FN Thomson Reuters Web of Science™ VR 1.0 PT J AU BLELLOCH, GE CHATTERJEE, S ZAGHA, M AF BLELLOCH, GE CHATTERJEE, S ZAGHA, M TI SOLVING LINEAR RECURRENCES WITH LOOP RAKING SO JOURNAL OF PARALLEL AND DISTRIBUTED COMPUTING LA English DT Note ID PARALLEL; SUPERCOMPUTERS; VECTORIZATION; COMPUTATION; ALGORITHMS; EQUATIONS; COMPUTER AB We present a variation of the partition method for solving linear recurrences that is well-suited to vector multiprocessors. The algorithm fully utilizes both vector and multiprocessor capabilities, and reduces the number of memory accesses and temporary memory requirements as compared to the more commonly used version of the partition method. Our variation uses a general loop restructuring technique called loop raking. We describe an implementation of this technique on the GRAY Y-MP C90, and present performance results for first- and second-order linear recurrences. On a single processor of the C90 our implementations are up to 7.3 times faster than the corresponding optimized library routines in SCILIB, an optimized mathematical library supplied by Gray Research. On four processors, we gain an additional speedup of at least 3.7. (C) 1995 Academic Press, Inc. C1 NASA,AMES RES CTR,RIACS,MOFFETT FIELD,CA 94035. RP BLELLOCH, GE (reprint author), CARNEGIE MELLON UNIV,SCH COMP SCI,PITTSBURGH,PA 15213, USA. NR 34 TC 4 Z9 4 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0743-7315 J9 J PARALLEL DISTR COM JI J. Parallel Distrib. Comput. PD FEB 15 PY 1995 VL 25 IS 1 BP 91 EP 97 DI 10.1006/jpdc.1995.1031 PG 7 WC Computer Science, Theory & Methods SC Computer Science GA QP814 UT WOS:A1995QP81400008 ER PT J AU WEAVER, ML NOEBE, RD LEWANDOWSKI, JJ OLIVER, BF KAUFMAN, MJ AF WEAVER, ML NOEBE, RD LEWANDOWSKI, JJ OLIVER, BF KAUFMAN, MJ TI THE EFFECTS OF INTERSTITIAL CONTENT, HEAT-TREATMENT, AND PRESTRAIN ON THE TENSILE PROPERTIES OF NIAL SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article; Proceedings Paper CT 3rd International Conference on High Temperature Intermetallics CY MAY 16-19, 1994 CL SAN DIEGO, CA SP ASM INT DE HEAT TREATMENT; TENSILE PROPERTIES; NICKEL; ALUMINUM ID BEHAVIOR; PRESSURE AB The tensile stress-strain response of polycrystalline NiAl was studied as a function of purity and pretest treatment (annealing and/or prestrain). After annealing at 1100 K for 7200 s (i.e. 2 h) followed by furnace cooling, high-purity and nitrogen-doped alloys exhibited continuous yielding, while conventional-purity or carbon-doped alloys exhibited a distinct yield point and Luders strain. Prestrain by hydrostatic pressurization removed the yield point, but it could be reintroduced by further annealing treatments. Yield points could be reintroduced more rapidly if the specimens were prestrained uniaxially rather than hydrostatically, owing to the arrangement of dislocations into cell structures during uniaxial deformation. The time dependence of the strain aging events followed a t(2/3) relationship. In total, these results suggest that the yield points observed in polycrystalline NiAl result from the pinning of mobile dislocations by interstitials, specifically carbon, i.e. classic static strain aging. C1 NASA, LEWIS RES CTR, CLEVELAND, OH 44135 USA. CASE WESTERN RESERVE UNIV, CLEVELAND, OH 44106 USA. UNIV TENNESSEE, KNOXVILLE, TN 37996 USA. RP WEAVER, ML (reprint author), UNIV FLORIDA, GAINESVILLE, FL 32611 USA. RI Kaufman, Michael/A-7737-2012 NR 34 TC 21 Z9 21 U1 1 U2 2 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD FEB 15 PY 1995 VL 192 BP 179 EP 185 DI 10.1016/0921-5093(94)03233-5 PG 7 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA QP321 UT WOS:A1995QP32100025 ER PT J AU DEMARCO, HK ARDELL, AJ NOEBE, RD AF DEMARCO, HK ARDELL, AJ NOEBE, RD TI THE EFFECTS OF HEAT-TREATMENT AND PURITY ON THE MECHANICAL-PROPERTIES OF MONOCRYSTALLINE NIAL SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article; Proceedings Paper CT 3rd International Conference on High Temperature Intermetallics CY MAY 16-19, 1994 CL SAN DIEGO, CA SP ASM INT DE HEAT TREATMENT; MECHANICAL PROPERTIES; NICKEL; ALUMINUM; CRYSTALS ID 1050 DEGREES K; DISK-BEND TEST; SINGLE-CRYSTALS; PLASTIC-DEFORMATION; UNIFORM DEFORMATION; BEHAVIOR; TENSILE; DUCTILITY; FRACTURE; KINKING AB The yield stress, sigma(y), strain to fracture, epsilon(f), and thickness-compensated fracture load of monocrystalline NiAl were investigated as functions of purity, annealing