNE AND THE TRANSFORMATION OF PRECISION INSTRUMENT-MAKING IN FRANCE 1760-1830 - TURNER,AJ SO ANNALS OF SCIENCE LA English DT Book Review RP BEDINI, SA (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU TAYLOR & FRANCIS LTD PI LONDON PA ONE GUNDPOWDER SQUARE, LONDON, ENGLAND EC4A 3DE SN 0003-3790 J9 ANN SCI JI Ann. Sci. PD MAR PY 1993 VL 50 IS 2 BP 198 EP 199 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA KM743 UT WOS:A1993KM74300017 ER PT J AU HARRIS, DE STERN, CP WILLIS, AG DEWDNEY, PE AF HARRIS, DE STERN, CP WILLIS, AG DEWDNEY, PE TI THE MEGAPARSEC RADIO RELIC IN SUPERCLUSTER, ROOD NUMBER 27 SO ASTRONOMICAL JOURNAL LA English DT Article ID MAGNETIC-FIELD; COMA CLUSTER; GALAXY; HALO AB New observations have been obtained of the extended source of low surface brightness adjacent to three Abell clusters of galaxies of Rood Group #27. Although this source was originally classified as a radio halo associated with a poor group of galaxies, it now appears that it is a ''relic'' of a currently inactive radio galaxy. If the source is at the same distance (z = 0.125) as the three Abell clusters and the two galaxies near the source center, the largest dimension is approximately 1.6 Mpc (H0 = 50 km/s/Mpc). We provide new evidence that the spectrum is not a simple power law. Below a few hundred MHz alpha greater-than-or-equal-to 1.0, but there is a flatter component between 300 and 1400 MHz where alpha approximately 0.6 (S(nu) = k(s)nu(-alpha)). The fractional polarization is high, and the magnetic field direction appears to be coherent over scales of at least several hundred kpc. A comparison of this source, other relics, and the Coma radio halo indicates that the energetics of all these sources are similar, but the polarization and morphologies of relics are distinct from those of cluster halos. We ascribe the differences to the different environment provided by the core of a cluster compared to that encountered in the outer fringes of the hot gas distribution which produces the characteristic x-ray emission. C1 DOMINION RADIO ASTROPHYS OBSERV,PENTICTON V2A 6K3,BC,CANADA. RP HARRIS, DE (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 16 TC 32 Z9 32 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 1993 VL 105 IS 3 BP 769 EP 777 DI 10.1086/116470 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KQ553 UT WOS:A1993KQ55300001 ER PT J AU FABRICANT, D KURTZ, M GELLER, M ZABLUDOFF, A MACK, P WEGNER, G AF FABRICANT, D KURTZ, M GELLER, M ZABLUDOFF, A MACK, P WEGNER, G TI A STUDY OF THE RICH CLUSTER OF GALAXIES A119 SO ASTRONOMICAL JOURNAL LA English DT Article ID X-RAY; VELOCITY DISPERSIONS; REDSHIFTS AB We use Einstein Observatory x-ray images, galaxy photometry, and galaxy redshifts to study the cluster of galaxies Abell 119. We report 60 new radial velocities, as well as new photographic and CCD photometry. We find corresponding evidence for substructure in the projected galaxy distribution and the x-ray surface brightness profile. A multiple clump model, in which galaxies trace the condensations in the dark matter, reproduces the main features of the photometric and x-ray data. The galaxy velocity histogram of A119 is Gaussian (with the exception of a superposed foreground group), but the velocity data do not sample the subclumps adequately. C1 MICHIGAN DARTMOUTH MIT OBSERV, TUCSON, AZ 85735 USA. DARTMOUTH COLL, HANOVER, NH 03755 USA. RP FABRICANT, D (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. OI Kurtz, Michael/0000-0002-6949-0090 NR 29 TC 31 Z9 31 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 1993 VL 105 IS 3 BP 788 EP 796 DI 10.1086/116472 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KQ553 UT WOS:A1993KQ55300003 ER PT J AU BERNSTEIN, GM TYSON, JA KOCHANEK, CS AF BERNSTEIN, GM TYSON, JA KOCHANEK, CS TI A LARGE ARC IN THE GRAVITATIONAL LENS SYSTEM 0957+561 SO ASTRONOMICAL JOURNAL LA English DT Article ID DEEP CCD SURVEY; HUBBLE CONSTANT; QUASAR 0957+561; DARK MATTER; GALAXY; MODELS; CLUSTERS; IMAGES; Q0957+561 AB New R- and B(J) band images of the gravitational lens 0957 + 561 show a pair of elongated blue objects 20'' from the lens center; their morphology strongly suggests that they are distorted images of background galaxies, and as such they place new constraints on models of this lens system. The implications for the Hubble constant and for the mass distribution in the lens are investigated using a variety of parametric models. The models of Falco et al. [ApJ, 310, 568 (1991)] and of Kochanek [ApJ 382, 58 (1991)] cannot describe the observed arcs. Lenses consisting of an isothermal galaxy (G1) and softened-core isothermal cluster cannot form the arc for velocity dispersions comparable to those observed. Models in which the mass of the galaxy traces its light also fail without the addition of a third strong deflector. Galaxy mass profiles of nonisothermal power laws can produce the arc, but only if the lens is marginal, G1 has low mass, and therefore the implied value of H0 is below 32. Inclusion of a mass of order 10(14) M. at the location of the z = 0.5 group of galaxies in the field allows a new branch of solutions with higher galaxy masses, cluster masses consistent with the measured velocity dispersions, and values of H0 up to 68. The further addition of a constant shear to the lens model allows the Hubble constant to be as large as 87. These models satisfy all of the lensing constraints, agree with the locally determined distance scale, and have masses consistent with all existing dynamical estimates. Further observation of the system should differentiate between the low-H0 and high-H0 sets of solutions. Surface photometry of the outer portions of the lens galaxy G1 show that it is well fit by a deVaucouleurs profile with r(e) almost-equal-to 14h-1 kpc and m(R) almost-equal-to 17.0, and is a typical brightest cluster elliptical. If the high-H0 models are correct, then the galaxy mass profile is at least as steep as isothermal, perhaps as steep as mass traces light. C1 AT&T BELL LABS, MURRAY HILL, NJ 07974 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, DEPT ASTRON MS-51, CAMBRIDGE, MA 02138 USA. RP BERNSTEIN, GM (reprint author), UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85721 USA. NR 39 TC 38 Z9 38 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 1993 VL 105 IS 3 BP 816 EP 830 DI 10.1086/116474 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KQ553 UT WOS:A1993KQ55300005 ER PT J AU AANNESTAD, PA KENYON, SJ HAMMOND, GL SION, EM AF AANNESTAD, PA KENYON, SJ HAMMOND, GL SION, EM TI COOL METALLIC-LINE WHITE-DWARFS, RADIAL-VELOCITIES, AND INTERSTELLAR ACCRETION SO ASTRONOMICAL JOURNAL LA English DT Article ID STARS; ABUNDANCES; DIFFUSION; EVOLUTION; HYDROGEN; GRAINS; DA AB From observations of the spectra of 15 cool metallic-line white dwarfs we derive their radial velocities from the positions of the H and K lines of Ca II. A pressure shift correction is included, and the resulting mean gravitational redshift is 35 km/s. By projecting their spatial distribution and space velocity components onto and perpendicular to the galactic plane, and including 13 additional stars not observed by us, we compare the present and past spatial distribution of the white dwarfs with the distribution of local interstellar matter. If the metallic-line white dwarfs are accreting their metals from the interstellar medium, one would expect a spatial correlation between the stars and the local gas. However, we conclude that only very few of the stars could possibly just have accreted or presently be accreting metals from local clouds. We also consider several scenarios for interstellar accretion that may have taken place within the last million years, assuming that the local medium has not substantially changed. Our results show that Ca accretion from local interstellar matter in the past cannot have proceeded at a rate high enough to explain the observed photospheric abundances of Ca, at least in the cool metallic-line degenerates. The main factors in limiting the accretion rates are the lack of dense clouds in the local medium and low effective stellar temperatures that reduce the accretion rate much below the fluid rate. Alternatives to accretion from the local interstellar medium must be seriously considered. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV S FLORIDA, DEPT MATH, TAMPA, FL 33620 USA. VILLANOVA UNIV, DEPT ASTRON & ASTROPHYS, VILLANOVA, PA 19085 USA. RP AANNESTAD, PA (reprint author), ARIZONA STATE UNIV, DEPT PHYS & ASTRON, TEMPE, AZ 85287 USA. OI Kenyon, Scott/0000-0003-0214-609X NR 54 TC 62 Z9 62 U1 2 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAR PY 1993 VL 105 IS 3 BP 1033 EP 1044 DI 10.1086/116491 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KQ553 UT WOS:A1993KQ55300022 ER PT J AU CANIZARES, CR MARKERT, TH MARKOFF, S HUGHES, JP AF CANIZARES, CR MARKERT, TH MARKOFF, S HUGHES, JP TI THE INSIGNIFICANCE OF HEATING FLOWS IN COOLING FLOW CLUSTERS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE COOLING FLOWS; GALAXIES, CLUSTERING; INTERGALACTIC MEDIUM; X-RAYS, GALAXIES ID SUPER-NOVA REMNANTS; X-RAY-EMISSION; SPHERICAL CLOUDS; HOT GAS; IMAGING OBSERVATIONS; EVAPORATION; MODELS; CONDUCTION; BOUNDARY; NGC-4696 AB We consider the possibility that so-called ''cooling flow'' clusters are really ''heating flow'' clusters, in which cold gas clouds evaporate in the hot intracluster medium. Saturated evaporation is treated following the work of Cowie & McKee. We estimate the total X-ray luminosity to be approximately 2.2 x 10(38)(M(evap)/1 M. yr-1) ergs s-1, where M(evap) is the total evaporation rate. This is approximately 10,000 times smaller than the X-ray luminosity of material that is cooling at the same rate. We also compute the X-ray line emissivity for evaporating clouds. Because the time scale for an atom to move from the cold cloud to the hot surrounding medium is much shorter than the ionization time scale for ions of interest, our computation uses a nonequilibrium ionization code. Again, we find that the effective line emissivities of evaporating clouds are approximately 1000 times smaller than for cooling clouds. More specific comparisons are made using measured line fluxes for M87 and the Perseus cluster, for which we derive evaporation rates of approximately 10(4) and approximately 10(6) M. yr-1, respectively. We conclude that evaporative heating flow models require mass fluxes many orders of magnitude higher than cooling flow models to explain the same X-ray emission. This requirement greatly exceeds any plausible mass source by similar factors. We show that these conclusions are very general and serve to reject all heating flow models as viable alternatives to cooling flows. C1 MIT,CTR SPACE RES,CAMBRIDGE,MA 02139. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP CANIZARES, CR (reprint author), MIT,DEPT PHYS,ROOM 37-241,CAMBRIDGE,MA 02139, USA. NR 36 TC 7 Z9 7 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAR 1 PY 1993 VL 405 IS 1 BP L17 EP L20 DI 10.1086/186755 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KP298 UT WOS:A1993KP29800005 ER PT J AU MEYLAN, T FURENLID, I WIGGS, MS AF MEYLAN, T FURENLID, I WIGGS, MS TI A CRITICAL LIST OF VOIGT-FITTED EQUIVALENT WIDTH MEASUREMENTS BASED ON THE SOLAR FLUX SPECTRUM SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE SUN, ABUNDANCES; SUN, ATMOSPHERE; TECHNIQUES, SPECTROSCOPIC ID FE-I LINES; OSCILLATOR-STRENGTHS AB Equivalent widths of around 570 carefully selected absorption lines in the solar flux spectrum have been measured, using the Solar Flux Atlas from 296 to 1300 nm by Kurucz et al. The equivalent widths were derived from Voigt functions fitted to the selected line profiles in the Solar Flux Atlas. The measurements were used to determine two sets of solar log gf-values; one set is based on the solar model in the 1979 model grid by Kurucz and the other set on a similar 1990 solar model, also by Kurucz, using revised metal abundances by Anders and Grevesse. The data provide a homogeneous, high-precision reference for studies of differential stellar abundances based on equivalent widths, using the solar flux spectrum as the standard. C1 GEORGIA STATE UNIV,ATLANTA,GA 30303. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 19 TC 48 Z9 48 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAR PY 1993 VL 85 IS 1 BP 163 EP 180 DI 10.1086/191759 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KM956 UT WOS:A1993KM95600007 ER PT J AU KALFATOVIC, MR AF KALFATOVIC, MR TI AN ARTFUL LIFE - A BIOGRAPHY OF KAHNWEILER,D.H., 1884-1979 - ASSOULINE,P SO BIOGRAPHY-AN INTERDISCIPLINARY QUARTERLY LA English DT Book Review RP KALFATOVIC, MR (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 SN 0162-4962 J9 BIOGRAPHY JI Biography-Interdiscip. Q. PD SPR PY 1993 VL 16 IS 2 BP 173 EP 175 PG 3 WC Literature SC Literature GA LA816 UT WOS:A1993LA81600007 ER PT J AU WELDON, PJ FERGUSON, MWJ AF WELDON, PJ FERGUSON, MWJ TI CHEMORECEPTION IN CROCODILIANS - ANATOMY, NATURAL-HISTORY, AND EMPIRICAL RESULTS SO BRAIN BEHAVIOR AND EVOLUTION LA English DT Article; Proceedings Paper CT SATELLITE SYMP ON REPTILIAN CHEMICAL SENSES AND SIGNALS, AT THE MEETING ON THE CHEMICAL SIGNALS IN VERTEBRATES CY JUN 16-21, 1991 CL PHILADELPHIA, PA SP NICHHD DE CROCODILIA; OLFACTION; GUSTATION; FEEDING BEHAVIOR; PHEROMONES ID ALLIGATOR ALLIGATOR-MISSISSIPPIENSIS; PARACLOACAL GLAND SECRETIONS; THIN-LAYER CHROMATOGRAPHY AB Anatomical and behavioral aspects of chemoreception in crocodilians are reviewed. Extant crocodilians possess valvular nostrils regulated by smooth muscles; paired nasal cavities, each with three conchae; and flaps closing the rear of the buccopharyngeal passage to channel inspired air through the nasopharyngeal duct. Olfaction is enhanced by gular pumping, whereby the floor of the pharynx is alternately lowered and raised to pulse air through the nasal cavity. Taste buds occur on the tongue, palate, and pharyngeal walls. Crocodilians in nature or in semi-natural enclosures locate distant carrion or concealed meat, implying chemoattraction to food. The American alligator exhibits underwater head-waving and mouth-opening in response to aqueous and chloroform extracts of meat. Alligators increase gular pumping in response to the scents of various meats, indicating that they detect food chemicals by olfaction. Paired gular and paracloacal glands on the integument of crocodilians are thought to produce pheromones. Juvenile crocodilians exhibit heightened gular pumping in response to airborne skin gland secretions. Observations of adults suggest that gular and paracloacal glands produce chemical signals used in mating and/or nesting activities, but behavioral responses to skin gland exudates are too poorly documented to ascribe pheromonal properties. C1 TEXAS A&M UNIV SYST,DEPT BIOL,COLL STN,TX 77843. UNIV MANCHESTER,DEPT CELL & STRUCT BIOL,MANCHESTER M13 9PL,LANCS,ENGLAND. RP WELDON, PJ (reprint author), SMITHSONIAN INST,DEPT HERPETOL,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 41 TC 24 Z9 25 U1 3 U2 20 PU KARGER PI BASEL PA ALLSCHWILERSTRASSE 10, CH-4009 BASEL, SWITZERLAND SN 0006-8977 J9 BRAIN BEHAV EVOLUT JI Brain Behav. Evol. PD MAR-MAY PY 1993 VL 41 IS 3-5 BP 239 EP 245 DI 10.1159/000113845 PG 7 WC Behavioral Sciences; Neurosciences; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Zoology GA KX567 UT WOS:A1993KX56700018 PM 8477347 ER PT J AU SMITH, RW AF SMITH, RW TI MODERN COSMOLOGY IN RETROSPECT - BERTOTTI,B, BALBINOT,R, BERGIA,S, MESSINA,A SO BRITISH JOURNAL FOR THE HISTORY OF SCIENCE LA English DT Book Review RP SMITH, RW (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0007-0874 J9 BRIT J HIST SCI JI Br. J. Hist. Sci. PD MAR PY 1993 VL 26 IS 88 BP 124 EP 125 PN 1 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA KT396 UT WOS:A1993KT39600054 ER PT J AU KOLTES, KH AF KOLTES, KH TI ASPECTS OF THE REPRODUCTIVE-BIOLOGY AND SOCIAL-STRUCTURE OF THE STOPLIGHT PARROTFISH SPARISOMA-VIRIDE, AT GRAND TURK, TURKS-AND-CAICOS-ISLANDS, BWI SO BULLETIN OF MARINE SCIENCE LA English DT Article ID CROICENSIS BLOCH SCARIDAE; REEF FISHES; CORAL-REEF; SEX-CHANGE AB The reproductive biology and social structure of the protogynous stoplight parrotfish, Sparisoma viride, were investigated from 1985-1987 in shallow-water areas (< 10 m) at Grand Turk, Turks and Caicos Islands, B.W.I. Over 225 fish were speared, and size at maturation and sex reversal, number of eggs in ripe females, stage of sexual development and variation in reproductive condition were determined. Sex reversal occurred from 150 to 250 mm standard length (SL). Females matured between 170 and 270 mm SL, but ripe eggs were found only in females > 260 mm SL indicating a period of growth between maturation and reproduction. Gonadal indices for females > 260 mm SL varied among sites, with higher gonadal indices found al the more exposed sites. Egg counts among ripe females varied widely (5,543-68,606 eggs.female-1) and showed no relationship to size. Visual surveys indicated that abundance and sex ratio varied according to habitat, with males predominating in the lagoon and females off the ends of the island. Overall, stoplight parrotfish were more abundant off the ends of the island where reproductively active individuals appeared to congregate. Results indicate that S. viride at Grand Turk maintains some sort of haremic mating system. C1 SMITHSONIAN INST,MARINE SYST LAB,WASHINGTON,DC 20560. NR 34 TC 12 Z9 12 U1 2 U2 14 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 SN 0007-4977 J9 B MAR SCI JI Bull. Mar. Sci. PD MAR PY 1993 VL 52 IS 2 BP 792 EP 805 PG 14 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA LD105 UT WOS:A1993LD10500010 ER PT J AU WIEGMANN, BM MITTER, C THOMPSON, FC AF WIEGMANN, BM MITTER, C THOMPSON, FC TI EVOLUTIONARY ORIGIN OF THE CYCLORRHAPHA (DIPTERA) - TESTS OF ALTERNATIVE MORPHOLOGICAL HYPOTHESES SO CLADISTICS-THE INTERNATIONAL JOURNAL OF THE WILLI HENNIG SOCIETY LA English DT Article ID PERMUTATION TESTS; PHYLOGENY; CLADOGRAM; PHORIDAE; HOMOLOGY C1 SMITHSONIAN INST,USDA ARS,SYST ENTOMOL LAB,WASHINGTON,DC 20560. RP WIEGMANN, BM (reprint author), UNIV MARYLAND,DEPT ENTOMOL,COLL PK,MD 20742, USA. NR 90 TC 33 Z9 34 U1 0 U2 6 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0748-3007 J9 CLADISTICS JI Cladistics-Int. J. Willi Hennig Soc. PD MAR PY 1993 VL 9 IS 1 BP 41 EP 81 DI 10.1111/j.1096-0031.1993.tb00208.x PG 41 WC Evolutionary Biology SC Evolutionary Biology GA LW211 UT WOS:A1993LW21100002 ER PT J AU EBERHARD, WG AF EBERHARD, WG TI FUNCTIONAL-SIGNIFICANCE OF SOME SECONDARY SEXUAL CHARACTERS IN 3 SPECIES OF MACRODACTYLUS (COLEOPTERA, MELOLONTHIDAE) SO COLEOPTERISTS BULLETIN LA English DT Article AB Observations of courtship and copulation behavior suggest that secondary sexual modifications of the sculpturing of the front legs, the ventral bristles, and the overall leg length of male Macrodactylus may function as courtship devices prior to and during copulation. RP EBERHARD, WG (reprint author), SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 0 TC 3 Z9 3 U1 0 U2 0 PU COLEOPTERISTS SOC PI NATCHEZ PA P.O. BOX 767, NATCHEZ, MS 39121 SN 0010-065X J9 COLEOPTS BULL JI Coleopt. Bull. PD MAR PY 1993 VL 47 IS 1 BP 53 EP 60 PG 8 WC Entomology SC Entomology GA KW158 UT WOS:A1993KW15800013 ER PT J AU HUANG, LN AF HUANG, LN TI RACIALLY MIXED PEOPLE IN AMERICA - ROOT,MPP SO CONTEMPORARY PSYCHOLOGY LA English DT Book Review C1 AMER PSYCHOL ASSOC,MINOR FELLOWSHIP PROGRAM,WASHINGTON,DC. SMITHSONIAN INST,WASHINGTON,DC 20560. RP HUANG, LN (reprint author), AMERICAN UNIV,WASHINGTON,DC 20016, USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU AMER PSYCHOLOGICAL ASSOC PI WASHINGTON PA 750 FIRST ST NE, WASHINGTON, DC 20002-4242 SN 0010-7549 J9 CONTEMP PSYCHOL JI Comtemp. Psychol. PD MAR PY 1993 VL 38 IS 3 BP 306 EP 307 PG 2 WC Psychology, Multidisciplinary SC Psychology GA KQ916 UT WOS:A1993KQ91600053 ER PT J AU BUDD, AF MANN, KO GUZMAN, HM AF BUDD, AF MANN, KO GUZMAN, HM TI ENVIRONMENTAL INTERPRETATION USING INSOLUBLE RESIDUES WITHIN REEF CORAL SKELETONS - PROBLEMS, PITFALLS, AND PRELIMINARY-RESULTS SO CORAL REEFS LA English DT Article ID GROWTH; PATTERNS; FLORIDA; RATES AB Insoluble residue concentrations have been measured within colonies of four massive reef corals from seven localities along the Caribbean coast of Panama to determine if detrital sediments, incorporated within the skeletal lattice during growth, record changes in sedimentation over the past twenty years. Amounts of resuspended sediment have increased to varying degrees at the seven localities over the past decades in response to increased deforestation in nearby terrestrial habitats. Preliminary results of correlation and regression analyses reveal few consistent temporal trends in the insoluble residue concentration. Analyses of variance suggest that amounts of insoluble residues, however, differ among environments within species, but that no consistent pattern of variation exists among species. D. strigosa and P. astreoides possess high concentrations at protected localities, S. siderea at localities with high amounts of resuspended sediment, and M. annularis at the least turbid localities. Little correlation exists between insoluble residue concentration and growth band width within species at each locality. Only in two more efficient suspension feeders (S. siderea and D. strigosa) do weak negative correlations with growth band width exist overall. These results indicate that insoluble residue concentrations cannot be used unequivocally in environmental interpretation, until more is known about tissue damage, polyp behavior, and their effects on the incorporation of insolubles in the skeleton during growth in different coral species. Insoluble residue data are highly variable; therefore, large sample sizes and strong contrasts between environments are required to reveal significant trends. C1 JUNIATA COLL,DEPT GEOL,HUNTINGDON,PA 16652. SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP BUDD, AF (reprint author), UNIV IOWA,DEPT GEOL,IOWA CITY,IA 52242, USA. NR 24 TC 16 Z9 16 U1 1 U2 2 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD MAR PY 1993 VL 12 IS 1 BP 31 EP 42 DI 10.1007/BF00303782 PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA KX781 UT WOS:A1993KX78100004 ER PT J AU KAEPPLER, A AF KAEPPLER, A TI THE SPIRITED EARTH - DANCE, MYTH, AND RITUAL FROM SOUTH-ASIA TO THE SOUTH-PACIFIC - GINN,V SO DANCE RESEARCH JOURNAL LA English DT Book Review RP KAEPPLER, A (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CONGRESS RESEARCH DANCE (CORD) PI BROCKPORT PA NEW YORK STATE UNIV, DEPT DANCE, COLLEGE BROCKPORT, BROCKPORT, NY 14420 SN 0149-7677 J9 DANCE RES J JI Dance Res. J. PD SPR PY 1993 VL 25 IS 1 BP 41 EP 41 DI 10.2307/1478193 PG 1 WC Dance SC Dance GA LG190 UT WOS:A1993LG19000008 ER PT J AU COLEY, PD KURSAR, TA MACHADO, JL AF COLEY, PD KURSAR, TA MACHADO, JL TI COLONIZATION OF TROPICAL RAIN-FOREST LEAVES BY EPIPHYLLS - EFFECTS OF SITE AND HOST PLANT LEAF LIFETIME SO ECOLOGY LA English DT Note ID LIGHT ENVIRONMENTS; NITROGEN C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP COLEY, PD (reprint author), UNIV UTAH,DEPT BIOL,SALT LAKE CITY,UT 84112, USA. NR 33 TC 49 Z9 56 U1 0 U2 14 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE, NW, STE 400, WASHINGTON, DC 20036 SN 0012-9658 J9 ECOLOGY JI Ecology PD MAR PY 1993 VL 74 IS 2 BP 619 EP 623 DI 10.2307/1939322 PG 5 WC Ecology SC Environmental Sciences & Ecology GA KN556 UT WOS:A1993KN55600031 ER PT J AU LORNELL, K AF LORNELL, K TI THE EARLY MINSTREL SHOW + WINANS,R - NEW-WORLD-RECORDS-NW-338 SO ETHNOMUSICOLOGY LA English DT Record Review RP LORNELL, K (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC ETHNOMUSICOLOGY INC PI BLOOMINGTON PA MORRISON HALL, ROOM 005 INDIANA UNIVERSITY, BLOOMINGTON, IN 47405 SN 0014-1836 J9 ETHNOMUSICOLOGY JI Ethnomusicology PD SPR-SUM PY 1993 VL 37 IS 2 BP 302 EP 304 PG 3 WC Music SC Music GA LZ566 UT WOS:A1993LZ56600011 ER PT J AU WASSER, SK SEWALL, G SOULES, MR AF WASSER, SK SEWALL, G SOULES, MR TI PSYCHOSOCIAL STRESS AS A CAUSE OF INFERTILITY SO FERTILITY AND STERILITY LA English DT Note DE INFERTILITY; PSYCHOSOCIAL STRESS; ADAPTATION; REPRODUCTIVE FILTERING MODEL C1 UNIV WASHINGTON,SCH MED,DEPT OBSTET & GYNECOL,DIV RENAL TRANSPLANT,SEATTLE,WA 98195. RP WASSER, SK (reprint author), SMITHSONIAN INST,CONSERVAT & RES,ENDOCRINE RES LAB,1500 REMOUNT RD,FRONT ROYAL,VA 22630, USA. FU NICHD NIH HHS [R01HD18967-06] NR 4 TC 44 Z9 48 U1 1 U2 7 PU AMER SOC REPRODUCTIVE MEDICINE PI BIRMINGHAM PA 1209 MONTGOMERY HIGHWAY, BIRMINGHAM, AL 35216-2809 SN 0015-0282 J9 FERTIL STERIL JI Fertil. Steril. PD MAR PY 1993 VL 59 IS 3 BP 685 EP 689 PG 5 WC Obstetrics & Gynecology; Reproductive Biology SC Obstetrics & Gynecology; Reproductive Biology GA KQ171 UT WOS:A1993KQ17100038 PM 8458480 ER PT J AU PLATTNER, S ARONSON, G ABELLERA, B AF PLATTNER, S ARONSON, G ABELLERA, B TI RECENT TRENDS IN FUNDING ANTHROPOLOGICAL RESEARCH AT THE NATIONAL-SCIENCE-FOUNDATION SO HUMAN ORGANIZATION LA English DT Editorial Material DE FUNDING RESEARCH; NATIONAL-SCIENCE-FOUNDATION; PROPOSALS C1 SMITHSONIAN INST,REPATRIAT PROJECT,WASHINGTON,DC 20560. CATHOLIC UNIV AMER,WASHINGTON,DC 20064. RP PLATTNER, S (reprint author), NATL SCI FDN,WASHINGTON,DC 20550, USA. NR 12 TC 2 Z9 2 U1 0 U2 0 PU SOC APPLIED ANTHROPOLOGY PI OKLAHOMA CITY PA BUSINESS OFFICE BOX 24083, OKLAHOMA CITY, OK 73124 SN 0018-7259 J9 HUM ORGAN JI Hum. Organ. PD SPR PY 1993 VL 52 IS 1 BP 110 EP 114 PG 5 WC Anthropology; Social Sciences, Interdisciplinary SC Anthropology; Social Sciences - Other Topics GA KR474 UT WOS:A1993KR47400012 ER PT J AU ROBINSON, CA WOOD, JA AF ROBINSON, CA WOOD, JA TI RECENT VOLCANIC ACTIVITY ON VENUS - EVIDENCE FROM RADIOTHERMAL EMISSIVITY MEASUREMENTS SO ICARUS LA English DT Article ID RADAR REFLECTIVITY; SURFACE RP ROBINSON, CA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 22 TC 19 Z9 19 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD MAR PY 1993 VL 102 IS 1 BP 26 EP 39 DI 10.1006/icar.1993.1030 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KX515 UT WOS:A1993KX51500002 ER PT J AU ENGLAND, MN SCHMIDLIN, FJ JOHANSSON, JM AF ENGLAND, MN SCHMIDLIN, FJ JOHANSSON, JM TI ATMOSPHERIC MOISTURE MEASUREMENTS - A MICROWAVE RADIOMETER - RADIOSONDE COMPARISON SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article ID WATER-VAPOR; PATH-DELAY; LIQUID AB The NASA/Goddard Space Flight Center Crustal Dynamics Project microwave Water Vapor Radiometer (WVR-J03) is used to measure the thermal emission of the sky at three frequencies (20.7, 22.2, and 31.4 GHz). Measurements were taken during the Atmospheric Moisture Intercomparison Study (ATMIS) held at Wallops Island, VA during April 1989. These measurements were compared with brightness temperatures inferred from measurements from VAISALA radiosonde packages launched every 3 hours during the experiment period. An error analysis for the radiosonde-inferred brightness temperatures was performed assuming reasonable random uncertainties for the pressure, temperature, and humidity measurements and propagating these uncertainties through the analysis algorithm. For the assumed uncertainties (sigma(P) = sigma(T) = 0.84 K, and sigma(RH) = 5% RH) the dominant contribution to the total uncertainty comes from the temperature measurement (66% - 88%) whereas the relative humidity measurement contributes only 2% - 8%, except in the vicinity of the water vapor line, where the contribution is 10% - 20%. Sky brightness temperature random errors range from 0.03 K to 0.6 K, with systematic errors between 0.4 K and 1.8 K. Two different water vapor emission models were used for the derivation of the brightness temperatures from the radiosonde measurements. The Liebe model and VAISALA radiosonde data give better agreement with the WVR for the 20.7 and 22.2 GHz frequencies (mean differences [WVR - VAI] of -0.32 +/- 0.56 K and -0.22 +/- 0.77 K, respectively) than does the Waters model and VAISALA radiosonde data. Agreement is best at 31.4 GHz using the Waters model (mean difference [WVR - VAI] -0.28 +/- 0.5 K), although in all cases the differences are less than the estimated uncertainties on the radiosonde inferred brightness temperatures. Differences between the two models increase as the moisture content increases and vary as a function of frequency. C1 NASA,GODDARD SPACE FLIGHT CTR,HYDROSPHER PROC,WALLOPS ISL,VA 23337. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP ENGLAND, MN (reprint author), NASA,GODDARD SPACE FLIGHT CTR,OBSERV COMP SCI CORP,GREENBELT,MD 20771, USA. NR 30 TC 19 Z9 19 U1 0 U2 0 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017-2394 SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD MAR PY 1993 VL 31 IS 2 BP 389 EP 398 DI 10.1109/36.214915 PG 10 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA LD280 UT WOS:A1993LD28000007 ER PT J AU CHEN, ZY STANLEY, DJ AF CHEN, ZY STANLEY, DJ TI ALLUVIAL STIFF MUDS (LATE PLEISTOCENE) UNDERLYING THE LOWER NILE DELTA PLAIN, EGYPT - PETROLOGY, STRATIGRAPHY AND ORIGIN SO JOURNAL OF COASTAL RESEARCH LA English DT Article DE ALLUVIAL PLAIN; ALLUVIAL SANDS; COASTAL SEDIMENTS; DELTA DEPOSITS; DELTAIC FORMATION; NILE SHELF; STRATIGRAPHIC SEQUENCE ID LATE QUATERNARY STRATIGRAPHY; HEAVY MINERALS; GYPSUM NODULES; EVOLUTION; SUBSIDENCE; SEDIMENTS; HISTORY; FLOODS; FACIES; RATES AB Stiff muds of late Pleistocene age, interbedded with alluvial sands, are buried beneath Holocene deposits of the Nile delta in Egypt. The origin of the muds are interpreted on the basis of the petrology, stratigraphy and distribution of radiocarbon-dated sections recovered in cores across the northern delta. Four distinct stiff mud sequences, or subfacies, are defined on the basis of lithology, sand-sized composition and clay mineralogy. These sequences include (I) calcareous nodule-, (II) gypsum nodule-, (III) shell- and (IV) plant debris-bearing stiff muds. They accumulated: I, in seasonally flooded inland sebkhas proximal to Nile channels, which were then covered with wind-blow sand; II, in somewhat more central sectors of such playas, more distal to flood channels; III, in mom permanent salt lakes; and IV, in freshwater to low salinity marshes adjoining seasonally flooded playas. Sequence I, the dominant lithofacies, is concentrated in 14 geographically distinct lithosomes. Sequence II occurs at or near the center of these lithosomes, while III and IV are more localized. Spatial and temporal distribution of muds suggest a predominance of incised channels in the north-central Nile alluvial plain, and more laterally migrating channels to the northeast and northwest. Most stiff mud layers, deposited earlier than 34,000 and at approximately 28,000-22,000 and approximately 16,000- > 10,000 years BP, are correlated with several late Pleistocene aggradational phases of the Nile in upper Egypt. The more time-restricted gypsum nodule-bearing sequence II accumulated primarily during a period of increased aridity. Lower alluvial plain muds are also correlated with deposits of equivalent age offshore, on the Nile Cone. Paleogeographic reconstructions indicate that River Nile sediments bypassed the northwestern delta plain and were deposited on the Cone. Nile stiff mud facies, primarily sequences I and III, are compared with those of equivalent age in Yangtze and Mississippi delta cores. Gypsum-rich subfacies (sequence II) are regionally more restricted to warm, arid regions such as the Nile. We postulate that stiff muds underlie Holocene sections in all major delta plains, having accumulated at times of eustatic lowstands. Their petrology and distribution patterns are best explained in terms of depositional setting, fluvial sediment load and flood patterns, and especially, climate. The native and configuration of stiff muds has practical applications for civil engineering and construction purposes in deltaic settings, and also for hydrocarbon exploration. RP CHEN, ZY (reprint author), SMITHSONIAN INST,MEDITERRANEAN BASIN PROGRAM,E-207 NMNH,WASHINGTON,DC 20560, USA. NR 87 TC 19 Z9 26 U1 2 U2 4 PU COASTAL EDUCATION & RESEARCH FOUNDATION PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 SN 0749-0208 J9 J COASTAL RES JI J. Coast. Res. PD SPR PY 1993 VL 9 IS 2 BP 539 EP 576 PG 38 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA KW243 UT WOS:A1993KW24300017 ER PT J AU MANOLOPOULOS, DE JAMIESON, MJ PRADHAN, AD AF MANOLOPOULOS, DE JAMIESON, MJ PRADHAN, AD TI JOHNSON LOG DERIVATIVE ALGORITHM REDERIVED SO JOURNAL OF COMPUTATIONAL PHYSICS LA English DT Note ID MOLECULAR-SCATTERING THEORY; NUMERICAL-METHODS; BOUND-STATES C1 UNIV GLASGOW,DEPT COMP SCI,GLASGOW G12 8QQ,SCOTLAND. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MANOLOPOULOS, DE (reprint author), UNIV NOTTINGHAM,DEPT CHEM,NOTTINGHAM NG7 2RD,ENGLAND. NR 20 TC 27 Z9 27 U1 1 U2 5 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0021-9991 J9 J COMPUT PHYS JI J. Comput. Phys. PD MAR PY 1993 VL 105 IS 1 BP 169 EP 172 DI 10.1006/jcph.1993.1062 PG 4 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA KT822 UT WOS:A1993KT82200015 ER PT J AU HU, YQ HABBAL, SR AF HU, YQ HABBAL, SR TI DOUBLE SHOCK PAIRS IN THE SOLAR-WIND SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LARGE HELIOCENTRIC DISTANCES; CORONAL MASS EJECTIONS; SLOW SHOCKS; STREAMS; REVERSE; WAVES; MODEL AB This paper presents a numerical study of the evolution of a velocity enhancement disturbance in the solar wind in terms of a one-dimensional, isentropic MHD flow model. It is shown that the disturbance steepens and evolves into a double shock pair while propagating outward away from the Sun. The double shock pair consists of a reverse fast shock, a reverse slow shock, a forward slow shock, and a forward fast shock in order of distance away from the Sun. The formation time of the double shock pair is nearly inversely proportional to the average velocity gradient of the disturbance. When the double shock pair is fully developed, the strength of the fast shocks is essentially determined by the disturbance amplitude, while the slow shocks behave differently. Their strength increases first with the disturbance amplitude but starts to decrease once the disturbance amplitude exceeds a certain value. However, the fully developed slow shocks will retain their identity up to 1 AU and even farther, though their propagation speed in the solar wind frame and the jump in velocity and total pressure across them decrease substantially with heliocentric distance. Theoretically, double shock pairs would occur frequently in the inner heliosphere, since the solar wind there is characterized by various large-scale structures and disturbances, which provide an appropriate ground for the formation of double shock pairs. Such a prediction remains to be confirmed by observations and data interpretation. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138. NR 22 TC 7 Z9 19 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 SN 0148-0227 J9 J GEOPHYS RES JI J. Geophys. Res-Space Phys. PD MAR 1 PY 1993 VL 98 IS A3 BP 3551 EP 3561 DI 10.1029/92JA02567 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KP929 UT WOS:A1993KP92900008 ER PT J AU LEFEBVREBRION, H YOSHINO, K AF LEFEBVREBRION, H YOSHINO, K TI TENTATIVE INTERPRETATION OF THE RYDBERG SERIES CONVERGING TO THE A2-PI-U STATE OF N-2(+) SO JOURNAL OF MOLECULAR SPECTROSCOPY LA English DT Article ID HUND CASE E; ELECTRONIC AUTOIONIZATION; MOLECULAR NITROGEN; N2; ABSORPTION; SPECTRUM; PHOTOIONIZATION; THRESHOLD; SPECTROSCOPY; 1-PI-U C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP LEFEBVREBRION, H (reprint author), UNIV PARIS 11,PHOTOPHYS MOLEC LAB,BAT 213,F-91405 ORSAY,FRANCE. NR 36 TC 21 Z9 21 U1 1 U2 2 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 SN 0022-2852 J9 J MOL SPECTROSC JI J. Mol. Spectrosc. PD MAR PY 1993 VL 158 IS 1 BP 140 EP 146 DI 10.1006/jmsp.1993.1061 PG 7 WC Physics, Atomic, Molecular & Chemical; Spectroscopy SC Physics; Spectroscopy GA KQ338 UT WOS:A1993KQ33800014 ER PT J AU WARKENTIN, IG AF WARKENTIN, IG TI PRESUMPTIVE FORAGING ASSOCIATION BETWEEN SHARP-SHINNED HAWKS (ACCIPITER-STRIATUS) AND WHITE-FACED CAPUCHIN MONKEYS (CEBUS-CAPUCINUS) SO JOURNAL OF RAPTOR RESEARCH LA English DT Letter RP WARKENTIN, IG (reprint author), SMITHSONIAN INST,DEPT ZOOL RES,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 9 TC 3 Z9 3 U1 0 U2 2 PU RAPTOR RESEARCH FOUNDATION INC PI HASTINGS PA 12805 ST CROIX TRAIL, HASTINGS, MN 55033 SN 0892-1016 J9 J RAPTOR RES JI J. Raptor Res. PD MAR PY 1993 VL 27 IS 1 BP 46 EP 47 PG 2 WC Ornithology SC Zoology GA KV209 UT WOS:A1993KV20900011 ER PT J AU WASSER, SK THOMAS, R NAIR, PP GUIDRY, C SOUTHERS, J LUCAS, J WILDT, DE MONFORT, SL AF WASSER, SK THOMAS, R NAIR, PP GUIDRY, C SOUTHERS, J LUCAS, J WILDT, DE MONFORT, SL TI EFFECTS OF DIETARY FIBER ON FECAL STEROID MEASUREMENTS IN BABOONS (PAPIO-CYNOCEPHALUS-CYNOCEPHALUS) SO JOURNAL OF REPRODUCTION AND FERTILITY LA English DT Article ID PREGNANCY DIAGNOSIS; REPRODUCTIVE SUPPRESSION; RADIOLABELED ESTRADIOL; EXCRETED STEROIDS; FECAL STEROIDS; YELLOW BABOONS; FECES; METABOLITES; ESTROGENS; HEIFERS AB A study was conducted in captive baboons to determine (i) the impact of cereal dietary fibre on faecal progestogen excretion, and (ii) whether means of controlling dietary effects could be identified. Blood was collected on 3 days per week and faeces on 5 days per week from four unanaesthetized cyclic female baboons, consecutively fed three diets of 5, 10 and 20% fibre for 90 days per diet. A 2 day lag time was detected before progesterone in the blood appeared in the faeces, regardless of diet (mean correlation was 0.62, P = 0.002). Increased dietary fibre had a negative effect on progestogen excretion (P < 0.004). Correspondence between blood and faecal progestogens was consistently greatest and the effect of dietary fibre least when faecal progestogens were expressed g-1 dry faeces. Several means of indexing faecal steroid excretion rates were examined including dehydroepiandrosterone (DHEA) and a number of byproducts of cholesterol metabolism. The cholesterol metabolite, cholestanone, was positively correlated with dietary fibre (r = 0.27; P < 0.04). Multiplying faecal progestogen concentration by the cholestanone g-1 dry faeces concentration increased the correlation between serum and cholestanone-indexed faecal progestogens (r = 0.78, P = 0.0001) compared with nonindexed progestogens (r = 0.71, P = 0.0001). We conclude that expressing faecal progestogens g-1 dry faeces may be sufficient and the most cost-effective method for controlling for most dietary effects when the objective is monitoring longitudinal endocrine status in baboons. However, it may be appropriate to express faecal progestogens by cholestanone concentrations when increased precision is needed to overcome the effects of profound variations in dietary fibre. C1 USDA,LIPID NUTR LAB,BELTSVILLE,MD 20705. NIH,PRIMATE RES UNIT,BETHESDA,MD 20892. RP WASSER, SK (reprint author), SMITHSONIAN INST,CONSERVAT & RES CTR,NATL ZOOL PK,FRONT ROYAL,VA 22630, USA. NR 27 TC 121 Z9 126 U1 2 U2 15 PU J REPROD FERTIL INC PI CAMBRIDGE PA 22 NEWMARKET RD, CAMBRIDGE, ENGLAND CB5 8DT SN 0022-4251 J9 J REPROD FERTIL JI J. Reprod. Fertil. PD MAR PY 1993 VL 97 IS 2 BP 569 EP 574 PG 6 WC Reproductive Biology SC Reproductive Biology GA KX726 UT WOS:A1993KX72600036 PM 8388960 ER PT J AU SIMPSON, JP WITTEBORN, FC GRAPS, A FAZIO, GG KOCH, DG AF SIMPSON, JP WITTEBORN, FC GRAPS, A FAZIO, GG KOCH, DG TI PARTICLE SIGHTINGS BY THE INFRARED TELESCOPE ON SPACELAB-2 SO JOURNAL OF SPACECRAFT AND ROCKETS LA English DT Article ID OPTICAL-CONSTANTS AB Part of the objective of the cooled infrared telescope on Spacelab 2 was to determine the particle environment around the Space Shuttle. The telescope scanned the sky in six wavelength bands ranging from 2 to 100 mum with high time resolution. Dust particles could be identified from their particular signature in the data stream. Particle data from about 4 h early in the mission were analyzed in terms of size, color temperature, velocity, and time. The 1100 particles that were seen were slow moving and ranged in color temperature from 190 to 350 K with a few much hotter. The minimum detectable diameter is between 5 and 15 mum, depending on temperature. The size distribution resembles sample distributions collected at a Shuttle preparation facility. Although particle detection rates varied widely with time, no specific events were identified to be associated with particle production. It was not possible to determine the particle composition, although it was probably not ice. C1 STERLING SOFTWARE,PALO ALTO,CA. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP SIMPSON, JP (reprint author), NASA,AMES RES CTR,MS 245-6,MOFFETT FIELD,CA 94035, USA. NR 12 TC 3 Z9 3 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0022-4650 J9 J SPACECRAFT ROCKETS JI J. Spacecr. Rockets PD MAR-APR PY 1993 VL 30 IS 2 BP 216 EP 221 DI 10.2514/3.11530 PG 6 WC Engineering, Aerospace SC Engineering GA KW276 UT WOS:A1993KW27600010 ER PT J AU GOODWAY, M AF GOODWAY, M TI CHARACTERIZATION OF EARLY AND MODERN WIRE FOR AN ITALIAN HARPSICHORD - DISCUSSION SO JOURNAL OF TESTING AND EVALUATION LA English DT Discussion DE BRASS WIRE; HARDNESS; HARPSICHORD; TENSILE STRENGTH; TABOR RELATIONSHIP; KNOOP HARDNESS METHOD; VICKERS HARDNESS METHOD RP GOODWAY, M (reprint author), SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC TESTING MATERIALS PI W CONSHOHOCKEN PA 100 BARR HARBOR DR, W CONSHOHOCKEN, PA 19428-2959 SN 0090-3973 J9 J TEST EVAL JI J. Test. Eval. PD MAR PY 1993 VL 21 IS 2 BP 136 EP 137 PG 2 WC Materials Science, Characterization & Testing SC Materials Science GA LB485 UT WOS:A1993LB48500008 ER PT J AU SOLOUNIAS, N HAYEK, LAC AF SOLOUNIAS, N HAYEK, LAC TI NEW METHODS OF TOOTH MICROWEAR ANALYSIS AND APPLICATION TO DIETARY DETERMINATION OF 2 EXTINCT ANTELOPES SO JOURNAL OF ZOOLOGY LA English DT Article ID DENTAL MICROWEAR; MOLAR MICROWEAR; EVOLUTION; RUMINANTS; CEBUS AB A separation exists between the tooth microwear of extant ruminant browsers and grazers when examined with new statistical techniques such as the dichotomous, polychotomous and continuous methods. Extant mixed feeders, however, could not be discerned as a distinct group. Many variables were used in the analysis, including two new variables; the area and perimeter of scars. A standard definition of a pit is deduced and a recommendation is made for a method and a model which best characterizes the enamel scars for determination of browsing and grazing dietary categories. The best diagnostic method of tooth microwear analysis utilizes the number of pits smaller than or equal to the ratio four (length over width), the number of scratches between four and 100 micrometres in length to width ratio, and the number of gouges greater than 100 micrometres in length to width ratio. Browsers have many pits and few scratches, with the exception of the giraffe. Grazers have many scratches and few pits, with the exception of the common waterbuck. The tooth microwear analysis suggests that Tragoportax amalthea (Boselaphini, Bovidae) was a mixed feeder at Pikermi and a grazer at Samos. Using the dietary adaptations and the time differences (Pikermi is slightly older than Samos), it is assumed that we have recorded evolutionary change from a mixed feeder to a grazer. Tragoportax rugosifrons from Samos was a grazer. Pikermi and Samos are Miocene (Turolian) localities in Greece. C1 JOHNS HOPKINS UNIV,SCH MED,DEPT CELL BIOL & ANAT,BALTIMORE,MD 21205. SMITHSONIAN INST,WASHINGTON,DC 20560. NR 36 TC 78 Z9 83 U1 0 U2 6 PU OXFORD UNIV PRESS UNITED KINGDOM PI OXFORD PA WALTON ST JOURNALS DEPT, OXFORD, ENGLAND OX2 6DP SN 0952-8369 J9 J ZOOL JI J. Zool. PD MAR PY 1993 VL 229 BP 421 EP 445 PN 3 PG 25 WC Zoology SC Zoology GA KR867 UT WOS:A1993KR86700005 ER PT J AU KOROM, FJ AF KOROM, FJ TI 2 TRADITIONS OF THE BENGALI LANGUAGE - DIL,A SO LANGUAGE IN SOCIETY LA English DT Book Review RP KOROM, FJ (reprint author), SMITHSONIAN INST,CTR FOLKLIFE PROGRAMS & CULTURAL STUDIES,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0047-4045 J9 LANG SOC JI Lang. Soc. PD MAR PY 1993 VL 22 IS 1 BP 138 EP 140 PG 3 WC Linguistics; Sociology SC Linguistics; Sociology GA KR479 UT WOS:A1993KR47900013 ER PT J AU FUDALI, RF AF FUDALI, RF TI THE STRATIGRAPHIC AGE OF AUSTRALITES REVISITED SO METEORITICS LA English DT Note AB The proposed stratigraphic age of 5000-15,000 years for australites found in the vicinity of Port Campbell, Victoria, is demonstrably incorrect. These tektites are not in situ and are also found in an older horizon than previously reported. A minimum stratigraphic age of 250,000 years is calculated from the cosmic-ray-produced He-3 in alluvial diamonds from a horizon that also contains australites near Lake Argyle, Western Australia. There is no reason to believe that a true, rather than a minimum, stratigraphic age for Lake Argyle tektites would not match the many radiometric ages reported in the literature. RP FUDALI, RF (reprint author), SMITHSONIAN INST,DEPT MINERAL SCI,WASHINGTON,DC 20560, USA. NR 16 TC 10 Z9 10 U1 0 U2 0 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 SN 0026-1114 J9 METEORITICS JI Meteoritics PD MAR PY 1993 VL 28 IS 1 BP 114 EP 119 PG 6 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA LA778 UT WOS:A1993LA77800016 ER PT J AU LORNELL, K AF LORNELL, K TI DUKE/PEACOCK-RECORDS - AN ILLUSTRATED HISTORY WITH DISCOGRAPHY - GART,G, AMES,RC SO NOTES LA English DT Book Review RP LORNELL, K (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MUSIC LIBRARY ASSN PI CATON PA BUSINESS OFFICE PO BOX 487, CATON, MA 02021 SN 0027-4380 J9 NOTES JI Notes PD MAR PY 1993 VL 49 IS 3 BP 1076 EP 1077 DI 10.2307/898987 PG 2 WC Music SC Music GA KQ368 UT WOS:A1993KQ36800074 ER PT J AU LORNELL, K AF LORNELL, K TI THE ALADDIN/IMPERIAL LABELS - A DISCOGRAPHY - RUPPLI,M SO NOTES LA English DT Book Review RP LORNELL, K (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU MUSIC LIBRARY ASSN PI CATON PA BUSINESS OFFICE PO BOX 487, CATON, MA 02021 SN 0027-4380 J9 NOTES JI Notes PD MAR PY 1993 VL 49 IS 3 BP 1077 EP 1078 DI 10.2307/898988 PG 2 WC Music SC Music GA KQ368 UT WOS:A1993KQ36800075 ER PT J AU MCLAUGHLIN, BM GILLAN, CJ BURKE, PG DAHLER, JS AF MCLAUGHLIN, BM GILLAN, CJ BURKE, PG DAHLER, JS TI (3)SIGMA-U+ BOUND AND CONTINUUM STATES IN E(-)-HE-2(+) SCATTERING SO PHYSICAL REVIEW A LA English DT Article ID R-MATRIX METHOD; LASER-ASSISTED IONIZATION; POTENTIAL-ENERGY CURVES; ASSOCIATIVE IONIZATION; INFRARED-SPECTRUM; HYPERFINE-STRUCTURE; RYDBERG STATES; COLLISIONS; HELIUM; ATOMS AB Ab initio calculations are performed on the e--He2+ complex using the R-matrix technique. A two-state approximation is utilized in which the X 2SIGMA(u)+ and the A 2SIGMA(g)+ electronic states of He2+, in the close-coupling expansion, are represented by truncated configuration-interaction (CI) wave functions obtained from multiconfiguration-self-consistent-field-complete-active-space-SCF (MCSCF-CASSCF) calculations. A (4s,2p,2d) Slater basis is used to perform bound-state calculations at SCF, full CI, and MCSCF-CASSCF levels, to gauge the quality of wave functions at various bond separations. Elastic cross sections are presented for selected bond lengths in the range 1.5-4.0a0, for the 3SIGMA(u)+ total symmetry. He2*(1sigma(g)1sigma(u)2npsigma and nfsigma3SIGMA(u)+) resonances are detected at each separation and fitted to Breit-Wigner formulas in order to determine their energies and autoionization widths. In addition, low-lying He2*(1sigma(g)21sigma(u)ns,nd, and ng 3SIGMA(u)+) bound states are also calculated at several geometries. C1 QUEENS UNIV BELFAST,DEPT APPL MATH & THEORET PHYS,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. UNIV MINNESOTA,DEPT CHEM,MINNEAPOLIS,MN 55455. UNIV MINNESOTA,DEPT CHEM ENGN & MAT SCI,MINNEAPOLIS,MN 55455. RP MCLAUGHLIN, BM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 68 TC 7 Z9 7 U1 0 U2 5 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAR PY 1993 VL 47 IS 3 BP 1967 EP 1980 DI 10.1103/PhysRevA.47.1967 PG 14 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA KV980 UT WOS:A1993KV98000047 ER PT J AU HU, YQ HABBAL, SR AF HU, YQ HABBAL, SR TI INTERACTION BETWEEN PERPENDICULAR MAGNETOHYDRODYNAMIC SHOCKS SO PHYSICS OF FLUIDS B-PLASMA PHYSICS LA English DT Article AB This paper discusses the interaction between perpendicular magnetohydrodynamic shocks (S) as well as tangential discontinuities (T). The main conclusions are as follows: (1) The collision between a forward shock (S) and a reverse shock (S<--) produces a shock system consisting of a weaker reverse shock, a tangential discontinuity, and a weaker forward shock, namely, S-->S<-- --> S<--TS-->. (2) The merging of two forward shocks leads to a stronger forward shock, followed by a tangential discontinuity and a reverse wave. For a given beta(r) (the ratio of gas pressure to magnetic pressure) of the background plasma, there exists a critical parameter gamma(c). When the adiabatic index gamma < gamma(c), the reverse wave is a rarefaction wave (R). When gamma > gamma(c), the reverse wave produced by merging of strong shocks is still a rarefaction wave but the reverse wave becomes a shock when weak shocks merge. (3) The interaction between a forward shock and a tangential discontinuity may form S<--TS-->, R<--TS-->, or TS-->, depending on the strength of the initial forward shock and the property of the initial tangential discontinuity. C1 UNIV SCI & TECHNOL CHINA,DEPT EARTH & SPACE SCI,HEFEI 230026,PEOPLES R CHINA. RP HU, YQ (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 5 TC 4 Z9 6 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0899-8221 J9 PHYS FLUIDS B-PLASMA PD MAR PY 1993 VL 5 IS 3 BP 732 EP 741 DI 10.1063/1.860516 PG 10 WC Physics, Fluids & Plasmas SC Physics GA KR123 UT WOS:A1993KR12300008 ER PT J AU PULLIN, AS WOLDA, H AF PULLIN, AS WOLDA, H TI GLYCEROL AND GLUCOSE ACCUMULATION DURING DIAPAUSE IN A TROPICAL BEETLE SO PHYSIOLOGICAL ENTOMOLOGY LA English DT Article DE STENOTARSUS; DIAPAUSE; COLD TOLERANCE; CRYOPROTECTANT; GLYCEROL ID PIERIS-BRASSICAE; COLD TOLERANCE; PHYSIOLOGY AB Carbohydrate changes were measured during the 10-month adult diapause in the neotropical beetle, Stenotarsus rotundus Arrow (Endomychidae, Coleoptera) to test the hypothesis that metabolic suppression causes the accumulation of polyols in the absence of the need for cold tolerance. Glycerol and glucose both accumulate during the first 3 months from June to September, but decline in October, accumulate again in December-January and finally decline after January and stay low until the adults leave their diapause site in April. Any adaptive significance for this pattern is unknown but its coincidence with previously measured metabolic suppression suggests that glycerol and glucose accumulate as a result of metabolic adjustments during diapause. The relevance of these results to the evolution of polyol accumulation for cryoprotection in temperate insects in discussed. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. RP PULLIN, AS (reprint author), UNIV KEELE,DEPT BIOL SCI,KEELE ST5 5BG,STAFFS,ENGLAND. NR 15 TC 24 Z9 26 U1 2 U2 7 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0307-6962 J9 PHYSIOL ENTOMOL JI Physiol. Entomol. PD MAR PY 1993 VL 18 IS 1 BP 75 EP 78 DI 10.1111/j.1365-3032.1993.tb00451.x PG 4 WC Entomology SC Entomology GA KT356 UT WOS:A1993KT35600010 ER PT J AU MANNING, RD AF MANNING, RD TI CULTURAL-DIVERSITY OR DIVERSE CULTURES - THE TANGLED FOLIAGE OF MULTICULTURALISM SO PROTEUS LA English DT Article C1 SMITHSONIAN INST,INSTITUTIONAL STUDIES OFF,WASHINGTON,DC 20560. RP MANNING, RD (reprint author), AMERICAN UNIV,WASHINGTON,DC 20016, USA. NR 34 TC 1 Z9 1 U1 0 U2 1 PU PROTEUS PI SHIPPENSBURG PA SHIPPENSBURG UNIV, SHIPPENSBURG, PA 17257 SN 0889-6348 J9 PROTEUS JI Proteus PD SPR PY 1993 VL 10 IS 1 BP 3 EP 10 PG 8 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA LD146 UT WOS:A1993LD14600004 ER PT J AU BUNCH, LG AF BUNCH, LG TI MORE THAN KNOTTS-BERRY-FARM, MUSEUMS AND SOUTHERN-CALIFORNIA + GUIDE TO HISTORIC-HOUSES, MUSEUMS, PRESIDENTIAL-ARCHIVES AND ETHNOGRAPHIC-COLLECTIONS REVIEWED BY CALIFORNIA RESIDENTS SO PUBLIC HISTORIAN LA English DT Article RP BUNCH, LG (reprint author), SMITHSONIAN INST,NATL MUSEUM AMER HIST,WASHINGTON,DC 20560, USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU UNIV CALIF PRESS PI BERKELEY PA JOURNALS DEPT 2120 BERKELEY WAY, BERKELEY, CA 94720 SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD SPR PY 1993 VL 15 IS 2 BP 161 EP 210 PG 50 WC History SC History GA KY640 UT WOS:A1993KY64000030 ER PT J AU PROSSER, CF SCHILD, RE STAUFFER, JR JONES, BF AF PROSSER, CF SCHILD, RE STAUFFER, JR JONES, BF TI PHOTOMETRIC LIGHT CURVES FOR 10 RAPIDLY ROTATING STARS IN ALPHA PERSEI, THE PLEIADES, AND THE FIELD SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID MAIN-SEQUENCE STARS; LOW-MASS STARS; X-RAY SURVEY; TAURUS-AURIGA; MOLECULAR CLOUD; TIME-SERIES; CLUSTER; VELOCITIES; EVOLUTION; DWARFS AB We present the results from a photometric monitoring program of ten rapidly rotating stars observed during 1991 using the Fred Lawrence Whipple Observatory (FLWO) 48-in. telescope. Brightness variations for an additional six cluster stars observed with the Lick 40-in. telescope are also given. The periods and light curves for seven alpha Persei members, two Pleiades members, and one naked T Tauri field star are reported. The individual photometric measurements have been deposited with the NSSDC. C1 UNIV CALIF SANTA CRUZ,LICK OBSERV,BOARD STUDIES ASTRON & ASTROPHYS,SANTA CRUZ,CA 95064. RP PROSSER, CF (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 45 TC 44 Z9 44 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD MAR PY 1993 VL 105 IS 685 BP 269 EP 276 DI 10.1086/133141 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KU971 UT WOS:A1993KU97100002 ER PT J AU MATHIS, WN AF MATHIS, WN TI A NEW SPECIES AND SUBGENUS OF PERISCELIS LOEW FROM AUSTRALIA (DIPTERA, PERISCELIDIDAE) SO JOURNAL OF THE AUSTRALIAN ENTOMOLOGICAL SOCIETY LA English DT Article AB Periscelis (Notioscelis) fasciata subgen. et sp.n., from New South Wales and Queensland, is the first species of Periscelidinae to be described from Australian specimens. Family, subfamily, generic and subgeneric diagnoses and a key to subgenera of Periscelis are provided. Notioscelis is suggested to be the sister group of Periscelis sensu stricto based on morphological evidence. RP MATHIS, WN (reprint author), SMITHSONIAN INST,DEPT ENTOMOL,NHB 169,WASHINGTON,DC 20560, USA. NR 24 TC 2 Z9 2 U1 0 U2 0 PU AUSTRALIAN ENTOMOLOGICAL SOC PI CANBERRA PA CSIRO ENTOMOLOGY GPO BOX 1700, CANBERRA 2601, AUSTRALIA SN 0004-9050 J9 J AUST ENTOMOL SOC JI J. Aust. Entomol. Soc. PD FEB 26 PY 1993 VL 32 BP 13 EP 19 PN 1 PG 7 WC Entomology SC Entomology GA KQ583 UT WOS:A1993KQ58300004 ER PT J AU DOLLFUS, A DESCHAMPS, M ZIMBELMAN, JR AF DOLLFUS, A DESCHAMPS, M ZIMBELMAN, JR TI SOIL TEXTURE AND GRANULOMETRY AT THE SURFACE OF MARS SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARTIAN DUST STORMS; PHYSICAL-PROPERTIES; POLARIMETRIC ANALYSIS; THERMAL INERTIA; ALBEDO; ATMOSPHERE; HISTORY; CLOUDS; SITES AB The physical behavior of the Martian surface soil has been characterized remotely by both photopolarimetry and radiometry. The degree of linear polarization defines a coefficient b which is related to the top surface soil texture and is calibrated in terms of grain size, or as a fraction of the area exhibiting uncovered clean rocks, This coefficient b was recorded with the instrument VPM (Visual Polarimeter Mars) on board Soviet orbiter MARS 5 in 1974. The radiometric thermal inertia coefficient I is essentially a measurement of the soil compaction, or an effective average particle size in the soil texture, through the few decimeters below the top surface sensed by polarimetry. The instrument IRTM (Infra Red Thermal Mapper) was used on board the Viking spacecraft between 1976 and 1982. The polarimetric scans raked a strip covering two contrasting regions, the dark-hued Mare Erythraeum and the light-hued Thaumasia. Over these wide areas, several smaller typical terrains were characterized by the three parameters A (albedo), b (related to top surface grain size) and I (underlaying compaction or block size). The large dark region Erythraeum is characterized everywhere by a uniform polarization response, despite the large geomorphological diversity of the surface. The values of A and b indicate a ubiquitous coating or mantling with small dark grains of albedo 12.7%, with a radius of 10 to 20 mum. Thermal inertia coefficient I indicates that the sub-surface is divided in pieces around 300 to 600 mum in size. A simple model consisting of sand-size particles completely coated with 15 mum black grains is compatible with both measurements. Conversely, the brighter terrain Thaumasia discloses a large variety of soil properties. A typical location with albedo 16.3% has a surface covered with orange grains, probably very dispersed in size, for which the largest grains are 20 to 40 mum. The subsurface is divided into pieces 180-300 mum or smaller, if cemented. On the basis of terrestrial analogs of the Martian soil (Morris et al., 1990), it is surmised that the near-surface soil on the dark areas could be tachylite sand-size grains surficially coated by cohesive black particles of titanomagnetite. The bright orange grains in the Thaumasia-like terrains could be made of the weathered (palagonitized) basalt glass particles of sideromelane, as found in terrestrial analogs (Singer, 1982). Thaumasia is known to be a source area for dust storm production. The observed soil texture provides the large grains needed for saltation to occur, causing the intermixed small grains to be ejected from the surface and carried by wind. C1 SMITHSONIAN