treatment and cooling rates. A miniaturized disk bend test was employed to test disks 3 mm in diameter and approximately 250 mu m thick. Specimens in the soft (110) orientation from commercial purity (CP) and high-purity (HP) alloys were tested. The annealing treatments affected sigma(y) more strongly than the other mechanical properties. The yield stresses of both of the as-received alloys increased significantly after annealing at 1300 degrees C followed by furnace cooling. Subsequent annealing at 400 degrees C for 2 h resulted in a reduction of sigma(y). This behavior is attributed to the role of excess vacancies retained during cooling, which annealed out at the lower temperature. The mean values of the yield strength also tended to decrease with increasing cooling rate from 400 degrees C, but the effect was small. A substantial increase in sigma(y) of the CP alloy was found on prolonged aging at 400 degrees C, whereas sigma(y) of the HP alloy was unaffected. We attribute this behavior to the precipitation of very small particles or solute atom clusters in the CP alloy. The ductility of the CP alloy, and the thickness-compensated fracture loads of both alloys, were relatively insensitive to the heat treatments. C1 NASA, LEWIS RES CTR, CLEVELAND, OH 44135 USA. RP DEMARCO, HK (reprint author), UNIV CALIF LOS ANGELES, DEPT MAT SCI & ENGN, LOS ANGELES, CA 90024 USA. NR 35 TC 3 Z9 3 U1 0 U2 1 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD FEB 15 PY 1995 VL 192 BP 333 EP 339 DI 10.1016/0921-5093(94)03215-7 PG 7 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA QP321 UT WOS:A1995QP32100044 ER PT J AU TIWARI, R TEWARI, SN ASTHANA, R GARG, A AF TIWARI, R TEWARI, SN ASTHANA, R GARG, A TI DEVELOPMENT OF NIAL-BASED INTERMETALLIC ALLOYS - EFFECT OF CHROMIUM ADDITION SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article; Proceedings Paper CT 3rd International Conference on High Temperature Intermetallics CY MAY 16-19, 1994 CL SAN DIEGO, CA SP ASM INT DE NICKEL; ALUMINUM; CHROMIUM; INTERMETALLICS; ALLOYS ID MECHANICAL-PROPERTIES; TEMPERATURE; DUCTILITY; FRACTURE; TENSILE; FEAL AB The mechanical behavior of dual-phase NiAl(Cr) microstructures, consisting of elongated primary NiAl grains aligned with an intergranular NiAl-Cr eutectic phase, produced by extrusion of a cast NiAl(Cr) alloy, has been examined. Chromium addition to create a dual phase NiAl-based aligned microstructure leads to large increases in the yield strength but no significant toughness improvement. This is achieved primarily by solid solution hardening and precipitation hardening. The constitutional hardening rate resulting from deviations from stoichiometry in the nickel-rich NiAl was estimated to be about 66 MPa per atomic per cent of nickel. C1 NASA, LEWIS RES CTR, DIV MAT, CLEVELAND, OH 44135 USA. RP TIWARI, R (reprint author), CLEVELAND STATE UNIV, DEPT CHEM ENGN, CLEVELAND, OH 44115 USA. NR 21 TC 14 Z9 15 U1 0 U2 2 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD FEB 15 PY 1995 VL 192 BP 356 EP 363 DI 10.1016/0921-5093(94)03218-1 PG 8 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA QP321 UT WOS:A1995QP32100047 ER PT J AU BELL, KL HIBBERT, A STAFFORD, RP BRAGE, T AF BELL, KL HIBBERT, A STAFFORD, RP BRAGE, T TI TRANSITION-PROBABILITIES FOR SOME SPECTRAL-LINES OF N-III SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ATOMIC DATA; ATOMIC PROCESSES ID LIFETIMES AB Transition probabilities based on sophisticated configuration-interaction wave functions have been obtained for transitions between the 20 lowest lying fine-structure levels of the 2s(2)2p, 2s2p2, 2p3, 2s(2)3s, 2s(2)3p and 2s(2)3d states of N III. The calculations were performed using the CIV3 code of Hibbert, and small empirical adjustments were introduced to the diagonal Hamiltonian matrix elements in order to achieve accurate energy separations between the levels. The present results are believed to be the most accurate available. Comparison is made with the recent experimental data of Fang et al. for the radiative lifetimes of the 2s2p2 4P metastable levels, and the discrepancy between theory and experiment is discussed. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP BELL, KL (reprint author), QUEENS UNIV BELFAST,DEPT APPL MATH & THEORET PHYS,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. NR 11 TC 14 Z9 14 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 FEB 15 PY 1995 VL 272 IS 4 BP 909 EP 912 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QH169 UT WOS:A1995QH16900022 ER PT J AU STEBBINS, A VEERARAGHAVAN, S AF STEBBINS, A VEERARAGHAVAN, S TI BEYOND THE SMALL-ANGLE APPROXIMATION FOR MBR ANISOTROPY FROM SEEDS SO PHYSICAL REVIEW D LA English DT Article ID RADIOMETER 1ST-YEAR MAPS; COSMIC STRINGS; GLOBAL TEXTURE; DOMAIN-WALLS; MICROWAVE; UNIVERSE C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP STEBBINS, A (reprint author), FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,MS 209,POB 500,BATAVIA,IL 60510, USA. NR 21 TC 10 Z9 10 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 FEB 15 PY 1995 VL 51 IS 4 BP 1465 EP 1478 DI 10.1103/PhysRevD.51.1465 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA QH867 UT WOS:A1995QH86700004 ER PT J AU SIGL, G TURNER, MS AF SIGL, G TURNER, MS TI MASSIVE TAU-NEUTRINO AND SN 1987A SO PHYSICAL REVIEW D LA English DT Article ID DIRAC NEUTRINOS; RADIATIVE DECAY; SUPERNOVA 1987A; SN-1987A; LIMITS; CONSTRAINTS; LIFETIMES; COINCIDENCE; SN1987A; MASSES C1 FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. UNIV CHICAGO,ENRICO FERMI INST,DEPT PHYS,CHICAGO,IL 60637. RP SIGL, G (reprint author), UNIV CHICAGO,ENRICO FERMI INST,DEPT ASTRON & ASTROPHYS,CHICAGO,IL 60637, USA. NR 32 TC 10 Z9 10 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 FEB 15 PY 1995 VL 51 IS 4 BP 1499 EP 1509 DI 10.1103/PhysRevD.51.1499 PG 11 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA QH867 UT WOS:A1995QH86700007 ER PT J AU ALLEN, B CALDWELL, RR KORANDA, S AF ALLEN, B CALDWELL, RR KORANDA, S TI CBR TEMPERATURE-FLUCTUATIONS INDUCED BY GRAVITATIONAL-WAVES IN A SPATIALLY CLOSED INFLATIONARY UNIVERSE SO PHYSICAL REVIEW D LA English DT Article ID QUANTUM LINEARIZATION INSTABILITIES; ROBERTSON-WALKER UNIVERSES; DESITTER SPACETIME; SITTER SPACE; GRAVITY C1 FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. UNIV CAMBRIDGE,DEPT APPL MATH & THEORET PHYS,CAMBRIDGE CB3 9EW,ENGLAND. RP ALLEN, B (reprint author), UNIV WISCONSIN,DEPT PHYS,POB 413,MILWAUKEE,WI 53201, USA. RI Allen, Bruce/K-2327-2012; OI Allen, Bruce/0000-0003-4285-6256; Caldwell, Robert/0000-0001-7490-7463 NR 20 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 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD FEB 15 PY 1995 VL 51 IS 4 BP 1553 EP 1562 DI 10.1103/PhysRevD.51.1553 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA QH867 UT WOS:A1995QH86700012 ER PT J AU ANGELANTONJ, C AMENDOLA, L LITTERIO, M OCCHIONERO, F AF ANGELANTONJ, C AMENDOLA, L LITTERIO, M OCCHIONERO, F TI STRING COSMOLOGY AND INFLATION SO PHYSICAL REVIEW D LA English DT Article ID SUPERSTRING COSMOLOGY; SCALAR FIELD; UNIVERSE; DUALITY; MODELS; INVARIANCE; DIMENSIONS; GRAVITY; VACUA; ORDER C1 OSSERV ASTRON ROMA,I-00136 ROME,ITALY. FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. UNIV ROMA LA SAPIENZA,IST ASTRON,I-00161 ROME,ITALY. RP ANGELANTONJ, C (reprint author), UNIV AQUILA,DIPARTIMENTO FIS,VIA VETOIO,I-67010 COPPITO,ITALY. OI Angelantonj, Carlo/0000-0003-2549-2382 NR 44 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 0556-2821 J9 PHYS REV D JI Phys. Rev. D PD FEB 15 PY 1995 VL 51 IS 4 BP 1607 EP 1616 DI 10.1103/PhysRevD.51.1607 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA QH867 UT WOS:A1995QH86700017 ER PT J AU RAO, KBS KALLURI, S HALFORD, GR MCGAW, MA AF RAO, KBS KALLURI, S HALFORD, GR MCGAW, MA TI SERRATED FLOW AND DEFORMATION SUBSTRUCTURE AT ROOM-TEMPERATURE IN INCONEL-718 SUPERALLOY DURING STRAIN CONTROLLED FATIGUE SO SCRIPTA METALLURGICA ET MATERIALIA LA English DT Article ID MECHANISMS C1 NASA,LEWIS RES CTR,NYMA INC,CLEVELAND,OH 44135. RP RAO, KBS (reprint author), NASA,LEWIS RES CTR,DIV STRUCT,MS-49-7,21000 BROOK PK RD,CLEVELAND,OH 44135, USA. NR 16 TC 21 Z9 21 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0956-716X J9 SCRIPTA METALL MATER JI Scr. Metall. Materialia PD FEB 15 PY 1995 VL 32 IS 4 BP 493 EP 498 DI 10.1016/0956-716X(95)90826-6 PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA PY850 UT WOS:A1995PY85000003 ER PT J AU BRILL, RW BALAZS, GH HOLLAND, KN CHANG, RKC SULLIVAN, S GEORGE, JC AF BRILL, RW BALAZS, GH HOLLAND, KN CHANG, RKC SULLIVAN, S GEORGE, JC TI DAILY MOVEMENTS, HABITAT USE, AND SUBMERGENCE INTERVALS OF NORMAL AND TUMOR-BEARING JUVENILE GREEN TURTLES (CHELONIA-MYDAS L) WITHIN A FORAGING AREA IN THE HAWAIIAN-ISLANDS SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE BEHAVIOR; DIVING; FIBROPAPILLOMA; FIBROPAPILLOMATOSIS; SEA TURTLE; TUMOR ID LOGGERHEAD SEA-TURTLE; CUTANEOUS FIBROPAPILLOMAS; CARETTA-CARETTA; GAS-EXCHANGE; ACID-BASE; REST; VENTILATION AB Depth-sensitive ultrasonic transmitters monitored the horizontal and vertical movements of 12 juvenile (<65 cm carapace length) green turtles (Chelonia mydas L.) in Kaneohe Bay, Oahu (Hawaii, USA). This site was chosen because of its accessibility, its importance as a foraging area, and the high incidence (almost-equal-to 50%) of fibropapillomatosis, a tumor disease of unknown etiology. Our objectives were to determine the daily movements, habitat use, and submergence intervals of normal and tumor-bearing animals. The presence of tumors had no obvious effects on movement patterns or habitat use. All turtles remained within a small portion of the bay where patch reefs and shallow coral-covered areas are common, and algal growth most abundant. During daylight, two normal and two tumor-bearing animals remained within known feeding areas, all other turtles studied stayed within deep mud bottom channels or within crevices on the sides of reefs. All, except one tumor-bearing turtle, moved up on to shallow patch reefs or shallow coral-covered areas at night. Submergence intervals for both groups were short (over 90% were 33 min or less and none exceeded 66 min) compared to maximum breath-hold times (up to 5 h) measured in the laboratory by earlier workers. Juvenile green turtles in Hawaii, therefore, most likely maintain aerobic metabolism while submerged and surface before oxygen stores are significantly depleted. Tumor-bearing turtles had a higher frequency of longer submergence intervals during the night, indicating they may have been somewhat less active at night. Normal turtles showed no such day-night difference. C1 UNIV HAWAII, HAWAII INST MARINE BIOL, KANEOHE, HI 96744 USA. RP BRILL, RW (reprint author), NOAA, NATL MARINE FISHERIES SERV, HONOLULU LAB, SW FISHERIES SCI CTR, 2570 DOLE ST, HONOLULU, HI 96822 USA. NR 57 TC 45 Z9 49 U1 1 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD FEB 13 PY 1995 VL 185 IS 2 BP 203 EP 218 DI 10.1016/0022-0981(94)00146-5 PG 16 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA QJ016 UT WOS:A1995QJ01600005 ER PT J AU MELISSARIS, AP SUTTER, JK LITT, MH SCHEIMAN, DA SCHUERMAN, MA AF MELISSARIS, AP SUTTER, JK LITT, MH SCHEIMAN, DA SCHUERMAN, MA TI HIGH-MODULUS AND HIGH T-G THERMALLY STABLE POLYMERS FROM P-ETHYNYL-TERMINATED RIGID-ROD MONOMERS .2. SO MACROMOLECULES LA English DT Article AB Novel p-ethynyl-substituted rigid rod monomers were studied by pressure differential scanning calorimetry (DSC), thermogravimetric analysis (TGA), isothermogravimetric analysis (IGA), and TGA-IR. These monomers, 4,4'-bis[((4-ethynylphenyl)carbonyl)oxy] designated 1, 1,5-bis[((4-ethynylphenyl)carbonyl)oxy]naphthalene, designated 2, and bis(4-ethynylphenyl)pyromellitimide, designated 3, were polymerized in the solid state. Thermal polymerization in Nz or air produced highly cross-linked resins with polymerization exotherms centered between 212 and 276 degrees C. The Delta H's of polymerization of these resins in air were found to be double those in N-2. When monomers 1 and 2 were heated in air from 23 to 750 degrees C at 10 degrees C/min, the main decomposition product was carbon dioxide, evolving at a maximum rate between 500 and 600 degrees C; water was also detected as a decomposition product. Void-free neat resin moldings, designated 1p to 3p, were made by compression molding the monomers and then heating them. The resulting polymers were highly cross-linked, and their glass transition temperatures (T-g) were much higher than their polymerization temperatures. Using thermomechanical analysis (TMA), we found that polymers 1p to 3p had T-g's of 422, 329, and 380 degrees C, respectively. The thermal and thermooxidative stabilities improved when 1p to 3p were postcured in N-2 (the postcured polymers were designated 1pp to 3pp). The linear thermal expansions (LTE) for 1p and 3p were 1% between 23 and 420 degrees C. Using theological analysis, we could not clearly detect the T-g's of 1p to 3p because their moduli dropped only slightly between 23 and 490 degrees C and the changes in tan delta were very low. Because of high cross-link density, their moduli changed little as the resins went from a glassy to a robbery state. Their