INST, NASM, CEPS, WASHINGTON, DC 20560 USA. RP DOLLFUS, A (reprint author), OBSERV PARIS, ASTROPHYS SECT, 5 PL JULES JANSSEN, F-92195 MEUDON, FRANCE. NR 56 TC 11 Z9 11 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB 25 PY 1993 VL 98 IS E2 BP 3413 EP 3429 DI 10.1029/92JE01502 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA KX587 UT WOS:A1993KX58700027 ER PT J AU CRADDOCK, RA MAXWELL, TA AF CRADDOCK, RA MAXWELL, TA TI GEOMORPHIC EVOLUTION OF THE MARTIAN HIGHLANDS THROUGH ANCIENT FLUVIAL PROCESSES SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PHYSICAL-PROPERTIES; EARLY ATMOSPHERE; ISIDIS BASIN; MARS; WATER; VALLEYS; MORPHOLOGY; HISTORY; RELEASE; EJECTA AB Craters in the Martian highlands are preserved in various stages of degradation. As a result of an erosional process active from the Middle Noachian (4.40-3.92 b.y.) through the Hesperian (3.55-1.8 b.y.), ejecta associated with fresh impact craters became etched, hummocky, and dissected by runoff channels. With time, interior gullies became deeply incised and ejecta deposits were entirely removed. Infilling of the craters followed until, in some instances, the craters were completely buried. Only fluvial processes explain these morphologic variations, the size range of affected craters, and the size-frequency distribution curves associated with these crater populations. Based on the number of superposed fresh impact craters, fluvial processes affecting the highlands ceased entirely by the end of the Hesperian. No correlation between cessation of degradation and latitude exists. However, a strong correlation exists between cessation of degradation and elevation. Degradation ended at higher elevations (e.g., 3-4 km; N[5]= approximately 200, Late Noachian) before lower elevations (e.g., 1-2 km; N[5]= approximately 180, Early Hesperian), suggesting that cessation was coupled to desiccation of the volatile reservoir and degassing of a 5-20 bar primordial atmosphere. Volatiles released to the surface by runoff channel formation and seepage may have been part of a complex hydrologic cycle that included periodic, heavy amounts of precipitation. Rainfall was principally responsible for degrading the highlands, eroding impact craters, and redistributing sediments. Rainfall also recharged the highland aquifers, allowing sapping and seepage to continue for hundreds of millions of years. As the primordial atmosphere was lost, cloud condensation, and thus rainfall and aquifer recharge, occurred at progressively lower elevations. Based on estimates on the amount of material removed and duration of degradation, denudation rates averaged 0.0001-0.005 mm/yr. These rates arc equivalent to those in terrestrial periglacial environments. RP SMITHSONIAN INST, NATL AIR & SPACE MUSEUM, CTR EARTH & PLANETARY STUDIES, WASHINGTON, DC 20560 USA. RI Craddock, Robert/B-3884-2013 NR 92 TC 159 Z9 159 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD FEB 25 PY 1993 VL 98 IS E2 BP 3453 EP 3468 DI 10.1029/92JE02508 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA KX587 UT WOS:A1993KX58700029 ER PT J AU RALLS, K MEADOWS, R AF RALLS, K MEADOWS, R TI CONSERVATION GENETICS - BREEDING LIKE FLIES SO NATURE LA English DT Editorial Material RP RALLS, K (reprint author), SMITHSONIAN INST,NATL ZOOL PK,WASHINGTON,DC 20008, USA. NR 12 TC 12 Z9 12 U1 0 U2 1 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD FEB 25 PY 1993 VL 361 IS 6414 BP 689 EP 690 DI 10.1038/361689a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA KN789 UT WOS:A1993KN78900031 PM 8441462 ER PT J AU BAND, YB AF BAND, YB TI FORMATION OF LARGE-SCALE COSMIC STRUCTURE BY THE DOPPLER INSTABILITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE INSTABILITIES; LARGE-SCALE STRUCTURE OF UNIVERSE ID PRIMORDIAL STELLAR EVOLUTION; LASER-RADIATION; HYDROGEN; ATOMS; PHASE AB Hogan suggested that a bulk Doppler instability of homogeneous hydrogen interacting with electromagnetic radiation via atomic resonance scattering could be responsible for the large-scale structure of the universe. We carry out an analysis within the context of the Hogan model to determine the consequences of including the dynamical effects of viscosity, long-range radiation trapping and radiation attenuation forces, heat conduction, radiation loss, and also the effect of matter which does not directly interact with the rear-resonant radiation, but is coupled to the hydrogen by collisions. The Doppler instability survives inclusion of all these effects. We find that (a) the Doppler instability growth rate for large-scale perturbations, proportional to photon density in a spectrally narrow blueshifted feature, is very large (10(-6) yr-1 even for excess blueshifted photon densities that are 10(-16) of the hydrogen density at z almost-equal-to 1000), (b) it is unlikely that the homogeneous microwave radiation is affected given the small number of photons required to initiate the instability, (c) the long-range radiation trapping and radiation attenuation forces are too weak to affect the growth rate of fluctuations because the atomic density in the cosmos after recombination is small, and (d) the effects of pressure and viscosity limit the fluctuations only for submegaparsec scales. However, the source of spectrally narrow features to the blue of hydrogen (or He) resonance lines is problematic. We propose a mechanism for the production of photons in narrow energy ranges to the blue of Lyman resonance lines of H involving Balmer lines produced in the recombination of He II. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. RP BAND, YB (reprint author), BEN GURION UNIV NEGEV,DEPT CHEM,IL-84105 BEER SHEVA,ISRAEL. NR 25 TC 1 Z9 1 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1993 VL 404 IS 2 BP 425 EP 435 DI 10.1086/172295 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KL879 UT WOS:A1993KL87900002 ER PT J AU HURT, RL TURNER, JL HO, PTP MARTIN, RN AF HURT, RL TURNER, JL HO, PTP MARTIN, RN TI WARM MOLECULAR GAS IN A STARBURST - CO (3-2) OBSERVATIONS OF MAFFEI-2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (MAFFEI-2); GALAXIES, ISM; GALAXIES, SPIRAL; GALAXIES, STARBURST ID CARBON-MONOXIDE; SPIRAL GALAXIES; STAR FORMATION; HOT GAS; CLOUDS; EMISSION; NUCLEUS; CALIBRATION; EXTINCTION; LINES AB We have mapped the CO J = 3-2 emission in the inner 60'' (1500 pc) of the nearby SBb(s) pec galaxy Maffei 2 with the Caltech Submillimeter Observatory (CSO). The morphology of the CO (3-2) matches that seen in CO (1-0) interferometric maps, possessing a barlike structure that is coincident with the morphology of radio continuum and mid-infrared observations of the extended starburst region. By assuming that the observed CO (3-2) emission is optically thin we set lower limits to the molecular column densities along the bar of N(H-2)6-9 x 10(20) CM-2 and to the total molecular mass of M(H-2) greater-than-or-equal-to 10(6) M.. Since this reflects only approximately 3% of the total molecular mass for the region estimated from (CO)-C13 (1-0) measurements, the CO (3-2) observations probably sample only the outer, and possibly warmer, surfaces of very optically thick molecular clouds. Indeed, comparisons with other CO transitions indicate that the emission is optically thick with tau(CO)(3-2) approximately 25-35 [equivalent to tau(CO(1-0)) approximately 5-7], which is consistent with the optical depths inferred from CO (1-0) observations. C1 UNIV CALIF LOS ANGELES, DEPT PHYS, LOS ANGELES, CA USA. UNIV CALIF LOS ANGELES, DEPT ASTRON, LOS ANGELES, CA USA. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85721 USA. NR 36 TC 22 Z9 22 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1993 VL 404 IS 2 BP 602 EP 610 DI 10.1086/172313 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KL879 UT WOS:A1993KL87900020 ER PT J AU HUGHES, JP BUTCHER, JA STEWART, GC TANAKA, Y AF HUGHES, JP BUTCHER, JA STEWART, GC TANAKA, Y TI GINGA OBSERVATIONS OF THE COMA CLUSTER AND STUDIES OF THE SPATIAL-DISTRIBUTION OF IRON SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERS, INDIVIDUAL (COMA); GALAXIES, INTERGALACTIC MEDIUM; X-RAYS, GALAXIES ID X-RAY ASTRONOMY; SPIRAL GALAXIES; ENERGY-SPECTRA; PERSEUS; TEMPERATURE; A1367; GAS AB The large area counters on the Japanese satellite Ginga have been used to determine the X-ray spectrum from the central region of the Coma cluster of galaxies over the energy range from 1.5 to 20 keV. The spectrum is well represented by an isothermal model of temperature 8.21 + 0.16 keV and a heavy element (iron) abundance of 0.212 +/- 0.027, relative to the cosmic value. The Ginga spectrum was found to be consistent with the X-ray spectra from the Tenma and EXOSAT satellites for a large class of nonisothermal temperature distributions. The measured iron elemental abundances were used to set a lower limit on the total mass of iron in Coma under the assumption that the iron is not distributed uniformly throughout the cluster. The mass ratio of iron relative to hydrogen (within 2 Mpc) is not less than 18% of the cosmic iron to hydrogen mass ratio. This compares to an average abundance of 24 % if the iron is distributed uniformly. We discuss these results in terms of models for the production of iron in galaxy clusters. C1 UNIV LEICESTER,DEPT PHYS,X-RAY ASTRON GRP,LEICESTER LE1 7RH,ENGLAND. INST SPACE & ASTRONAUT SCI,SAGAMIHARA,KANAGAWA 229,JAPAN. RP HUGHES, JP (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 35 TC 54 Z9 54 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1993 VL 404 IS 2 BP 611 EP 619 DI 10.1086/172314 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KL879 UT WOS:A1993KL87900021 ER PT J AU VRTILEK, SD SOKER, N RAYMOND, JC AF VRTILEK, SD SOKER, N RAYMOND, JC TI EFFECTS OF INCLINATION ANGLE ON THE SPECTRA OF X-RAY BINARIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; X-RAYS, STARS ID K LINE EMISSION; HERCULES X-1-HZ HERCULIS; ACCRETION DISK CORONAE; SCORPIUS X-1; CYGNUS X-2; EXOSAT OBSERVATIONS; MULTIWAVELENGTH CAMPAIGN; ORBITAL PERIOD; SYSTEM; IUE AB Iron emission and absorption features from nine X-ray binaries are compared with a model that predicts characteristics of iron K-shell features corresponding to different viewing angles for the accretion disk. In this model, emission and absorption features arise from an accretion disk corona whose structure is computed under the assumptions of ionization, thermal, and hydrostatic balance of gas illuminated by the central continuum source. Hence the equivalent widths of the emission and absorption features are predicted without the introduction of any free parameters to control the physical conditions in the disk corona. Our data/model comparison suggests an explanation for the equivalent widths of the iron K(alpha) emission and the depth of the absorption edge in terms of (1) the angle of inclination between the observer's line of sight and the plane of the accretion disk and (2) the shape of the incident source spectrum. RP VRTILEK, SD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 62 TC 22 Z9 22 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1993 VL 404 IS 2 BP 696 EP 705 DI 10.1086/172323 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KL879 UT WOS:A1993KL87900030 ER PT J AU SAAR, SH HUOVELIN, J AF SAAR, SH HUOVELIN, J TI BROAD-BAND LINEAR-POLARIZATION IN COOL STARS .2. AMPLITUDE AND WAVELENGTH DEPENDENCE FOR MAGNETIC AND SCATTERING REGIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE POLARIZATION; STARS, LATE-TYPE; STARS, MAGNETIC FIELDS ID STELLAR MODEL CHROMOSPHERES; SOLAR-TYPE STARS; OUTER ATMOSPHERES; ALPHA-ORIONIS; DWARF STARS; TEMPERATURE; SPECTRA; FIELDS AB We have developed a model to estimate the amplitude and wavelength dependence of broad-band linear polarization (BLP) from magnetic regions on cool stars. The model includes corrections both for line blends and for the partial cancellation of polarization in the vector sum over the stellar disk. Our results agree with recent calculations of BLP in the red, but show larger amplitudes and a different wavelength dependence in the blue. We find that the detailed wavelength dependence of the polarization is complex and varies with effective temperature and gravity due to changes in line blanketing. The BLP amplitudes depend strongly on field strength, blanketing, and magnetic region filling factor and geometry. We make rough estimates of the maximum BLP for stars of various spectral types and demonstrate a method for deriving a lower limit to the filling factor from the maximum observed BLP. This lower limit is related to the fractional area covered by the spatially asymmetric component of magnetic regions. Since Rayleigh and Thomson scattering are also sources of BLP. we estimate their amplitudes for a variety of cool stars. In cool dwarfs, magnetic BLP will usually dominate; only in stars of low gravity are similar levels of scattering and magnetic BLP likely. It is possible to distinguish the source of BLP by its wavelength dependence; however, to do so requires data of very high accuracy (typically a few times 10(-5)). We reanalyze some previous BLP observations to determine whether they are dominated by magnetic or Rayleigh scattering effects. In most cases, the wavelength dependence of the data admit either possibility; the polarization amplitudes, however, suggest that magnetic origins are more likely. C1 UNIV HELSINKI, ASTROPHYS LAB, SF-00130 HELSINKI, FINLAND. UNIV HELSINKI OBSERV, SF-00130 HELSINKI, FINLAND. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 59 TC 21 Z9 21 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1993 VL 404 IS 2 BP 739 EP 750 DI 10.1086/172328 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KL879 UT WOS:A1993KL87900035 ER PT J AU TORRELLES, JM RODRIGUEZ, LF CANTO, J HO, PTP AF TORRELLES, JM RODRIGUEZ, LF CANTO, J HO, PTP TI A CIRCUMSTELLAR MOLECULAR GAS STRUCTURE ASSOCIATED WITH THE MASSIVE YOUNG STAR CEPHEUS-A-HW-2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (CEPHEUS-A); ISM, JETS AND OUTFLOWS; ISM, MOLECULES; H-II REGIONS ID OUTFLOWS; OBJECTS; TAURI; DISK AB We report the detection via VLA-D observations of ammonia of a circumstellar high-density molecular gas structure toward the massive young star related to the object Cepheus A-HW 2, a firm candidate for the powering source of the high-velocity molecular outflow in the region. This structure has a deconvolved angular size of 3.3'' x 2.3'' (p.a. = 22-degrees), or 2400 x 1700 AU at a distance of 725 pc. For this circumstellar molecular gas structure we derive an average column density N(H2) congruent-to 1 X 10(24)(X(NH3)/10(-8)) cm-2 , a volume density n(H-2) congruent-to 3 X 10(7)(X(NH3)/10(-8)) cm-3, and a mass M(H-2) congruent-to 2(X(NH3)/10(-8)) M.. The ammonia emission shows velocity variations of approximately 4 km s-1 across the condensation. HW 2 was previously reported to be a double radio source, separated by approximately 0.2'' (or 150 AU) with p.a. congruent-to 30-degrees-40-degrees. We suggest that the circumstellar molecular gas structure could be related to the circumstellar disk previously suggested from infrared, H2O, and OH maser observations. We consider as a plausible scenario that the double radio continuum source of HW 2 could represent the ionized inner part of the circumstellar disk, in the same way as proposed to explain the double radio source in L1551. The observed motions in the circumstellar molecular gas can be produced by bound motions (e.g., infall or rotation) around a central mass of approximately 10-20 M. (BO.5 V star or earlier). C1 Univ Nacl Autonoma Mexico, INST ASTRON, MEXICO CITY 04510, DF, MEXICO. HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP TORRELLES, JM (reprint author), CSIC, INST ASTROFIS ANDALUCIA, CORREOS 3004, C SANCHO PANZA S-N, E-18080 GRANADA, SPAIN. OI Torrelles, Jose Maria/0000-0002-6896-6085 NR 24 TC 15 Z9 15 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 20 PY 1993 VL 404 IS 2 BP L75 EP + DI 10.1086/186747 PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KL881 UT WOS:A1993KL88100011 ER PT J AU SCOTT, TC BABB, JF DALGARNO, A MORGAN, JD AF SCOTT, TC BABB, JF DALGARNO, A MORGAN, JD TI RESOLUTION OF A PARADOX IN THE CALCULATION OF EXCHANGE FORCES FOR H-2+ SO CHEMICAL PHYSICS LETTERS LA English DT Article ID ENERGY; H2+ AB Tang, Toennies and Yiu have shown that despite the inherent symmetry of H-2+, wavefunctions obtained from a combination of the unsymmetrized polarization expansion and the 1/R expansion can be used in the Holstein-Herring formula to calculate for large internuclear distances R the leading O (e(-R)) terms in the exchange energy between the lowest pair of states. However, the associated claim by Tang and Toennies that the polarization expansion of the wavefunction converges not to the gerade molecular wavefunction, but to an asymmetric function localized about a single nucleus, conflicts with other numerical and analytical results. We show by a limiting procedure that use of the infinite polarization expansion for the wavefunction in the Holstein-Herring formula provides a result that is not equal to the exact exchange energy, although it has the correct leading O (e(-R)) behavior and is impressively close to the exact exchange energy for large R. C1 UNIV DELAWARE,DEPT PHYS & ASTRON,NEWARK,DE 19716. RP SCOTT, TC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Babb, James/0000-0002-3883-9501 NR 18 TC 19 Z9 19 U1 1 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2614 J9 CHEM PHYS LETT JI Chem. Phys. Lett. PD FEB 19 PY 1993 VL 203 IS 2-3 BP 175 EP 183 DI 10.1016/0009-2614(93)85383-Y PG 9 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA KL975 UT WOS:A1993KL97500015 ER PT J AU HUANG, SQ DUBINSKI, J CARLBERG, RG AF HUANG, SQ DUBINSKI, J CARLBERG, RG TI ORBITAL DEFLECTIONS IN N-BODY SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE CELESTIAL MECHANICS, STELLAR DYNAMICS; GALAXIES, KINEMATICS AND DYNAMICS; METHODS, NUMERICAL ID STELLAR-SYSTEMS; MERGING GALAXIES; SIMULATIONS; EVOLUTION AB We discuss two types of orbital deflection in N-body systems with a softened field: two-body relaxation and orbital divergence. We study two-body relaxation using tree code N-body simulations of King models with N ranging from 10(2) to 4 x 10(5), and a softening length, epsilon, ranging from 2 x 10(-4) to 7.5 x 10(-2) in units of the half-mass radius. The relaxation time, T(E), depends linearly on N for a fixed softening length, i.e., T(E) is-proportional-to N in contrast to the usually quoted N/ln N dependence. The relaxation time also depends on epsilon as, T(E) is-proportional-to 1/ln (R/epsilon), where R is the radius of the system. At the half-mass radius, T(E) is 0.6-1.0 times the local orbit-averaged Fokker-Planck estimate. The energy evolution of particles is a pure random walk or diffusion process as shown by the constant rate of change of the squared energy fluctuation, SIGMA (DELTAE(i)2)/DELTAt, and the particles' energy power spectrum follows a power law with spectral index -2. The diffusion time is nearly equal to the relaxation time. We study orbital divergence using N-body simulations with N = 2.5 x 10(2) to 4 x 10(3) and epsilon = 0.0125 to 0.1. The orbital divergence follows the exponential law, DELTA(t) = DELTA(0) exp (t/T(e)), where T(e) is the e-folding time and, DELTA(0) is the initial phase separation. The averaged e-folding time is comparable with the crossing time, T(c), and varies as N(alpha)epsilon(beta), where alpha and beta measured from numerical simulations are 0.26 and 0.45, respectively. The deviation of alpha and beta from Goodman, Heggie, and Hut's values of 1/3 and 2/3 is discussed. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP HUANG, SQ (reprint author), UNIV TORONTO,DEPT ASTRON,60 ST GEORGE ST,TORONTO M5S 1A7,ONTARIO,CANADA. RI Carlberg, Raymond/I-6947-2012 OI Carlberg, Raymond/0000-0002-7667-0081 NR 29 TC 26 Z9 27 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 1993 VL 404 IS 1 BP 73 EP 80 DI 10.1086/172259 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KK912 UT WOS:A1993KK91200007 ER PT J AU REYNOLDS, PT AKERLOF, CW CAWLEY, MF CHANTELL, M FEGAN, DJ HILLAS, AM LAMB, RC LANG, MJ LAWRENCE, MA LEWIS, DA MACOMB, D MEYER, DI MOHANTY, G OFLAHERTY, KS PUNCH, M SCHUBNELL, MS VACANTI, G WEEKES, TC WHITAKER, T AF REYNOLDS, PT AKERLOF, CW CAWLEY, MF CHANTELL, M FEGAN, DJ HILLAS, AM LAMB, RC LANG, MJ LAWRENCE, MA LEWIS, DA MACOMB, D MEYER, DI MOHANTY, G OFLAHERTY, KS PUNCH, M SCHUBNELL, MS VACANTI, G WEEKES, TC WHITAKER, T TI SURVEY OF CANDIDATE GAMMA-RAY SOURCES AT TEV ENERGIES USING A HIGH-RESOLUTION CERENKOV IMAGING-SYSTEM - 1988-1991 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA RAYS, BURSTS; ISM, INDIVIDUAL (CRAB NEBULA) ID GALACTIC PLANE; CRAB-NEBULA; HERCULES-X-1; EMISSION; SEARCH; PULSAR AB The steady TeV gamma-ray emission from the Crab Nebula has been used to optimize the sensitivity of the Whipple Observatory atmospheric Cerenkov imaging telescope. Using this method, which is of order 20 times more sensitive than the standard method using a simple non-imaging detector, it is possible to detect the Crab Nebula at a significance level in excess of 6 standard deviations (6 sigma) in under 1 hr on source (with a corresponding time observing a background comparison region); a source one-tenth the strength of the Crab Nebula can be detected at the 4 sigma level after 40 hr on the source (and 40 hr on a background region). A variety of sources have been monitored using this technique over the period 1988-1991, but none were detected apart from the Crab Nebula. Upper limits are presented which in many instances are a factor of 10 below the flux of the Crab Nebula. These upper limits assume steady emission from the source and cannot rule out sporadic gamma-ray emission with short duty cycles. C1 IOWA STATE UNIV SCI & TECHNOL,DEPT PHYS & ASTRON,AMES,IA 50011. UNIV MICHIGAN,RANDALL LAB PHYS,ANN ARBOR,MI 48109. ST PATRICKS COLL,DEPT PHYS,MAYNOOTH,KILDARE,IRELAND. HARVARD SMITHSONIAN CTR ASTROPHYS,FRED LAWRENCE WHIPPLE OBSERV,AMADO,AZ 85645. UNIV LEEDS,DEPT PHYS,LEEDS LS2 9JT,W YORKSHIRE,ENGLAND. RP REYNOLDS, PT (reprint author), NATL UNIV IRELAND UNIV COLL DUBLIN,DEPT PHYS,DUBLIN 4,IRELAND. OI Punch, Michael/0000-0002-4710-2165; Lang, Mark/0000-0003-4641-4201 NR 70 TC 136 Z9 136 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 1993 VL 404 IS 1 BP 206 EP 218 DI 10.1086/172269 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KK912 UT WOS:A1993KK91200017 ER PT J AU PETERSON, RC ORE, CMD KURUCZ, RL AF PETERSON, RC ORE, CMD KURUCZ, RL TI THE NONSOLAR ABUNDANCE RATIOS OF ARCTURUS DEDUCED FROM SPECTRUM SYNTHESIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, ABUNDANCES; STARS, INDIVIDUAL (ALPHA-BOOTIS); STARS, LATE-TYPE ID RELATIVE OSCILLATOR-STRENGTHS; METAL-POOR STARS; FE-I; SOLAR ABUNDANCE; LINES; IRON; TRANSITIONS; METALLICITY; TEMPERATURE; EVOLUTION AB Using opacity distribution functions based on a newly expanded atomic and molecular line list, we have calculated a model atmosphere for Arcturus that reproduces the observed flux distribution. Individual line parameters in the list were adjusted to match the solar spectrum in a preliminary way, in the regions 5000-5500 angstrom, 6000-6500 angstrom, and 7500-9000 angstrom. The Arcturus model spectrum calculated with these adjustments reproduces well the profiles of all lines in the observed spectrum of the Griffin atlas for which the solar gf-values are well determined. The Arcturus model has an iron abundance [Fe/H] = -0.5 +/- 0.1, a temperature T(eff) = 4300 +/- 30 K, gravity log g = 1.5 +/- 0.15, and an overabundance of the light metals. The factor of 2 enhancement in Arcturus of O, Mg, Si, Ca, and Ti is similar to that of halo stars of much lower metallicity and velocity about the Galactic center. This enhancement significantly affects the ionization equilibria and opacities of Arcturus. C1 SMITHSONIAN INST,WHIPPLE OBSERV,WASHINGTON,DC 20560. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 53 TC 125 Z9 125 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 10 PY 1993 VL 404 IS 1 BP 333 EP 347 DI 10.1086/172283 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KK912 UT WOS:A1993KK91200031 ER PT J AU DOMINIK, J STANLEY, DJ AF DOMINIK, J STANLEY, DJ TI BORON, BERYLLIUM AND SULFUR IN HOLOCENE SEDIMENTS AND PEATS OF THE NILE DELTA, EGYPT - THEIR USE AS INDICATORS OF SALINITY AND CLIMATE SO CHEMICAL GEOLOGY LA English DT Article ID LATE QUATERNARY; ENVIRONMENTS; SEQUENCES; SYSTEMS; SWAMP; COAL AB The concentrations of 14 major and trace elements (B, Ba, Be, Co, Cr, Cu, Fe, Mn, Ni, P, S, V, Zn and organic C) in bulk sediment samples of Holocene age from bore holes in the Nile delta, Egypt, are considered in terms of sediment grain size and depositional setting. Using this background information, an attempt is made to evaluate paleosalinity and paleoclimatic change by geochemical analyses of peats. In every sediment facies examined, we find that grain size is a major controlling factor of geochemical composition, but the B/Be ratio is helpful in paleoenvironmental interpretations. Organic-matter content is the major factor affecting element concentrations in peats. Zn, Cr, Fe, Be, Cu, Mn concentrations on an organic-matter-free basis are lower in these organic-rich layers than in other Nile delta sediment facies. The sulfur content of the peats indicates a decreased importance of freshwater input to Holocene lagoons from about 8000 to 3400 years BP. High boron/beryllium ratios and the presence of gypsum in peats deposited between 6300 and 4900 years BP record the most evaporitic phase affecting this region. This geochemical finding is in close agreement with results of other independent paleoclimatic studies which indicate the onset of arid conditions in northeast Africa at about 5000 years BP. C1 SMITHSONIAN INST,NMNH,MEDITERRANEAN BASIN,WASHINGTON,DC 20560. RP DOMINIK, J (reprint author), UNIV GENEVA,INST F A FOREL,ROUTE SUISSE,CH-1290 VERSOIX,SWITZERLAND. NR 40 TC 36 Z9 39 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0009-2541 J9 CHEM GEOL JI Chem. Geol. PD FEB 10 PY 1993 VL 104 IS 1-4 BP 203 EP 216 DI 10.1016/0009-2541(93)90151-8 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA KP493 UT WOS:A1993KP49300012 ER PT J AU BLUNDELL, R PAPA, DC BROWN, ER PARKER, CD AF BLUNDELL, R PAPA, DC BROWN, ER PARKER, CD TI RESONANT-TUNNELING DIODE OSCILLATOR AS AN ALTERNATIVE LO FOR SIS RECEIVER APPLICATIONS SO ELECTRONICS LETTERS LA English DT Article DE OSCILLATORS; TUNNEL DIODES; SUPERCONDUCTING DEVICES AB The resonant tunnelling diode (RTD) oscillator has been demonstrated for the first time as a local oscillator (LO) in a heterodyne receiver. Noise measurements made on a sensitive 200 GHz superconductor-insulator-superconductor receiver using both a multiplied Gunn diode and an RTD oscillator as the LO revealed no difference in receiver noise as a function of oscillator type. C1 MIT,LINCOLN LAB,LEXINGTON,MA 02173. RP BLUNDELL, R (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 9 TC 9 Z9 9 U1 0 U2 1 PU IEE-INST ELEC ENG PI HERTFORD PA MICHAEL FARADAY HOUSE SIX HILLS WAY STEVENAGE, HERTFORD, ENGLAND SG1 2AY SN 0013-5194 J9 ELECTRON LETT JI Electron. Lett. PD FEB 4 PY 1993 VL 29 IS 3 BP 288 EP 290 DI 10.1049/el:19930197 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA LB764 UT WOS:A1993LB76400027 ER PT J AU POST, RC AF POST, RC TI INNOVATION AS A SOCIAL-PROCESS - THOMSON,ELIHU AND THE RISE OF GENERAL-ELECTRIC, 1870-1900 - CARLSON,WB SO AMERICAN HISTORICAL REVIEW LA English DT Book Review RP POST, RC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU AMER HISTORICAL REVIEW PI WASHINGTON PA 400 A ST SE, WASHINGTON, DC 20003 SN 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD FEB PY 1993 VL 98 IS 1 BP 258 EP 258 DI 10.2307/2166554 PG 1 WC History SC History GA KN839 UT WOS:A1993KN83900182 ER PT J AU SNOW, AA SPIRA, TP AF SNOW, AA SPIRA, TP TI INDIVIDUAL VARIATION IN THE VIGOR OF SELF POLLEN AND SELF-FED PROGENY IN HIBISCUS-MOSCHEUTOS (MALVACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article ID TUBE GROWTH; CHAMAECRISTA-FASCICULATA; NONRANDOM FERTILIZATION; INBREEDING DEPRESSION; AMSINCKIA-GRANDIFLORA; SEXUAL SELECTION; INCOMPATIBILITY; CONSEQUENCES; PLANTS AB In some self-compatible species, self pollen tubes grow more slowly than outcross pollen, presumably leading to low selfing rates when mixtures of self and outcross pollen reach the stigma simultaneously. Here we show that the competitive ability of self pollen differed among individuals of Hibiscus moscheutos. Self pollen tubes grew slower than outcross pollen in three plants, faster than outcross pollen in four plants, and showed no difference in five other plants (based on rates of callose plug formation). Levels of inbreeding depression were examined by comparing progeny from self and outcross pollinations in seven maternal families. Self pollination led to reduced seed number in only one maternal family, and a slight decrease in seed size was seen in two maternal families. Considerable inbreeding depression occurred later in the life cycle, and the degree of inbreeding depression varied among maternal families of 6-week-old plants. Our results demonstrate the potential for unpredictable effects of pollen competition on individual selfing rates, which in turn may affect progeny vigor. This complex situation contrasts with previous reports of species in which outcross pollen consistently outcompetes self pollen (cryptic self-incompatibility). C1 UNIV MICHIGAN,BIOL STN,PELLSTON,MI 49769. GEORGIA SO UNIV,DEPT BIOL,STATESBORO,GA 30460. SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. RP SNOW, AA (reprint author), OHIO STATE UNIV,DEPT PLANT BIOL,COLUMBUS,OH 43210, USA. NR 25 TC 33 Z9 35 U1 0 U2 9 PU BOTANICAL SOC AMER INC PI COLUMBUS PA OHIO STATE UNIV-DEPT BOTANY 1735 NEIL AVE, COLUMBUS, OH 43210 SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD FEB PY 1993 VL 80 IS 2 BP 160 EP 164 DI 10.2307/2445035 PG 5 WC Plant Sciences SC Plant Sciences GA KM635 UT WOS:A1993KM63500007 ER PT J AU GLINSMAN, LA HAYEK, LC AF GLINSMAN, LA HAYEK, LC TI A MULTIVARIATE-ANALYSIS OF RENAISSANCE PORTRAIT MEDALS - AN EXPANDED NOMENCLATURE FOR DEFINING ALLOY COMPOSITION SO ARCHAEOMETRY LA English DT Article DE ITALIAN; RENAISSANCE; PORTRAIT MEDAL; X-RAY FLUORESCENCE; DISCRIMINANT ANALYSIS; ALLOY COMPOSITION; NOMENCLATURE AB This study gathered and reported compositional and descriptive analyses of over 200 Italian Renaissance portrait medals in the collection of the National Gallery of Art, Washington. A statistical model was developed for allocation of these medals into meaningful assemblages, using the surface alloy composition, and an expanded nomenclature was formulated. Copper zinc, tin and lead were the primary elements found to combine to form a wide range of alloys. Common impurities were discovered to be significantly lower in the sixteenth-century medals when compared with those in the fifteenth-century medals. Renaissance medallists had an extensive knowledge of metallurgy and could produce a variety of alloys without the use of modern technology. C1 SMITHSONIAN INST,WASHINGTON,DC 20560. RP GLINSMAN, LA (reprint author), NATL GALLERY ART,WASHINGTON,DC 20565, USA. NR 24 TC 8 Z9 8 U1 0 U2 0 PU OXFORD UNIV PI OXFORD PA RES LAB ARCHAEOL HIST ART 6 KEBLE RD, OXFORD, ENGLAND OX1 3QJ SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD FEB PY 1993 VL 35 BP 49 EP 67 DI 10.1111/j.1475-4754.1993.tb01023.x PN 1 PG 19 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA MJ820 UT WOS:A1993MJ82000005 ER PT J AU KENT, SM RAMELLA, M NONINO, M AF KENT, SM RAMELLA, M NONINO, M TI A SMALL DRIFT SCAN SURVEY FOR GALAXIES IN THE NORTHERN SKY SO ASTRONOMICAL JOURNAL LA English DT Article ID UNIVERSE; CATALOG AB CCD photometry has been obtained for 1054 galaxies to a limiting magnitude r(W) = 18.0 in a narrow strip of the sky 12' wide by 60-degrees long. The data are being used to calibrate photographic photometry as part of a parallel redshift survey, but can also be used to study the projected distribution of galaxies on large angular scales free from systematic effects that are present in photographic surveys. Fluctuations in the number density of order 20% are seen on angular scales of 5-degrees and apparently correlate with the distribution of Abell Clusters that lie within 2-degrees of the strip. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. OSSERV ASTRON TRIESTE,I-34131 TRIESTE,ITALY. RP KENT, SM (reprint author), FERMILAB NATL ACCELERATOR LAB,MS 127,POB 500,BATAVIA,IL 60510, USA. OI Nonino, Mario/0000-0001-6342-9662 NR 15 TC 9 Z9 9 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 1993 VL 105 IS 2 BP 393 EP 408 DI 10.1086/116438 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KK747 UT WOS:A1993KK74700001 ER PT J AU HAZEN, ML AF HAZEN, ML TI THE VARIABLE-STARS IN THE GLOBULAR-CLUSTER NGC-6642 SO ASTRONOMICAL JOURNAL LA English DT Article ID OOSTERHOFF PERIOD GROUPS; AGE; SYSTEM AB Photometry is presented for sixteen new and two previously discovered variables within the tidal radius of NGC 6642, and for eight new and three previously known variables outside the tidal radius. Of the former, ten have well-determined periods, indicating that they are RR Lyrae stars, and an additional seven are also probable RR Lyraes; most of these seem likely to be members of the cluster. An apparent visual distance modulus for NGC 6642 of 15.6 +/- 0.4 mag is derived. This value is 0.8 mag larger than the previous estimates. The RRc stars in the cluster show period shifts appropriate to its metallicity; the RRab stars show shifts corresponding to a somewhat lower metallicity. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 17 TC 3 Z9 3 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0004-6256 J9 ASTRON J JI Astron. J. PD FEB PY 1993 VL 105 IS 2 BP 557 EP 562 DI 10.1086/116452 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KK747 UT WOS:A1993KK74700015 ER PT J AU WALLINGTON, S NARAYAN, R AF WALLINGTON, S NARAYAN, R TI THE INFLUENCE OF CORE RADIUS ON GRAVITATIONAL LENSING BY ELLIPTIC LENSES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, FUNDAMENTAL PARAMETERS; GRAVITATIONAL LENSING; QUASARS, GENERAL ID MULTIPLY IMAGED QUASARS; DARK MATTER; POTENTIAL WELLS; SYSTEM 2016+112; GALAXIES; OBJECTS; STATISTICS; DISTRIBUTIONS; AO-0235+164; EVOLUTION AB We model a galaxy lens by means of a simple analytical potential with three parameters: velocity dispersion, ellipticity, and core radius. We compute lensing cross sections for a wide range of these parameters and integrate over the distributions of velocity dispersion and ellipticity appropriate to galaxies. The model predictions are in good agreement with the observations. The number of lensed quasars as a function of apparent magnitude and the relative numbers of doubly imaged and quadruply imaged quasars are predicted satisfactorily. Magnification bias is found to be extremely large at bright magnitudes, particularly for quadruply imaged configurations. The presence of an even number of images in nearly all examples of multiply imaged quasars discovered so far, despite the odd number expected theoretically, can be explained through demagnification of an image in the core of the lens. This requires lens core radii to be smaller than about 200 pc. RP WALLINGTON, S (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 48 TC 88 Z9 88 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1993 VL 403 IS 2 BP 517 EP 529 DI 10.1086/172222 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KJ468 UT WOS:A1993KJ46800008 ER PT J AU PIRAN, T SHEMI, A AF PIRAN, T SHEMI, A TI FIREBALLS IN THE GALACTIC HALO AND GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA RAYS, BURSTS AB If gamma-ray burst sources are in the Galactic halo, they inevitably involve the creation of an opaque pair plasma fireball, just like in cosmological sources. We find that the typical physical conditions in a Galactic halo fireball are optical depth almost-equal-to 10(8), thermal energy almost-equal-to 100 keV, maximal relativistic expansion GAMMA almost-equal-to 300, and a maximal baryonic load of almost-equal-to 10(-15) M. This does not rule out Galactic halo models, but it poses an additional severe constraint on all such sources. A comparison of these conditions with the physical conditions at cosmological fireballs reveal that Galactic halo fireballs are less favorable than cosmological ones as sources of gamma-ray bursts. C1 TEL AVIV UNIV,DEPT PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. HEBREW UNIV JERUSALEM,RACAH INST PHYS,JERUSALEM,ISRAEL. RP PIRAN, T (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 19 TC 38 Z9 39 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD FEB 1 PY 1993 VL 403 IS 2 BP L67 EP L69 DI 10.1086/186723 PN 2 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KJ470 UT WOS:A1993KJ47000005 ER PT J AU JOYCE, FJ AF JOYCE, FJ TI NESTING SUCCESS OF RUFOUS-NAPED WRENS (CAMPYLORHYNCHUS-RUFINUCHA) IS GREATER NEAR WASP NESTS SO BEHAVIORAL ECOLOGY AND SOCIOBIOLOGY LA English DT Article ID BICOLORED WREN; ENHANCEMENT AB Rufous-naped wrens (Campylorhynchus rufinucha) in northwestern Costa Rica build breeding nests most frequently in ant-acacia trees (Acacia collinsii) and occasionally near wasp nests in ant-acacia trees. By moving occupied wasp nests (Polybia rejecta) to randomly chosen ant-acacia trees with wren nests, I tested the hypothesis that wrens nesting near wasp nests were more likely to fledge young than wrens not nesting near wasp nests. Wrens whose nests were near experimentally relocated wasp nests were significantly more likely to fledge young (37.5% of 16 attempts in 1987 and 75% of 12 attempts in 1988) than were wrens whose nests had no wasp nests placed near them (0% of 16 attempts in 1987 and 20% of 15 attempts in 1988). In 15 cases, repeated nesting attempts occurred in the same trees both with and without experimentally-placed wasp nests. Analysis of these data allowed a comparison of the effect of wasp nests on fledging success while differences among trees were controlled. Within the same tree, nesting attempts associated with wasp nests were significantly more likely to fledge young than nesting attempts without wasp nests. Predation was the primary cause of nest failure, and within forest, white-faced monkeys (Cebus capucinus) were the most important predators. The difference in success of wren nests with and without wasps and observations of predators indicate that enhancement of fledging success was due to deterrence of predatory vertebrates by wasps. C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. NR 44 TC 25 Z9 25 U1 0 U2 7 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0340-5443 J9 BEHAV ECOL SOCIOBIOL JI Behav. Ecol. Sociobiol. PD FEB PY 1993 VL 32 IS 2 BP 71 EP 77 DI 10.1007/BF00164038 PG 7 WC Behavioral Sciences; Ecology; Zoology SC Behavioral Sciences; Environmental Sciences & Ecology; Zoology GA KL513 UT WOS:A1993KL51300001 ER PT J AU PARKER, GG HILL, SM KUEHNEL, LA AF PARKER, GG HILL, SM KUEHNEL, LA TI DECLINE OF UNDERSTORY AMERICAN CHESTNUT (CASTANEA-DENTATA) IN A SOUTHERN APPALACHIAN FOREST SO CANADIAN JOURNAL OF FOREST RESEARCH-REVUE CANADIENNE DE RECHERCHE FORESTIERE LA English DT Article ID MARSH BORKH; BLIGHT; VIRGINIA AB Formerly numerous understory stems of American chestnut (Castanea dentata (Marsh.) Borkh.) showed a precipitous decline in a 3-ha stem-mapped permanent plot in southwestern Virginia, United States. More than 64% of the understory chestnut stems died between 1982 and 1988; recruitment of new stems was less than 3% of initial stem numbers. Per capita mortality of chestnut was nearly three times that of all other species combined; the growth rate of surviving chestnut was slightly less than that of similarly sized stems of other species. Basal area increase of surviving stems did not compensate for a nearly 13% decline in basal area from dying stems. On a small spatial scale, chestnut stems were distributed in clusters generally 1 m in extent, having as many as five live individuals. Over 53% of these clusters disappeared, and only a few (1.2%) new clusters appeared in the intercensus interval. The probability of stem death appears to have been random in space. Chestnut mortality was probably not related to the ingrowth of potential competitors. Rather, the decline is likely to have been promoted by an interaction between the continuing action of the chestnut blight (Cryphonectria parasitica (Murr.) Barr) and severe drought in the growing seasons between censuses. C1 VIRGINIA POLYTECH INST & STATE UNIV,DEPT BIOL,BLACKSBURG,VA 24061. RP PARKER, GG (reprint author), SMITHSONIAN ENVIRONM RES CTR,POB 28,EDGEWATER,MD 21037, USA. OI Parker, Geoffrey/0000-0001-7055-6491 NR 24 TC 12 Z9 13 U1 0 U2 9 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA ON K1A 0R6, CANADA SN 0045-5067 J9 CAN J FOREST RES JI Can. J. For. Res.