shear storage moduli in air ranged from 0.82 (3p, 3pp) to 1.6 GPa (1pp) at 23 degrees C, from 0.16 (2p) to 0.7 GPa (1 pp) at 380 degrees C, and from 0.18 (1pp) to 0.6 GPa (2p) at 490 degrees C, Finally, these novel p-ethynyl polymers exhibited an excellent combination of high T-g, low LTE, and high thermooxidative stability. Most notably, 3pp lost only 3% of its initial weight when it was aged for 500 h at 288 degrees C in air. C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. CASE WESTERN RESERVE UNIV,DEPT MACROMOLEC SCI,CLEVELAND,OH 44106. SVERDRUP TECHNOL INC,LEWIS RES CTR GRP,BROOKPARK,OH 44142. NR 10 TC 12 Z9 12 U1 0 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA PO BOX 57136, WASHINGTON, DC 20037-0136 SN 0024-9297 J9 MACROMOLECULES JI Macromolecules PD FEB 13 PY 1995 VL 28 IS 4 BP 860 EP 865 DI 10.1021/ma00108a009 PG 6 WC Polymer Science SC Polymer Science GA QG795 UT WOS:A1995QG79500009 ER PT J AU ZHOU, SM CAMPBELL, S YEH, PC LIU, HK AF ZHOU, SM CAMPBELL, S YEH, PC LIU, HK TI 2-STAGE MODIFIED SIGNED-DIGIT OPTICAL COMPUTING BY SPATIAL DATA ENCODING AND POLARIZATION MULTIPLEXING SO APPLIED OPTICS LA English DT Article ID SYMBOLIC SUBSTITUTION; LOGIC; ADDER; ELEMENTS AB We propose and demonstrate an effective two-stage modified signed-digit optical computing technique (in contrast to previous three-stage techniques) based on spatial data encoding, polarization multiplexing, and multiple imaging. Our proposed reduction in operation stages requires a reference operation in addition to the transformation and weight operations common to three-stage systems. In our system's first stage a transformation (or weight) operation and a reference operation are implemented in parallel by use of four distinct polarization-multiplexed kernel operations. In the second stage the final desired result (e.g., addition and subtraction) and its complement are obtained in parallel with a single kernel operation. The operation speed of our two-stage modified signed-digit computing method is 33% faster than previous three-stage modified signed-digit algorithms. C1 CALTECH,JET PROP LAB,CTR SPACE MICROELECTR TECHNOL,PASADENA,CA 91109. RP ZHOU, SM (reprint author), UNIV CALIF SANTA BARBARA,DEPT ELECT & COMP ENGN,SANTA BARBARA,CA 93106, USA. RI Yeh, Pochi/A-2109-2010 NR 19 TC 17 Z9 19 U1 0 U2 1 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 SN 0003-6935 J9 APPL OPTICS JI Appl. Optics PD FEB 10 PY 1995 VL 34 IS 5 BP 793 EP 802 PG 10 WC Optics SC Optics GA QH124 UT WOS:A1995QH12400004 PM 21037597 ER PT J AU DAVIS, DS BIRD, CM MUSHOTZKY, RF ODEWAHN, SC AF DAVIS, DS BIRD, CM MUSHOTZKY, RF ODEWAHN, SC TI ABELL-548 - AN X-RAY AND OPTICAL ANALYSIS OF SUBSTRUCTURE SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERS, GENERAL; INTERGALACTIC MEDIUM; X-RAYS, GALAXIES ID COMA CLUSTER; DARK MATTER; RICH CLUSTERS; GALAXIES; MORPHOLOGY; EVOLUTION; DYNAMICS; EMISSION; CATALOG; MASSES AB X-ray observations of Abell 548 reveal that the hot gas in this cluster is at least as complex as the galaxy distribution. Our ROSAT Position Sensitive Proportional Counter image is used in conjunction with optical data from the Minnesota plate-scanning project and redshift data in the literature to investigate the degree of substructure in the intracluster medium and the galaxy distribution. A548 has several X-ray components: hot gas associated with clumps of galaxies, individual sources, and a newly discovered diffuse component. This diffuse component may be primordial gas falling into the cluster for the first time. The optical data suggest that this cluster consists of four major components, not three (as indicated when velocity data are ignored). Simple models of the orbital dynamics suggest that the cluster may not yet have reached its turnaround radius. C1 UNIV KANSAS,DEPT PHYS & ASTRON,LAWRENCE,KS 66045. NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. UNIV MINNESOTA,DEPT ASTRON,MINNEAPOLIS,MN 55455. RP DAVIS, DS (reprint author), UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742, USA. NR 48 TC 34 Z9 34 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 1995 VL 440 IS 1 BP 48 EP 59 DI 10.1086/175246 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QE505 UT WOS:A1995QE50500005 ER PT J AU STOTHERS, RB CHIN, CW AF STOTHERS, RB CHIN, CW TI TESTS OF 2 CONVECTION THEORIES FOR RED GIANT AND RED SUPERGIANT ENVELOPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE CONVECTION; STARS, EVOLUTION; STARS, INTERIORS; STARS, LATE-TYPE; SUPERGIANTS ID MIXING-LENGTH THEORY; INTERMEDIATE-MASS STARS; STANDARD SOLAR MODEL; OPEN CLUSTERS; TURBULENT CONVECTION; EFFECTIVE TEMPERATURES; EVOLUTION CALCULATIONS; THEORY APPROXIMATIONS; MOLECULAR OPACITIES; STELLAR CONVECTION AB Two theories of stellar envelope convection are considered here in the context of red giants and red supergiants of intermediate to high mass: Bohm-Vitense's standard mixing-length theory (MLT) and Canuto and Mazzitelli's new theory incorporating the full spectrum of turbulence (FST). Both theories assume incompressible convection. Two formulations of the convective mixing length are also evaluated: l proportional to the local pressure scale height (H-p) and l proportional to the distance from the upper boundary of the convection zone (z). Applications to test both theories are made by calculating stellar evolutionary sequences into the red phase of core helium burning. Since the theoretically predicted effective temperatures for cool stars are known to be sensitive to the assigned value of the mixing length, this quantity has been individually calibrated for each evolutionary sequence. The calibration is done in a composite Hertzsprung-Russell diagram for the red giant and red supergiant members of well-observed Galactic open clusters. The MLT model requires the constant of proportionality for the convective mixing length to vary by a small but statistically significant amount with stellar mass, whereas the FST model succeeds in all cases with the mixing length simply set equal to z (as Canuto and Mazzitelli have also found for the Sun and low-mass red giants). The structure of the deep stellar interior, however, remains very nearly unaffected by the choices of convection theory and mixing length. Inside the convective envelope itself, a density inversion always occurs, but is somewhat smaller for the convectively more efficient MLT model. On physical grounds the FST model is preferable, and seems to alleviate the problem of finding the proper mixing length. RP STOTHERS, RB (reprint author), NASA,GODDARD SPACE FLIGHT CTR,INST SPACE STUDIES,2880 BROADWAY,NEW YORK,NY 10025, USA. NR 58 TC 31 Z9 32 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 1995 VL 440 IS 1 BP 297 EP 302 DI 10.1086/175270 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QE505 UT WOS:A1995QE50500029 ER PT J AU ASCHWANDEN, MJ MONTELLO, ML DENNIS, BR BENZ, AO AF ASCHWANDEN, MJ MONTELLO, ML DENNIS, BR BENZ, AO TI SEQUENCES OF CORRELATED HARD X-RAY AND TYPE-III BURSTS DURING SOLAR-FLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCELERATION OF PARTICLES; SUN, FLARES; SUN, RADIO RADIATION; SUN, X-RAYS, GAMMA RAYS ID RADIO-BURSTS; ENERGETIC ELECTRONS; SPECTROMETER; MICROWAVES AB Acceleration and injection of electron beams in solar flares can be traced from radio type III (or type U) bursts and correlated hard X-ray pulses with similar timescales and nonthermal spectra. We perform a systematic survey of such correlated radio and HXR pulses with timescales of less than or similar to 2 s in flares simultaneously observed with the radio spectrometer Ikarus and the Hard X-Ray Burst Spectrometer (HXRBS) on SMM. We applied an epoch-folding technique to enhance correlated time patterns in burst sequences at the two wavelengths. We present the results from the strongest (10) flares with a HXRBS count rate greater than or equal to 3000 counts s(-1), which have a satisfactory signal-to-noise ratio for subsecond pulses. The major findings of this study are as follows: 1. Sequences of correlated HXR and radio bursts with equal burst durations and intervals at the two wavelengths are found in all strong flares. 2. The sequences were found to contain between two and nine correlated pulses in HXR and radio. 3. The epoch-folded HXR pulses (with respect to the peak times of the type III bursts) were found to have a high statistical significance of 6-57 sigma. 4. The duration of these correlated pulses varies from 0.2 to 2.0 s, the pulses have a duty cycle of about 50%, and the pulse duration in HXR and radio is highly correlated. 