-Rev. Can. Rech. For. PD FEB PY 1993 VL 23 IS 2 BP 259 EP 265 DI 10.1139/x93-035 PG 7 WC Forestry SC Forestry GA KT108 UT WOS:A1993KT10800018 ER PT J AU SCHOLZ, TT AF SCHOLZ, TT TI AVERAGING OF PSEUDORESONANT T-MATRIX ELEMENTS SO COMPUTER PHYSICS COMMUNICATIONS LA English DT Software Review DE INTERMEDIATE ENERGY SCATTERING; ELECTRON ATOM; PSEUDORESONANCES; T-MATRIX AVERAGING; CONVOLUTION; LEAST SQUARES CUBIC SPLINE FIT ID 1S-2P CROSS-SECTIONS; INTERMEDIATE ENERGIES; ELECTRON-SCATTERING; ATOMIC-HYDROGEN AB A program designed to average over pseudoresonances and produce a physically accurate T-matrix element is presented. The pseudoresonant matrix element arises in variational calculations of intermediate energy electron and positron scattering by atoms and molecules. Only their averaged values have physical meaning. The program first removes the dominant pseudoresonant structure by convolution with a Lorentzian and then performs a least squares cubic spline fit to generate the physically smooth result. RP SCHOLZ, TT (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,ITAMP,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 8 TC 1 Z9 1 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0010-4655 J9 COMPUT PHYS COMMUN JI Comput. Phys. Commun. PD FEB PY 1993 VL 74 IS 2 BP 256 EP 264 DI 10.1016/0010-4655(93)90096-U PG 9 WC Computer Science, Interdisciplinary Applications; Physics, Mathematical SC Computer Science; Physics GA KM822 UT WOS:A1993KM82200011 ER PT J AU ERWIN, DH AF ERWIN, DH TI INVERTEBRATE PALEONTOLOGY SO GEOTIMES LA English DT Article RP ERWIN, DH (reprint author), SMITHSONIAN INST,DEPT PALEOBIOL,NAT HIST BLDG 121,WASHINGTON,DC 20560, USA. RI Erwin, Douglas/A-9668-2009 NR 0 TC 0 Z9 0 U1 0 U2 1 PU AMER GEOLOGICAL INST PI ALEXANDRIA PA 4220 KING ST, ALEXANDRIA, VA 22302-1507 SN 0016-8556 J9 GEOTIMES JI Geotimes PD FEB PY 1993 VL 38 IS 2 BP 25 EP 25 PG 1 WC Geosciences, Multidisciplinary SC Geology GA KL388 UT WOS:A1993KL38800025 ER PT J AU JOHNSTON, PF AF JOHNSTON, PF TI TREASURE SALVAGE, ARCHAEOLOGICAL ETHICS AND MARITIME MUSEUMS SO INTERNATIONAL JOURNAL OF NAUTICAL ARCHAEOLOGY LA English DT Article; Proceedings Paper CT 10TH ANNUAL CONF OF THE AUSTRALIAN INST FOR MARITIME ARCHAEOLOGY CY SEP 25, 1991 CL ADELAIDE, AUSTRALIA SP AUSTR INST MARITIME ARCHAEOL RP JOHNSTON, PF (reprint author), SMITHSONIAN INST,NMAH 5010 MRC 628,WASHINGTON,DC 20560, USA. NR 22 TC 5 Z9 5 U1 1 U2 5 PU ACADEMIC PRESS LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0305-7445 J9 INT J NAUT ARCHAEOL JI Int. J. Naut. Archaeol. PD FEB PY 1993 VL 22 IS 1 BP 53 EP 60 DI 10.1111/j.1095-9270.1993.tb00391.x PG 8 WC Archaeology SC Archaeology GA LB772 UT WOS:A1993LB77200004 ER PT J AU HANSON, RB SORENSEN, SS BARTON, MD FISKE, RS AF HANSON, RB SORENSEN, SS BARTON, MD FISKE, RS TI LONG-TERM EVOLUTION OF FLUID ROCK INTERACTIONS IN MAGMATIC ARCS - EVIDENCE FROM THE RITTER RANGE PENDANT, SIERRA-NEVADA, CALIFORNIA, AND NUMERICAL MODELING SO JOURNAL OF PETROLOGY LA English DT Review ID PRESSURE METAMORPHIC BELTS; MID-OCEAN RIDGES; REGIONAL METAMORPHISM; HYDROTHERMAL SYSTEMS; ISOTOPIC FRACTIONATION; CONTACT-METAMORPHISM; TRANSPORT PHENOMENA; MINERAL REACTIONS; PHASE-EQUILIBRIA; EAST GREENLAND AB A record of > 100 million years of fluid flow, alteration, and metamorphism in the evolving Sierra Nevada magmatic arc is preserved in metavolcanic rocks of the Ritter Range pendant and surrounding granitoids. The metavolcanic rocks consist of. (1) a lower section of mostly marine volcaniclastic rocks, lavas, and intercalated carbonate rocks that is Triassic to Jurassic in age, and (2) an upper section comprising a subaerial caldera-fill complex of mid-Cretaceous age. Late Cretaceous high-temperature contact metamorphism (approximately 2 kbar, > 450-500-degrees-C) occurred after renewed normal faulting along the caldera-bounding fault system juxtaposed the two sections. The style and degree of alteration and deltaO-18 values differ among the rocks of the upper and lower sections and the granitoids. Rocks of the lower section show pervasive lithologically controlled alkali alteration, local Mn and Mg enrichment, and oxidation. Some ash flow tuffs now contain up to 10% K2O by weight. The rocks of the upper section show lesser extents of alkali alteration. Granitoids that cut both sections are generally unaltered. Most metavolcanic rocks of the lower section have high deltaO-18 values (+ 11 to + 16 parts per thousand; whole rock and quartz phenocrysts), however, lower-section rocks within the caldera-bounding fault system have low deltaO-18 values of + 4 to + 7 parts per thousand. The metavolcanic rocks of the upper section also have low deltaO-18 values of + 2 to + 7 parts per thousand. Granitoids have deltaO-18 values of + 7 to + 10 parts per thousand, typical of unaltered Sierran granitoids. The lower section contains discontinuous veins of high-temperature (450-500-degrees-C) calc-silicate minerals. These veins are typically < 5 m long, do not cross intrusive contacts, and postdate the pervasive alkali alteration. Late veins are typically > 10 m long, formed at temperatures of less than 450-500-degrees-C, and cross intrusive contacts. Veins have similar deltaO-18 values to those of the local host rocks. The nature of the alteration and the high oxygen isotopic values of the rocks of the lower section indicate that these rocks interacted extensively with seawater at temperatures < 300-degrees-C, probably in superposed marine hydrothermal systems associated with coeval volcanic centers. Metavolcanic rocks of the upper section evidently interacted with meteoric waters, probably in a hydrothermal system associated with the Cretaceous caldera; rocks of the lower section that were adjacent to the caldera were also affected by this alteration. The preservation of the signatures of these earlier events, the nature of the early veins, and results from numerical models of hydrothermal flow that include fluid production indicate that during prograde contact metamorphism, the rocks of the pendant primarily interacted with locally derived fluids. Fluid flow was predominantly upward and away from intrusive contacts and down-temperature. Permeabilities are estimated to have been between 0.1 and 1 muD, which is that necessary for maintenance of lithostatic fluid pressures. In hydrothermal models with such permeabilities, large-scale circulation of meteoric fluids develops after prograde metamorphism ceases. The nature of the late veins in the Ritter Range pendant suggests that such a flow pattern evolved only after the pendant and granitoids had cooled below 450-500-degrees-C. The long-term history of alteration documented in the Ritter Range pendant is probably typical of wall rocks in most batholiths. C1 SMITHSONIAN INST, DEPT MINERAL SCI, WASHINGTON, DC 20560 USA. UNIV CALIF LOS ANGELES, DEPT EARTH & SPACE SCI, LOS ANGELES, CA 90024 USA. NR 103 TC 35 Z9 35 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-3530 J9 J PETROL JI J. Petrol. PD FEB PY 1993 VL 34 IS 1 BP 23 EP 62 PG 40 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA KU095 UT WOS:A1993KU09500002 ER PT J AU FAUST, MA AF FAUST, MA TI PROROCENTRUM-BELIZEANUM, PROROCENTRUM-ELEGANS, AND PROROCENTRUM-CARIBBAEUM, 3 NEW BENTHIC SPECIES (DINOPHYCEAE) FROM A MANGROVE ISLAND, TWIN-CAYS, BELIZE SO JOURNAL OF PHYCOLOGY LA English DT Article ID PYRROPHYTA; NOV AB Three new benthic dinoflagellate species, Prorocentrum belizeanum, Prorocentrum elegans, and Prorocentrum caribbaeum, from mangrove floating detritus are described from scanning electron micrographs. Species were identified based on shape, size, surface micromorphology, ornamentation of thecal plates, and architecture of the periflagellar area and intercalary band. Cells of P. belizeanum are round to slightly oval with a cell size of 55-60 mum long and 50-55 mum wide. Areolae are round and numerous (853-1024 per valve) and range from 0.66 to 0.83 mum in size. The periflagellar area of P. belizeanum is a broad V-shaped depression; it accommodates a flagellar and an auxiliary pore and a flared, curved apical collar. The intercalary band of P. belizeanum is horizontally striated. Prorocentrum elegans is a small species 15-20 mum long and 10-14 mum wide, with an ovate cell shape. The thecal surface is smooth. Two sizes of valve pores were recognized: large, round pores (20-22 per valve) arranged in a distinct pattern and smaller pores situated in an array along the intercalary band. The periflagellar area is V-shaped; it accommodates an uneven sized flagellar pore, an auxiliary pore, and an angled protuberant flagellar plate. The intercalary band is transversely striated. It is a bloom-forming species. Prorocentrum caribbaeum cells are heart-shaped with a rounded anterior end and a pointed posterior end. Cells range from 40 to 45 mum long and 30 to 35 mum wide. Thecal surface has two different-sized pores: large, round pores (145-203 per valve) arranged perpendicularly from the posterior margins, and small, round pores unevenly distributed on the thecal surface. The periflagellar area is ornate. It is V-shaped with a curved apical collar located next to the auxiliary pore; a smaller protuberant apical plate is adjacent to the flagellar pore. The intercalary band is transversely striated and sinuous. Cells are active swimmers. RP FAUST, MA (reprint author), SMITHSONIAN INST,NATL MUSEUM NAT HIST,DEPT BOT,4201 SILVER HALL RD,SUITLAND,MD 20746, USA. NR 28 TC 42 Z9 45 U1 0 U2 2 PU PHYCOLOGICAL SOC AMER INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD FEB PY 1993 VL 29 IS 1 BP 100 EP 107 DI 10.1111/j.1529-8817.1993.tb00287.x PG 8 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA KP046 UT WOS:A1993KP04600015 ER PT J AU ZEH, DW MAY, CA COFFROTH, MA BERMINGHAM, E AF ZEH, DW MAY, CA COFFROTH, MA BERMINGHAM, E TI MBOI AND MACROHALTICA - QUALITY OF DNA FINGERPRINTS IS STRONGLY ENZYME-DEPENDENT IN AN INSECT (COLEOPTERA) SO MOLECULAR ECOLOGY LA English DT Note DE DNA FINGERPRINTING; MACROHALTICA-JAMAICENSIS; 33.15; 33.6; (CCAT); INSECT C1 SMITHSONIAN TROP RES INST,BALBOA,PANAMA. UNIV NOTTINGHAM HOSP,QUEENS MED CTR,DEPT GENET,NOTTINGHAM NG7 2UH,ENGLAND. SUNY BUFFALO,DEPT BIOL SCI,BUFFALO,NY 14260. NR 10 TC 5 Z9 6 U1 0 U2 0 PU BLACKWELL SCIENCE LTD PI OXFORD PA OSNEY MEAD, OXFORD, OXON, ENGLAND OX2 0EL SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD FEB PY 1993 VL 2 IS 1 BP 61 EP 63 DI 10.1111/j.1365-294X.1993.tb00100.x PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA KU837 UT WOS:A1993KU83700008 ER PT J AU DILLENBURG, LR WHIGHAM, DF TERAMURA, AH FORSETH, IN AF DILLENBURG, LR WHIGHAM, DF TERAMURA, AH FORSETH, IN TI EFFECTS OF BELOWGROUND AND ABOVEGROUND COMPETITION FROM THE VINES LONICERA-JAPONICA AND PARTHENOCISSUS-QUINQUEFOLIA ON THE GROWTH OF THE TREE HOST LIQUIDAMBAR-STYRACIFLUA SO OECOLOGIA LA English DT Article DE VINES; ABOVEGROUND AND BELOWGROUND COMPETITION; LONICERA-JAPONICA; PARTHENOCISSUS-QUINQUEFOLIA; LIQUIDAMBAR-STYRACIFLUA ID ROOT COMPETITION; NITROGEN NUTRITION; SEEDLINGS; RESPONSES; PLANTS; STRESS AB Detrimental effects of vines on tree growth in successional environments have been frequently reported. Little is known, however, about the relative importance of below and aboveground competition from vines on tree growth. The objective of this study was to quantify and compare the growth responses of Liquidambar styraciflua saplings to below and/or aboveground competition with the exotic evergreen vine, Lonicera japonica (Japanese honeysuckle), and the native deciduous vine, Parthenocissus quinquefolia (Virginia creeper). Soil trenching and/or vine-trellising were used to control the type of vine competition experienced by trees. Comparisons among untrenched treatments tested for effects of belowground competition, singly or in combination with aboveground competition. Comparisons among trenched treatments tested for effects of aboveground competition. After two growing seasons, Lonicera japonica had a greater effect on the growth of L. styraciflua than did P. quinquefolia. This effect was largely due to root competition, as canopy competition only had a negative effect on tree growth when it occurred in combination with root competition. Leaf expansion was consistently and similarly affected by all treatments which involved belowground competition. C1 SMITHSONIAN ENVIRONM RES CTR,EDGEWATER,MD 21037. UNIV MARYLAND,DEPT BOT,COLL PK,MD 20742. RI Rebello Dillenburg, Lucia /D-9120-2013 NR 46 TC 78 Z9 83 U1 6 U2 25 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0029-8549 J9 OECOLOGIA JI Oecologia PD FEB PY 1993 VL 93 IS 1 BP 48 EP 54 PG 7 WC Ecology SC Environmental Sciences & Ecology GA KL512 UT WOS:A1993KL51200008 PM 28313773 ER PT J AU SUNDARAM, B JENSEN, RV AF SUNDARAM, B JENSEN, RV TI SCARRING AND SUPPRESSION OF IONIZATION IN VERY INTENSE RADIATION-FIELDS SO PHYSICAL REVIEW A LA English DT Article ID HIGH-FREQUENCY; LASER FIELDS; PERIODIC-ORBITS; HYDROGEN-ATOM; STABILIZATION; SUPERINTENSE; STATES; SCARS; INTERFERENCE; REGIME AB The interaction of a model atom with very intense radiation fields is well approximated by a map that describes a free particle being kicked periodically by a double-well potential. Both the classical and quantum versions of the map are studied and are shown to provide a compact description of high-field stabilization in this strongly perturbed quantum system. In particular, we find that the ''stabilized'' wave function results from the excitation of a superposition of eigenstates of the periodic, time-evolution operator that are localized near classically unstable and weakly stable orbits. These ''scarred'' wave functions correspond to localized wave packets that oscillate back and forth in the strong external field while in the neighborhood of the attractive Coulomb field. The periodic bremsstrahlung, emitted as this wave packet passes the nucleus, provides a distinct experimental signature of the stabilized state. C1 WESLEYAN UNIV, DEPT PHYS, MIDDLETOWN, CT 06457 USA. HARVARD SMITHSONIAN CTR ASTROPHYS, INST THEORET ATOM & MOLEC PHYS, CAMBRIDGE, MA 02138 USA. RP SUNDARAM, B (reprint author), JOHNS HOPKINS UNIV, DEPT PHYS & ASTRON, BALTIMORE, MD 21218 USA. RI Sundaram, Bala/A-6532-2010 OI Sundaram, Bala/0000-0002-1728-704X NR 40 TC 36 Z9 36 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 EI 1094-1622 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 1993 VL 47 IS 2 BP 1415 EP 1430 DI 10.1103/PhysRevA.47.1415 PG 16 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA KV979 UT WOS:A1993KV97900086 ER PT J AU JENSEN, RV SUNDARAM, B AF JENSEN, RV SUNDARAM, B TI CLASSICAL-THEORY OF INTENSE-FIELD STABILIZATION SO PHYSICAL REVIEW A LA English DT Note ID FREQUENCY LASER FIELDS; HYDROGEN-ATOM; IONIZATION; SUPERINTENSE; SUPPRESSION; STATES AB A detailed classical analysis of the interaction of an atomic electron with an oscillating electric field with arbitrary initial quantum state n, magnetic quantum number m > 0, field strength, and frequency shows that the classical dynamics for the perturbed electron can be stabilized for large fields or high frequencies. Using a map approximation to the classical dynamics, explicit formulas are derived for the full parameter dependence of the boundaries of stability surrounding the domain of rapid classical ionization. These results provide motivation and guidance for further theoretical and experimental studies of the stabilization of atoms in superintense microwave and laser fields. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. RP JENSEN, RV (reprint author), WESLEYAN UNIV,DEPT PHYS,MIDDLETOWN,CT 06457, USA. RI Sundaram, Bala/A-6532-2010 OI Sundaram, Bala/0000-0002-1728-704X NR 19 TC 20 Z9 20 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD FEB PY 1993 VL 47 IS 2 BP R778 EP R781 DI 10.1103/PhysRevA.47.R778 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA KV979 UT WOS:A1993KV97900010 ER PT J AU HOLBROOK, R KALEDIN, LA KUNC, JA AF HOLBROOK, R KALEDIN, LA KUNC, JA TI PARTITION-FUNCTIONS OF RARE-EARTH-HALIDE PLASMAS SO PHYSICAL REVIEW E LA English DT Article AB The partition functions are calculated for gases consisting of Ln and X atoms and LnX molecules and their singly charged ions (Ln = Dy,Ho,Tm and X = I,Br). C1 MIT,DEPT CHEM,CAMBRIDGE,MA 02139. HARVARD UNIV,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP HOLBROOK, R (reprint author), UNIV SO CALIF,DEPT AEROSP ENGN,LOS ANGELES,CA 90089, USA. NR 30 TC 8 Z9 8 U1 0 U2 3 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1063-651X J9 PHYS REV E JI Phys. Rev. E PD FEB PY 1993 VL 47 IS 2 BP 1285 EP 1298 DI 10.1103/PhysRevE.47.1285 PG 14 WC Physics, Fluids & Plasmas; Physics, Mathematical SC Physics GA KY136 UT WOS:A1993KY13600066 ER PT J AU BODO, G MASSAGLIA, S ROSSI, P TRUSSONI, E FERRARI, A AF BODO, G MASSAGLIA, S ROSSI, P TRUSSONI, E FERRARI, A TI KELVIN-HELMHOLTZ INSTABILITIES IN RADIATING FLOWS SO PHYSICS OF FLUIDS A-FLUID DYNAMICS LA English DT Article ID VORTEX SHEET APPROXIMATION; GALACTIC RADIO-SOURCES; SHEAR-LAYER; BOUNDARY-LAYER; JETS; ASTROPHYSICS; STABILITY; PLASMA AB The linear Kelvin-Helmholtz stability regime of two radiating fluids in relative motion is discussed. The study is carried out in plane geometry and in the vortex-sheet approximation. Attention is focused on the effects of radiation losses on the instability pattern: it is found that the principal effect is the suppression of the cutoff at Mach number M = 2 square-root 2, typical of the adiabatic Kelvin-Helmholtz mode; in particular radiation effects are small on the instability below the cutoff, while they become dominant above. Radiating fluids are also typically affected by thermal instability. In fact thermal modes are found also in the present case: they may have growth rates comparable to the Kelvin-Helmholtz instability above the cutoff. C1 UNIV TURIN,INST FIS GEN,I-10125 TURIN,ITALY. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. UNIV TURIN,IST FIS MATEMAT,I-10123 TURIN,ITALY. RP BODO, G (reprint author), OSSERV ASTRON TORINO,I-10025 PINO TORINESE,ITALY. RI Bodo, Gianluigi/F-9223-2012 OI Bodo, Gianluigi/0000-0002-9265-4081 NR 29 TC 3 Z9 3 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0899-8213 J9 PHYS FLUIDS A-FLUID PD FEB PY 1993 VL 5 IS 2 BP 405 EP 411 DI 10.1063/1.858863 PG 7 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA KJ516 UT WOS:A1993KJ51600012 ER PT J AU FEUILLET, C AF FEUILLET, C TI NOMENCLATURAL SOLUTIONS IN THE GESNERIACEAE SO TAXON LA English DT Article AB Following the rejection of the spelling Jankaea versus Jancaea, a new spelling is given for the name of intergeneric hybrids. A new nothogeneric name, xCoracaea Feuillet, is established, with a new combination, xC bluemelii (Halda) Feuillet. The case of the overlooked generic name Columnea Raf. is presented. The status of Aikinia Wall. vs. Aikinia R. Br. is discussed. Arctocalyx Fenzl and Gesnera Mart. are typified. RP FEUILLET, C (reprint author), SMITHSONIAN INST,DEPT BOT,NHB-166,WASHINGTON,DC 20560, USA. NR 22 TC 0 Z9 0 U1 0 U2 1 PU INT ASSN PLANT TAXONOMY PI BERLIN PA BOTANISCHER GARTEN & MUSEUM KONIGIN-LUISSE-STRASSE 6-8, W-1000 BERLIN, GERMANY SN 0040-0262 J9 TAXON JI Taxon PD FEB PY 1993 VL 42 IS 1 BP 105 EP 109 DI 10.2307/1223313 PG 5 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA KQ948 UT WOS:A1993KQ94800017 ER PT J AU ZIMMER, EA AF ZIMMER, EA TI PATTERNS OF PLANT EVOLUTION INFERRED FROM NUCLEAR GENES SO JOURNAL OF CELLULAR BIOCHEMISTRY LA English DT Meeting Abstract C1 SMITHSONIAN INST,NMNH,MOLEC SYSTEMAT LAB,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0730-2312 J9 J CELL BIOCHEM JI J. Cell. Biochem. PD JAN 26 PY 1993 SU 17B BP 9 EP 9 PG 1 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA KN465 UT WOS:A1993KN46500021 ER PT J AU HERSHKOVITZ, MA ZIMMER, EA AF HERSHKOVITZ, MA ZIMMER, EA TI MOLECULAR STUDIES OF FLORAL MORPHOLOGICAL EVOLUTION SO JOURNAL OF CELLULAR BIOCHEMISTRY LA English DT Meeting Abstract C1 SMITHSONIAN INST,MSC,MOLEC SYSTEMAT LAB,WASHINGTON,DC 20560. RI Zimmer, Elizabeth/G-3890-2011 NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0730-2312 J9 J CELL BIOCHEM JI J. Cell. Biochem. PD JAN 26 PY 1993 SU 17B BP 15 EP 15 PG 1 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA KN465 UT WOS:A1993KN46500039 ER PT J AU WARD, DC AF WARD, DC TI CHANCELLORSVILLE 1863 - THE SOULS OF THE BRAVE - FURGURSON,EB SO NEW YORK TIMES BOOK REVIEW LA English DT Book Review RP WARD, DC (reprint author), SMITHSONIAN INST,WASHINGTON,DC 20560, USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU NEW YORK TIMES PI NEW YORK PA 229 W 43RD ST, NEW YORK, NY 10036-3959 SN 0028-7806 J9 NEW YORK TIMES BK R JI N. Y. Times Book Rev. PD JAN 24 PY 1993 BP 18 EP 18 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA KG626 UT WOS:A1993KG62600027 ER PT J AU KALLMAN, TR WILKES, BJ KROLIK, JH GREEN, R AF KALLMAN, TR WILKES, BJ KROLIK, JH GREEN, R TI CONSISTENCY OF SPHERICAL, GRAVITY-DOMINATED DYNAMICS WITH QUASAR HIGH-IONIZATION EMISSION-LINE PROFILES SO ASTROPHYSICAL JOURNAL LA English DT Article DE QUASARS, EMISSION LINES ID ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT QSOS; STELLAR OBJECTS; SEYFERT-GALAXIES; REGIONS; CLOUDS; SPECTRA; ACCRETION; GAS; SPECTROPHOTOMETRY AB Active galactic nucleus (AGN) emission-line profiles contain much information about the kinematics of the emission-line region. However, despite the large existing spectral data base, relatively little has been one to exploit this potential source of information fully because all existing analytic methods are strongly model-dependent and often involve large numbers of free parameters. In this paper we use line profile data to test a simple kinematic model-spherically symmetric gravitational free fall-in which we limit the number of free parameters by requiring physical self-consistency. The predictions of this model are fitted to high-resolution (1 angstrom) spectra of the stronger rest-frame ultraviolet emission lines in 12 quasars with z congruent-to 2. We find that if all the lines are radiated predominantly from the illuminated faces of the emission-line clouds, the profiles of Lyalpha, N V lambda1240, and C IV lambda1549 can be simultaneously well fitted with very similar parameters for all 12 quasars. However, three points cast doubt on whether this model actually describes the broad emission line regions of these quasars: in some cases, there are no parameter choices which lead to acceptable fits if C III] lambda1909 is added to the fist of predicted fine profiles; the best-fit parameters found for the fits to Lyalpha, N V lambda1240, and C IV lambda1549 are likely not to permit acceptable fits to other lines, once comparable profile data for them become available; finally, our results imply gravitational masses comparable to the most massive known galaxies, together with accretion rates which are likely to exceed known supply mechanisms. We therefore believe that spherically symmetric gravitational free fall does not correctly describe the dynamics of quasar broad emission line regions. Similar efforts applied to other dynamical scenario are likely to result in similarly severe constraints. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. NATL OPT ASTRON OBSERV,KITT PEAK NATL OBSERV,TUCSON,AZ 85726. RP KALLMAN, TR (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,CODE 665,GREENBELT,MD 20771, USA. OI Wilkes, Belinda/0000-0003-1809-2364 NR 51 TC 18 Z9 18 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1993 VL 403 IS 1 BP 45 EP 64 DI 10.1086/172182 PN 1 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KG277 UT WOS:A1993KG27700008 ER PT J AU FIELD, GB ROGERS, RD AF FIELD, GB ROGERS, RD TI RADIATION FROM MAGNETIZED ACCRETION DISKS IN ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; GALAXIES, ACTIVE; RADIATION MECHANISMS, MISCELLANEOUS ID X-RAY-SPECTRA; COMPTON REFLECTION; PAIR PRODUCTION; COLD MATTER; ORIGIN; ACCELERATION; GALAXIES; MODEL AB We present a model of active galactic nuclei (AGNs) based on accretion disks around 10(8) M. black holes, which incorporates a strong (B approximately 10(4) G) magnetic field in the disk, with loops above the disk in which B approximately 10(2) G. The mapetic energy in the loops dissipates, accelerating electrons to relativistic energies. The electrons emit synchrotron and inverse-Compton radiation, much of which is reflected or scattered by gas in the disk. We calculate the emitted spectrum from infrared to gamma rays. Of the total emission, 23% goes into a v-1 power law and 77% into thermal radiation at 24,000 K (due to the disk, which is heated by nonthermal radiation and energetic ions). The model accounts quantitatively for the X-ray and gamma-ray backgrounds, and it accounts qualitatively for certain features observed in individual AGNs: a far-infrared cutoff, a minimum at a few microns, the ultraviolet bump, the Compton reflection bump at approximately 30 keV, and a gamma-ray tail. C1 LAWRENCE LIVERMORE NATL LAB,LIVERMORE,CA 94550. RP FIELD, GB (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 32 TC 87 Z9 87 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1993 VL 403 IS 1 BP 94 EP 109 DI 10.1086/172185 PN 1 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KG277 UT WOS:A1993KG27700011 ER PT J AU CHRISTODOULOU, DM TOHLINE, JE AF CHRISTODOULOU, DM TOHLINE, JE TI DYNAMIC EVOLUTION OF GASEOUS DISKS IN HALO POTENTIALS .1. MASSLESS RINGS IN STATIC, SPHEROIDAL HALOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ISM; GALAXIES, KINEMATICS AND DYNAMICS; HYDRODYNAMICS; METHODS, NUMERICAL ID PREFERRED ORBIT PLANES; CLOUD-FLUID APPROACH; GALACTIC GAS DISKS; TRIAXIAL GALAXIES; POLAR RINGS; ELLIPTICAL GALAXIES; S0 GALAXIES; MODEL; AXIS; ORIENTATION AB We have conducted an experimental study of gaseous galaxy disks that evolve under the influence of an external halo potential. Because our numerical experiments are the first to employ a fully three-dimensional, Eulerian, hydrodynamical computer code, we have chosen the simplest possible initial conditions: the disks are massless and the external potential is either oblate or prolate spheroidal and nontumbling. The outcome and the details of each model's evolution depend critically on the degree of distortion of the halo from spherical symmetry and on the initial inclination of the disk from the equatorial plane of the halo. For small halo distortions and low initial inclinations, the disk identifies the symmetry plane of the halo as the preferred plane and settles to it, developing in the process a warped and twisted structure. As disks with higher initial inclinations are considered, matter inflow to the nuclear region of the potential becomes increasingly important relative to settling toward the preferred plane, and it dominates at moderate inclinations. Highly inclined disks and polar rings are able to survive at their original inclinations for long periods of time while they continuously supply small amounts of gas to the nuclear region. On the other hand, as the quadrupole distortion of the potential increases, the evolutions become progressively more violent at all initial inclinations. Finally, for strong halo distortions, disk evolutions are catastrophic and the dynamics does not involve only the competition between settling and inflow; the models develop extremely distorted structures after only a few rotations. In retrospect, smoothly warped and twisted gaseous disks seen in real galaxies should be at most moderately inclined inside weakly distorted dark halos. Highly inclined and nearly flat rings observed in polar-ring galaxies can be interpreted as transient features that survive because the dark halos around them are only slightly distorted. Because matter inflow does occur during settling, nuclear disks should be a common feature of such evolutions. A nuclear disk that is observed in a galaxy whose outer regions are dominated by a smooth warp should be an indication of a moderately tilted disk that is settling in the presence of only a slightly distorted halo potential. Nuclear disks and enhanced nuclear activity seen in galaxies that are not dominated by smooth warps may reflect moderately strong quadrupole distortions in the underlying potentials. Finally, extreme nuclear activity, disks in a stage of disruption, or even the irregular morphology of some galaxies can be caused by strongly distorted halos. C1 UNIV ARIZONA, STEWARD OBSERV, TUCSON, AZ 85721 USA. LOUISIANA STATE UNIV, DEPT PHYS & ASTRON, BATON ROUGE, LA 70803 USA. RP HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 42 TC 8 Z9 8 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1993 VL 403 IS 1 BP 110 EP 126 DI 10.1086/172186 PN 1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KG277 UT WOS:A1993KG27700012 ER PT J AU KRATZ, KL BITOUZET, JP THIELEMANN, FK MOLLER, P PFEIFFER, B AF KRATZ, KL BITOUZET, JP THIELEMANN, FK MOLLER, P PFEIFFER, B TI ISOTOPIC R-PROCESS ABUNDANCES AND NUCLEAR-STRUCTURE FAR FROM STABILITY - IMPLICATIONS FOR THE R-PROCESS MECHANISM SO ASTROPHYSICAL JOURNAL LA English DT Article DE NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES; SUPERNOVAE, GENERAL ID S-PROCESS NUCLEOSYNTHESIS; BETA-STRENGTH FUNCTIONS; NEUTRON-CAPTURE RATES; DECAY HALF-LIVES; SUPERHEAVY NUCLEI; FISSION BARRIERS; RICH NUCLEI; MODEL; HEAVY; APPROXIMATION AB Attempts to explain the source of r-process elements in nature by particular astrophysical sites face the entwined uncertainties, stemming from the extrapolation of nuclear properties far from stability, inconsistent sources of different properties (e.g., nuclear masses and half-lives), and the (poor) understanding of astrophysical conditions, which are hard to disentangle. We utilize the full isotopic r-process abundances in nature [especially in all of the three peaks (A congruent-to 80, 130, 195)] and a unified model for all nuclear properties involved (aided by recent experimental knowledge in the r-process path), to deduce uniquely the conditions necessary to produce such an abundance pattern. Recent analysis of a few isotopic ratios in the A almost-equal-to 80 and A almost-equal-to 130 r-process peaks led to the conclusion that the r-process abundances originate from a high-density and high-temperature environment, which supports an equilibrium between neutron captures and photodisintegrations. This excludes events where neutrons are released from (alpha, n) reactions in explosive He burning. The present study investigates also the nature of the steady-flow equilibrium of beta decays between isotonic chains. We find strong evidence that a steady flow was not global but only local in between neighboring peaks, which requires time scales not much longer than 1 s. The abundances have to be explained by a superposition of r-process components with varying neutron number densities n(n) > 10(2) cm-3 and temperatures T > 10(9) K, where each of the components proceeds up to one of the peaks. The remaining odd-even effects in observed abundances indicate that neutron densities dropped during freeze-out by orders of magnitude on time scales close to 0.04 s. A set of n(n)-T conditions is presented as a test for any astrophysical r-process site. We also show how remaining deficiencies in the produced abundance pattern can be used to extract nuclear properties far from stability. C1 HARVARD SMITHSONIAN CTR ASTROPHYS, CAMBRIDGE, MA 02138 USA. RP UNIV MAINZ, INST KERNCHEM, FRITZ STRASSMANN WEG 2, W-6500 MAINZ, GERMANY. NR 92 TC 329 Z9 330 U1 2 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JAN 20 PY 1993 VL 403 IS 1 BP 216 EP 238 DI 10.1086/172196 PN 1 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KG277 UT WOS:A1993KG27700022 ER PT J AU MOLLAAGHABABA, R GOTTLIEB, CA THADDEUS, P AF MOLLAAGHABABA, R GOTTLIEB, CA THADDEUS, P TI HYPERFINE-STRUCTURE OF THE SIC RADICAL SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID ELECTRON-SPIN-RESONANCE; PARAMETERS; SPECTRUM; MOLECULES; STATES; 4-K AB The millimeter-wave rotational spectrum of the free (SiC)-Si-29 radical in the X3PI ground state, produced in a low-pressure glow discharge through SiH4 and CO, was detected with the same reactive-molecule spectrometer used earlier to detect SiC and (SiC)-C-13. Eleven rotational transitions, all but two with resolved hyperfine structure, were measured between 195 GHz (J = 4 --> 5) and 372 GHz (J = 8 --> 9). Well-resolved hyperfine splittings in the three fine-structure ladders allow determination of the magnetic hyperfine constants to 2% or better. C1 HARVARD UNIV,DIV APPL SCI,CAMBRIDGE,MA 02138. HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP MOLLAAGHABABA, R (reprint author), HARVARD UNIV,DEPT PHYS,CAMBRIDGE,MA 02138, USA. NR 24 TC 19 Z9 19 U1 0 U2 4 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0021-9606 J9 J CHEM PHYS JI J. Chem. Phys. PD JAN 15 PY 1993 VL 98 IS 2 BP 968 EP 973 DI 10.1063/1.464260 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA KH442 UT WOS:A1993KH44200022 ER PT J AU KUNG, JH AF KUNG, JH TI COMPARISON OF THE SACHS-WOLFE EFFECT FOR GAUSSIAN AND NON-GAUSSIAN FLUCTUATIONS SO PHYSICAL REVIEW D LA English DT Article ID LARGE-SCALE STRUCTURE; COLD DARK MATTER; N-BODY SIMULATIONS; INFLATIONARY UNIVERSE; DENSITY PERTURBATIONS; COSMIC STRINGS; INITIAL CONDITIONS; GALAXY FORMATION; ANISOTROPIES; GENERATION AB A consequence of non-Gaussian perturbations on the Sachs-Wolfe effect is studied. For a particular power.spectrum, predicted Sachs-Wolfe effects are calculated for two cases: a Gaussian (random phase) configuration and a specific kind of non-Gaussian configuration. We obtain the result that the Sachs-Wolfe effect for the latter case is smaller when each temperature fluctuation is properly normalized with respect to the corresponding mass fluctuation (deltaM/M)(R). The physical explanation and the generality of the result are discussed. RP KUNG, JH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 43 TC 3 Z9 3 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD JAN 15 PY 1993 VL 47 IS 2 BP 409 EP 415 DI 10.1103/PhysRevD.47.409 PG 7 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA KG727 UT WOS:A1993KG72700005 ER PT J AU HODGES, HM AF HODGES, HM TI MIRROR BARYONS AS THE DARK MATTER SO PHYSICAL REVIEW D LA English DT Article ID INFLATION; PERTURBATIONS AB A ''parallel world'' with all of the standard particles, which primarily interacts gravitationally with our world, can be motivated via a symmetry principle designed to make a Lagrangian CP symmetric, while maintaining a CP asymmetry in the observable world. Such a symmetry is easily accommodated in grand unified theory models, and may also arise in superstring theories. The cosmological abundance of mirror particles is investigated after a period of chaotic inflation and subsequent reheating. Contrary to previous studies, I find that mirror and ordinary abundances may naturally be similar at the present epoch, and that mirror baryons can provide the closure density without violating nucleosynthesis con straints. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. NR 23 TC 105 Z9 106 U1 0 U2 0 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD JAN 15 PY 1993 VL 47 IS 2 BP 456 EP 459 DI 10.1103/PhysRevD.47.456 PG 4 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA KG727 UT WOS:A1993KG72700009 ER PT J AU PERIVOLAROPOULOS, L AF PERIVOLAROPOULOS, L TI COBE VERSUS COSMIC STRINGS - AN ANALYTICAL MODEL SO PHYSICS LETTERS B LA English DT Article ID EVOLUTION; NETWORKS AB We construct a simple analytical model to study the effects of cosmic strings on the microwave background radiation. Our model is based on counting random multiple impulses inflicted on photon trajectories by the string network between the time of recombination and today. We construct the temperature auto-correlation function and use it to obtain the effective power spectrum index n, the RMS-quadrupole-normalized amplitude Q(RMS-PS) and the RMS temperature variation smoothed on small angular scales. For the values of the scaling solution parameters obtained by Bennett and Bouchet [ Phys. Rev. D 41 ( 1990) 2408] and Allen and Shellard [Phys. Rev. Lett. 64 (1990) 119] we obtain n=1.14+/-0.5, Q(RMS-PS) = (4.5+/-1.5)Gmu and (DELTAT/T)RMS=5.5Gmu. Demanding consistency of these results with the COBE data leads to Gu=(1.7+/-0.7) x 10(-6) (where mu is the string mass per unit length), in good agreement with direct normalizations of mu from observations. RP PERIVOLAROPOULOS, L (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,DIV THEORET ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. OI Perivolaropoulos, Leandros/0000-0001-9330-2371 NR 23 TC 67 Z9 67 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-2693 J9 PHYS LETT B JI Phys. Lett. B PD JAN 14 PY 1993 VL 298 IS 3-4 BP 305 EP 311 DI 10.1016/0370-2693(93)91825-8 PG 7 WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA KJ489 UT WOS:A1993KJ48900010 ER PT J AU WHITNEY, BA HARTMANN, L AF WHITNEY, BA HARTMANN, L TI MODEL SCATTERING ENVELOPES OF YOUNG STELLAR OBJECTS .2. INFALLING ENVELOPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; CIRCUMSTELLAR MATTER; DUST, EXTINCTION; ISM, JETS AND OUTFLOWS; RADIATIVE TRANSFER; STARS, PRE-MAIN-SEQUENCE ID T-TAURI STARS; INFRARED IMAGES; HL-TAURI; CIRCUMSTELLAR DISKS; PROTOSTELLAR DISKS; REFLECTION NEBULAE; BIPOLAR NEBULAE; POLARIZATION; EVOLUTION; CLOUDS AB We present scattered light images for models of young stellar objects surrounded by dusty envelopes. The envelopes are assumed to have finite angular momentum and are falling in steady flow onto a disk. The model envelopes include holes, such as might be created by energetic bipolar flows. We calculate images using the Monte Carlo method to follow the light scattered in the dusty envelope and circumstellar disk, assuming that the photons originate from the central source. Adopting typical interstellar medium dust opacities and expected mass infall rates for protostars M approximately 10(-6) M. yr-1. we find that detectable amounts of optical radiation can escape from envelopes falling into a disk as small as approximately 10-100 AU, depending upon the viewing angle and the size of the bipolar flow cavity. The models explain general features of polarization maps of many young stellar objects. In particular, parallel polarization patterns ('' polarization disks '') can be produced by multiple scattering effects very simply in envelopes and do not require large-scale disk structure. We suggest that the extended optical and near-IR light observed around several young stars is scattered by dusty infalling envelopes rather than disks. RP WHITNEY, BA (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 52 TC 175 Z9 176 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1993 VL 402 IS 2 BP 605 EP 622 DI 10.1086/172163 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KG271 UT WOS:A1993KG27100025 ER PT J AU CALVET, N HARTMANN, L KENYON, SJ AF CALVET, N HARTMANN, L KENYON, SJ TI MASS-LOSS FROM PREMAIN-SEQUENCE ACCRETION DISKS .1. THE ACCELERATING WIND OF FU ORIONIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; STARS, MASS LOSS; STARS, PRE-MAIN-SEQUENCE ID YOUNG STELLAR OBJECTS; T-TAURI STARS; EVOLUTION; JETS; VARIABLES; ROTATION; MODELS; ORIGIN; FLOWS AB We present evidence that the wind of the pre-main-sequence object FU Orionis arises from the surface of the luminous accretion disk. A disk wind model calculated assuming radiative equilibrium explains the differential behavior of the observed asymmetric absorption-line profiles. The model predicts that strong lines should be asymmetric and blueshifted, while weak lines should be symmetric and double-peaked due to disk rotation, in agreement with observations. We propose that many blueshifted ''shell'' absorption features are not produced in a true shell of material, but rather form in a differentially expanding wind that is rapidly rotating. The inference of rapid rotation supports the proposal that pre-main-sequence disk winds are rotationally driven. FU Ori may lose substantial amounts of mass over a significant area of the innermost disk (approximately 10 stellar radii), which could have important implications for the structure of jets from young stellar objects. Our results support the suggestion that massive winds originate from rapidly accreting pre-main-sequence accretion disks. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. RP CALVET, N (reprint author), CTR INVEST ASTRON,AP P 264,MERIDA 5101A,VENEZUELA. OI Kenyon, Scott/0000-0003-0214-609X NR 43 TC 73 Z9 73 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1993 VL 402 IS 2 BP 623 EP 634 DI 10.1086/172164 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KG271 UT WOS:A1993KG27100026 ER PT J AU MYERS, PC FULLER, GA AF MYERS, PC FULLER, GA TI GRAVITATIONAL FORMATION TIMES AND STELLAR MASS DISTRIBUTIONS FOR STARS OF MASS 0.3-30 M-CIRCLE-DOT SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, CLOUDS; ISM, MOLECULES; STARS, FORMATION; STARS, LUMINOSITY FUNCTION, MASS FUNCTION ID DENSE CORES; PHOTODISSOCIATION REGION; MOLECULAR CLOUDS; NH3 OBSERVATIONS; DARK CLOUDS; CO SURVEY; NGC-7023 AB The width of the 1.3 cm line of NH3 in a dense core is related by simple power laws to the luminosity and mass of the most massive star associated with the core. These relations link the mass of the star to the initial conditions in the gas which formed the star. At the size scale approximately 0.1 pc of NH3 line observations, the effects of stellar winds on the core velocity dispersion are estimated from observations of cores with and without stars, and from the dependence of the wind momentum flux on stellar luminosity. The estimated wind contribution increases with stellar luminosity, but is generally comparable to or less than the nonstellar contribution to the nonthermal motions, which is probably of magnetic origin. The wind contribution is removed from the observed velocity dispersion to estimate the velocity dispersion in the prestellar core gas. This dispersion is used to estimate the time for a core associated with a star of mass 0.3-30 M. to form such a star. The infall model includes both thermal and nonthermal motions. The nonthermal part of the velocity dispersion in the region which contains one stellar mass of gas is assumed to be bounded by values (a) the same as observed at the radius r(obs), and (b) smaller than observed by a factor (r/r(obs))1/2. The predicted infall times for stars of mass 0.3, 3, and 30 M. are 1-2, 4-8, and 1-12 x 10(5) yr. The range of gravitational formation times is at most a factor of 10, significantly smaller than the factor of 100 in the range of stellar masses. A cloud forming a star cluster can produce a distribution of stellar masses which matches that of the IMF for stars more massive than 2-3 M., provided cores have pressure proportional to that of the underlying cluster cloud, and velocity dispersion related to stellar mass as indicated by NH3 line observations. RP MYERS, PC (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 36 TC 35 Z9 35 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 5720 S WOODLAWN AVE, CHICAGO, IL 60637 SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JAN 10 PY 1993 VL 402 IS 2 BP 635 EP 642 DI 10.1086/172165 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA KG271 UT WOS:A1993KG27100027 ER PT J AU MORAN, JM AF MORAN, JM TI ASTRONOMICAL MASERS - VIOLENT MOTIONS IN GALACTIC CORE SO NATURE LA English DT Editorial Material ID WATER-VAPOR MASER; EMISSION; NUCLEI RP MORAN, JM (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU MACMILLAN MAGAZINES LTD PI LONDON PA PORTERS SOUTH, 4 CRINAN ST, LONDON, ENGLAND N1 9XW SN 0028-0836 J9 NATURE JI Nature PD JAN 7 PY 1993 VL 361 IS 6407 BP 17 EP 18 DI 10.1038/361017a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA KF718 UT WOS:A1993KF71800020 ER PT B AU CONNAUGHTON, V AKERLOF, CW CHANTELL, M FEGAN, DJ FENNELL, S GAIDOS, J HILLAS, AM KERRICK, AD LEWIS, DA MEYER, DI MOHANTY, G ROVERO, A SEMBROSKI, G SCHUBNELL, MS PORTER, NA PUNCH, M WEEKES, TC WHITAKER, T WILSON, C AF CONNAUGHTON, V AKERLOF, CW CHANTELL, M FEGAN, DJ FENNELL, S GAIDOS, J HILLAS, AM KERRICK, AD LEWIS, DA MEYER, DI MOHANTY, G ROVERO, A SEMBROSKI, G SCHUBNELL, MS PORTER, NA PUNCH, M WEEKES, TC WHITAKER, T WILSON, C GP INT UNION PURE & APPL PHYS TI TEV COUNTERPARTS OF GAMMA RAY BURSTS SO 23RD INTERNATIONAL COSMIC RAY CONFERENCE, VOL 1: CONTRIBUTED PAPERS - OG SESSIONS 1-5 LA English DT Proceedings Paper CT 23rd International Cosmic Ray Conference (XXIII ICRC) CY JUL 19-30, 1993 CL CALGARY, CANADA SP INT UNION PURE & APPL PHYS C1 HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,CAMBRIDGE,MA 02138. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALGARY PR PI CALGARY PA 2500 UNIVERSITY DRIVE NW, CALGARY AB T2N 1N4, CANADA PY 1993 BP 112 EP 115 PG 4 WC Astronomy & Astrophysics; Physics, Applied; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BC03S UT WOS:A1993BC03S00029 ER PT B AU JIANG, Y FLEURY, P LEWIS, DA MOHANTY, G PARE, E ROVERO, AC URBAN, M VACANTI, G WEEKES, TC AF JIANG, Y FLEURY, P LEWIS, DA MOHANTY, G PARE, E ROVERO, AC URBAN, M VACANTI, G WEEKES, TC GP INT UNION PURE & APPL PHYS TI ABSOLUTE CALIBRATION OF AN ATMOSPHERIC CHERENKOW TELESCOPE USING MUON RING IMAGES SO 23RD INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: CONTRIBUTED PAPERS - HE SESSIONS LA English DT Proceedings Paper CT 23rd International Cosmic Ray Conference (XXIII ICRC) CY JUL 19-30, 1993 CL CALGARY, CANADA SP INT UNION PURE & APPL PHYS C1 HARVARD SMITHSONIAN CTR ASTROPHYS,WHIPPLE OBSERV,CAMBRIDGE,MA 02138. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALGARY PR PI CALGARY PA 2500 UNIVERSITY DRIVE NW, CALGARY AB T2N 1N4, CANADA PY 1993 BP 662 EP 665 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BC18G UT WOS:A1993BC18G00174 ER PT J AU MAJEWSKI, J AF MAJEWSKI, J GP AMER ASSOC ZOOL PARKS & AQUARIUMS TI SERVING A DIVERSE AUDIENCE - THE ADAS NICHE ON THE LEARNING-CURVE SO AAZPA ANNUAL CONFERENCE PROCEEDINGS 1993 LA English DT Proceedings Paper CT AAZPA Annual Conference CY SEP 12-16, 1993 CL OMAHA, NE SP AMER ASSOC ZOOLOG PARKS & AQUARIUMS C1 SMITHSONIAN INST,WASHINGTON,DC 20560. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC ZOOLOGICAL PARKS & AQUARIUMS PI WHEELING PA OGLEBAY PARK, WHEELING, WV 26003-1698 PY 1993 BP 326 EP 328 PG 3 WC Zoology SC Zoology GA BZ92Q UT WOS:A1993BZ92Q00077 ER PT J AU STANLEY, J AF STANLEY, J TI 3 CONTEMPORARY ETHIOPIANS SO AFRICAN ARTS LA English DT Art Exhibit Review RP STANLEY, J (reprint author), SMITHSONIAN INST,NATL MUSEUM AFRICAN ART LIB,WASHINGTON,DC 20560, USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIF PI LOS ANGELES PA AFRICAN STUDIES CNTR, LOS ANGELES, CA 90024 SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD JAN PY 1993 VL 26 IS 1 BP 76 EP 77 DI 10.2307/3337113 PG 2 WC Art SC Art GA KP609 UT WOS:A1993KP60900011 ER PT J AU KONIGER, M WINTER, K AF KONIGER, M WINTER, K TI GROWTH AND PHOTOSYNTHESIS OF GOSSYPIUM-HIRSUTUM L AT HIGH PHOTON FLUX DENSITIES - EFFECTS OF SOIL TEMPERATURES AND NOCTURNAL AIR TEMPERATURES SO AGRONOMIE LA English DT Article DE GOSSYPIUM-HIRSUTUM = COTTON; GROWTH REDUCTION; NIGHT TEMPERATURE; PHOTOSYNTHESIS; SOIL TEMPERATURE AB Gossypium hirsutum, when grown under both medium (1 000-1 100 mumol m-2 s-1) and high photon flux densities (PFD, 1 800 - 2 000 mumol m-2 s-1) showed reduced total dry weights and total leaf areas with decreasing temperatures during the dark period (25, 15 or 10-degrees-C), while photosynthetic capacity (PS(max)) and quantum yield of photosynthetic O2 evolution (empty set), as well as the light-use efficiency of photosystem II (F(V)/F(M)) were not affected. Maintaining a day/night soil temperature of 25-degrees-C for one set of plants (high PFD, 34-degrees/10-degrees-C) resulted in a 44% increase in total dry weight, an increase in turgor pressure, but no significant change in PS(max). During another set of experiments cotton plants were cultivated at either medium PFD and 20/25-degrees-C (day/night) air temperatures or at high PFD and either 24/25-degrees-C or 34/25-degrees-C air temperatures. The soil temperatures were maintained independent of the air temperatures at either 20-degrees or 30-degrees-C. Cultivating the plants at a soil temperature of 30-degrees rather than 20-degrees-C resulted in large percentage increases in total dry weight (28-55%), but did not have any impact on F(V)/F(M) and the pigment content of the leaves. The importance of night and rhizosphere temperatures for plant growth and development are discussed. RP KONIGER, M (reprint author), SMITHSONIAN TROP RES INST,POB 2072,BALBOA,PANAMA. NR 0 TC 6 Z9 6 U1 1 U2 1 PU EDITIONS SCIENTIFIQUES ELSEVIER PI PARIS CEDEX 15 PA 141 RUE JAVEL, 75747 PARIS CEDEX 15, FRANCE SN 0249-5627 J9 AGRONOMIE JI Agronomie PY 1993 VL 13 IS 5 BP 423 EP 431 DI 10.1051/agro:19930507 PG 9 WC Agronomy SC Agriculture GA LY521 UT WOS:A1993LY52100007 ER PT J AU BLACKMAN, MJ STEIN, GJ VANDIVER, PB AF BLACKMAN, MJ STEIN, GJ VANDIVER, PB TI THE STANDARDIZATION HYPOTHESIS AND CERAMIC MASS-PRODUCTION - TECHNOLOGICAL, COMPOSITIONAL, AND METRIC INDEXES OF CRAFT SPECIALIZATION AT TELL LEILAN, SYRIA SO AMERICAN ANTIQUITY LA English DT Article ID POTTERY; EXCHANGE AB Archaeologists often use measurements of standardization in ceramics as evidence for specialized craft Production. Analysis of fine-ware bowl kiln wasters from the urban center of Leilan, Syria (ca. 2300 B.C.) provides a rare opportunity to test the standardization hypothesis against the archaeological record of a single production event. Scanning-electron microscopy, xeroradiography, neutron activation, and metric analyses of the wasters show extreme uniformity in manufacturing technology, chemical composition, and vessel dimensions. However, when contrasted with sherds of the same bowl type from other contexts at Leilan, a higher degree of compositional and metric variability is observed. This ''cumulative blurring'' effect stems from the use of long-lived types from multiple workshops. Although ''cumulative blurring'' increases sample variability, it does not obscure the overall homogeneity of these ceramics. Our results suggest that standardization can be a reliable index of craft specialization only under conditions of close spatial and chronological control over the archaeological record. C1 NORTHWESTERN UNIV,DEPT ANTHROPOL,EVANSTON,IL 60208. RP BLACKMAN, MJ (reprint author), SMITHSONIAN INST,CONSERVAT ANALYT LAB,WASHINGTON,DC 20560, USA. NR 58 TC 62 Z9 62 U1 0 U2 9 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE WASHINGTON, DC 20002-3557 SN 0002-7316 J9 AM ANTIQUITY JI Am. Antiq. PD JAN PY 1993 VL 58 IS 1 BP 60 EP 80 DI 10.2307/281454 PG 21 WC Anthropology; Archaeology SC Anthropology; Archaeology GA KX084 UT WOS:A1993KX08400004 ER PT J AU LELLINGER, DB AF LELLINGER, DB TI BISHOP,LUTHER,EARL (1943-1991) SO AMERICAN FERN JOURNAL LA English DT Item About an Individual RP LELLINGER, DB (reprint author), SMITHSONIAN INST,DEPT BOT NHB-166,WASHINGTON,DC 20560, USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU AMER FERN SOC INC PI WASHINGTON PA C/O DAVID B LELLINGER, SMITHSONIAN INST, BOTANY DEPT, WASHINGTON, DC 20560 SN 0002-8444 J9 AM FERN J JI Am. Fern J. PD JAN-MAR PY 1993 VL 83 IS 1 BP 1 EP 2 PG 2 WC Plant Sciences SC Plant Sciences GA KV751 UT WOS:A1993KV75100001 ER PT J AU DYKE, B GAGE, TB BALLOU, JD PETTO, AJ TARDIF, SD WILLIAMS, LE AF DYKE, B GAGE, TB BALLOU, JD PETTO, AJ TARDIF, SD WILLIAMS, LE TI MODEL LIFE-TABLES FOR THE SMALLER NEW-WORLD MONKEYS SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE MORTALITY; NONHUMAN PRIMATES; SURVIVORSHIP AB Mortality statistics from five populations of small New World monkeys (including Callithrix jaccus, Leontopithecus rosalia, Saguinus fuscicollis, and Saguinus oedipus) were combined to generate a standard model life table reflecting the mortality patterns of these primates. The model is applied to three individual populations to illustrate a strategy for smoothing and interpolating mortality statistics of varying completeness and quality. C1 SUNY ALBANY,DEPT ANTHROPOL,ALBANY,NY 12222. SMITHSONIAN INST,DEPT ZOOL RES,NATL ZOOL PK,WASHINGTON,DC 20560. HARVARD UNIV,SCH MED,NEW ENGLAND REG PRIMATE RES CTR,SOUTHBOROUGH,MA 01772. OAK RIDGE ASSOCIATED UNIV,MARMOSET RES CTR,OAK RIDGE,TN 37830. UNIV SO ALABAMA,COLL MED,PRIMATE RES LAB,MOBILE,AL 36688. RP DYKE, B (reprint author), SW FDN BIOMED RES,DEPT GENET,SAN ANTONIO,TX 78228, USA. NR 7 TC 14 Z9 14 U1 1 U2 3 PU WILEY-LISS PI NEW YORK PA DIV JOHN WILEY & SONS INC 605 THIRD AVE, NEW YORK, NY 10158-0012 SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PY 1993 VL 29 IS 4 BP 269 EP 285 DI 10.1002/ajp.1350290404 PG 17 WC Zoology SC Zoology GA KV033 UT WOS:A1993KV03300003 ER PT J AU ALLEN, RO HAMROUSH, H STANLEY, DJ AF ALLEN, RO HAMROUSH, H STANLEY, DJ TI IMPACT OF THE ENVIRONMENT ON EGYPTIAN CIVILIZATION BEFORE THE PHARAOHS SO ANALYTICAL CHEMISTRY LA English DT Article ID NILE C1 UNIV CAIRO,FAC SCI,GIZA,EGYPT. US MUSEUM NAT HIST,SMITHSONIAN INST,WASHINGTON,DC 20560. RP ALLEN, RO (reprint author), UNIV VIRGINIA,DEPT CHEM,CHARLOTTESVILLE,VA 22901, USA. NR 7 TC 1 Z9 1 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 SN 0003-2700 J9 ANAL CHEM JI Anal. Chem. PD JAN 1 PY 1993 VL 65 IS 1 BP A32 EP & DI 10.1021/ac00049a002 PG 0 WC Chemistry, Analytical SC Chemistry GA KE643 UT WOS:A1993KE64300003 ER PT J AU HERSHKOVITZ, MA AF HERSHKOVITZ, MA TI REVISED CIRCUMSCRIPTIONS AND SUBGENERIC TAXONOMIES OF CALANDRINIA AND MONTIOPSIS (PORTULACACEAE) WITH NOTES ON PHYLOGENY OF THE PORTULACACEOUS ALLIANCE SO ANNALS OF THE MISSOURI BOTANICAL GARDEN LA English DT Article ID CISTANTHE SPACH PORTULACACEAE; ALLIED GENERA; CHARACTER STATES; CLAYTONIA-L; MONTIA L; CENTROSPERMAE; RYDB; CLASSIFICATION; CONSENSUS; ORIGIN AB Cladistic analysis of Portulacaceae supports a revised taxonomy of Calandrinia sensu lato. Calandrinia, as here circumscribed, comprises ca. 14 western American species in three sections: Calandrinia, Acaules, and Monocosmia. Previous taxonomies classified over 100 species in Calandrinia but recognized Monocosmia as a distinct genus. Calandrinia sects. Calandrinia and Monocosmia are probably cladistically nested in section Acaules and are not sister groups of either Rumicastrum or Montia, as proposed in a previous cladistic analysis. Montiopsis Kuntze, traditionally included in Calandrinia, comprises ca. 15 western South American species in two subgenera, Montiopsis and Dianthoideae. At present, cladistic analysis provides only weak evidence linking Calandrinia and Montiopsis to one another and poorly resolves their precise relationships to other Portulacaceae. This analysis supports a taxonomic distinction between the eastern American/African and western American members of Portulacaceae, but poorly resolves the relationship between the two groups. Cactaceae, Basellaceae, Didiereaceae, and perhaps Hectorellaceae, which were not included in the analysis, belong to the eastern American/African group. The present analysis provides a framework for additional studies of phylogeny of the portulacaceous alliance and of Centrospermae in general. RP HERSHKOVITZ, MA (reprint author), SMITHSONIAN INST,CTR MUSEUM SUPPORT,MOLEC SYSTEMAT LAB,WASHINGTON,DC 20560, USA. NR 121 TC 32 Z9 33 U1 1 U2 3 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 SN 0026-6493 J9 ANN MO BOT GARD JI Ann. Mo. Bot. Gard. PY 1993 VL 80 IS 2 BP 333 EP 365 DI 10.2307/2399789 PG 33 WC Plant Sciences SC Plant Sciences GA LC647 UT WOS:A1993LC64700008 ER EF