5. The radio bursts (detected at approximate to 300 MHz) are systematically delayed with respect to the HXR pulses by 0.4 +/- 0.6 s. 6. The best correlation was found for a lower energy cutoff of 40 +/- 22 keV in HXR. 7. The altitude of the particle injection site, inferred from energy-dependent (time-of-flight) delays of HXR-emitting electrons, was found in the range of 18-32 Mm in three flares. These observations strongly suggest that particle acceleration in solar flares occurs in a pulsed mode where electron beams are simultaneously injected in upward and downward directions. Since the sequences of correlated HXR and radio bursts show identical durations and intervals at the two wavelengths, they are believed to reflect most directly the temporal dynamics of the underlying common accelerator. As a consequence, thick-target models should be reconsidered under the aspect of electron injection with pulse durations of 0.2-2.0 s and duty cycles of approximate to 50%. C1 CATHOLIC UNIV AMER,DEPT MATH,WASHINGTON,DC 20064. NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. ETH ZURICH,INST ASTRON,CH-8092 ZURICH,SWITZERLAND. RP ASCHWANDEN, MJ (reprint author), UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742, USA. RI Dennis, Brian/C-9511-2012 NR 37 TC 50 Z9 50 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 1995 VL 440 IS 1 BP 394 EP 406 DI 10.1086/175281 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QE505 UT WOS:A1995QE50500040 ER PT J AU ZUO, M SMITH, SJ CHUTJIAN, A WILLIAMS, ID TAYAL, SS MCLAUGHLIN, BM AF ZUO, M SMITH, SJ CHUTJIAN, A WILLIAMS, ID TAYAL, SS MCLAUGHLIN, BM TI ELECTRON-EXCITATION CROSS-SECTION FOR THE 2S(2)2P(3) 4S(DEGREES)-]2S(2)2P(3) 2D(DEGREES) (FORBIDDEN) AND S-4(DEGREES)-]2S2P(4)-4P (RESONANCE) TRANSITIONS IN O-II SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC PROCESS ID MERGED-BEAMS METHODS; INTERMULTIPLET 1S(2)2S(2)2P(3); COLLISIONAL EXCITATION; OPACITY CALCULATIONS; ATOMIC OXYGEN; ENERGY-LOSS; IO-TORUS; SPECTROSCOPY; 1S(2)2S2P(4); STRENGTHS AB Experimental and theoretical excitation cross sections are reported for the first forbidden transition S-4(0) --> 2S(2)2p(3 2) D-0 (lambda lambda 3726, 3729) and the first allowed (resonance) transition S-4(0) --> 2s2p(4 4) P (lambda 833) in O II. Use is made of electron energy loss and merged-beams methods. The electron energy range covered is 3.33 (threshold) to 15 eV for the S --> D transition, and 14.9 (threshold) to 40 eV for the S --> P transition. Care was taken to assess and minimize the metastable fraction of the O II beam. An electron mirror was designed and tested to reflect inelastically backscattered electrons into the forward direction to account for the full range of polar scattering angles. Comparisons are made between present experiments and 11-state R-matrix calculations. Calculations are also presented for the S-4(0) --> 2S(2)2p(3) P-2(0) (lambda 2470) transition. C1 QUEENS UNIV BELFAST,DEPT PURE & APPL PHYS,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. CALTECH,JET PROP LAB,PASADENA,CA 91109. CLARK ATLANTA UNIV,DEPT PHYS,ATLANTA,GA 30314. CLARK ATLANTA UNIV,CTR THEORET STUDIES PHYS SYST,ATLANTA,GA 30314. HARVARD SMITHSONIAN CTR ASTROPHYS,INST THEORET ATOM & MOLEC PHYS,CAMBRIDGE,MA 02138. NR 38 TC 20 Z9 20 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 1995 VL 440 IS 1 BP 421 EP 429 DI 10.1086/175284 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QE505 UT WOS:A1995QE50500043 ER PT J AU WARD, WR HAHN, JM AF WARD, WR HAHN, JM TI DISK TIDES AND ACCRETION RUNAWAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; CELESTIAL MECHANICS, STELLAR DYNAMICS; PLANETS AND SATELLITES, GENERAL; SOLAR SYSTEM, FORMATION ID GIANT PLANETS; DENSITY WAVES; SOLAR NEBULA; PLANETESIMALS; EVOLUTION; LINDBLAD; PROTOPLANET; EXCITATION; RESONANCES; TORQUE AB It is suggested that tidal interaction of an accreting planetary embryo with the gaseous preplanetary disk may provide a mechanism to breach the so-called runaway limit during the formation of the giant planet cores. The disk tidal torque converts a would-be shepherding object into a ''predator,'' which can continue to cannibalize the planetesimal disk. This is more likely to occur in the giant planet region than in the terrestrial zone, providing a natural cause for Jupiter to predate the inner planets and form within the O(10(7) yr) lifetime of the nebula. C1 UNIV NOTRE DAME,DEPT PHYS,NOTRE DAME,IN 46556. SAN JUAN CAPISTRANO RES INST,SAN JUAN CAPISTRANO,CA. RP WARD, WR (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 30 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 10 PY 1995 VL 440 IS 1 BP L25 EP L28 DI 10.1086/187752 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QE506 UT WOS:A1995QE50600007 ER PT J AU GOLDSTEIN, ME WUNDROW, DW AF GOLDSTEIN, ME WUNDROW, DW TI INTERACTION OF OBLIQUE INSTABILITY WAVES WITH WEAK STREAMWISE VORTICES SO JOURNAL OF FLUID MECHANICS LA English DT Article ID TOLLMIEN-SCHLICHTING WAVES; BOUNDARY-LAYER-TRANSITION; TAYLOR-GORTLER VORTICES; NONLINEAR-INTERACTION; RESONANT-TRIAD; SHEAR LAYERS; UPPER BRANCH; FLAT-PLATE; FLOW; DISTURBANCES AB This paper is concerned with the effect of a weak spanwise-variable mean-flow distortion on the growth of oblique instability waves in a Blasius boundary layer. The streamwise component of the distortion velocity initially grows linearly with increasing streamwise distance, reaches a maximum, and eventually decays through the action of viscosity. This decay occurs slowly and allows the distortion to destabilize the Blasius flow over a relatively large streamwise region. It is shown that even relatively weak distortions can cause certain oblique Rayleigh instability waves to grow much faster than the usual two-dimensional Tollmien-Schlichting waves that would be the dominant instability modes in the absence of the distortion. The oblique instability waves can then become large enough to interact nonlinearly within a common critical layer. It is shown that the common amplitude of the interacting oblique waves is governed by the amplitude evolution equation derived in Goldstein & Choi (1989). The implications of these results for Klebanoff-type transition are discussed. C1 NYMA INC,LEWIS RES CTR GRP,CLEVELAND,OH 44135. RP GOLDSTEIN, ME (reprint author), NASA,LEWIS RES CTR,CLEVELAND,OH 44135, USA. NR 49 TC 15 Z9 15 U1 0 U2 0 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0022-1120 J9 J FLUID MECH JI J. Fluid Mech. PD FEB 10 PY 1995 VL 284 BP 377 EP 407 DI 10.1017/S0022112095000401 PG 31 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA QK089 UT WOS:A1995QK08900017 ER PT J AU COHEN, S HOLDAHL, S CAPRETTE, D HILLA, S SAFFORD, R SCHULTZ, D AF COHEN, S HOLDAHL, S CAPRETTE, D HILLA, S SAFFORD, R SCHULTZ, D TI UPLIFT OF THE KENAI PENINSULA, ALASKA, SINCE THE 1964 PRINCE-WILLIAM-SOUND EARTHQUAKE SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID CHUGACH MOUNTAINS; SOUTHERN AB Using Global Positioning System (GPS) receivers, we reoccupied several leveling benchmarks on the Kenai Peninsula of Alaska which had been surveyed by conventional leveling immediately following the March 27, 1964, Prince William Sound earthquake (M(w) = 9.3). By combining the two sets of measurements with a new, high-resolution model of the geoid in the region, we were able to determine the cumulative 1993-1964 postseismic vertical displacement. We find uplift at all of our benchmarks, relative to Seward, Alaska, a point that is stable according to tide gauge data. The maximum uplift of about 1 m occurs near the middle of the peninsula. The region of maximum uplift appears to be shifted northwest relative to the point of maximum coseismic subsidence. If we use tide gauge data at Nikishka and Seward to constrain the vertical motion, then the observed uplift has a trenchward tilt (down to the southeast) as well as an arching component. To explain the observations, we use creep-at-depth models. Most acceptable models require a fault slip of about 2.75 m, although this result is not unique. If the slip has been continuous since the 1964 earthquake, then the average slip rate is nearly 100 mm/yr, twice the plate convergence rate. Comparing the net uplift achieved in 29 years with that observed over 11 years in an adjacent region southeast of Anchorage, Alaska, we conclude that the rate of uplift is decreasing. A further decrease in the uplift rate is expected as the 29-year averaged displacement rate is about twice the plate convergence rate and therefore cannot be sustained over the entire earthquake cycle. C1 HUGHES STX CORP, LANHAM, MD 20706 USA. NOAA, NATL GEODET SURVEY, SILVER SPRING, MD 20910 USA. RP COHEN, S (reprint author), NASA, GODDARD SPACE FLIGHT CTR, CODE 921, GREENBELT, MD 20771 USA. NR 28 TC 14 Z9 15 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD FEB 10 PY 1995 VL 100 IS B2 BP 2031 EP 2038 DI 10.1029/94JB02880 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA QH690 UT WOS:A1995QH69000008 ER PT J AU SANTEE, ML READ, WG WATERS, JW FROIDEVAUX, L MANNEY, GL FLOWER, DA JARNOT, RF HARWOOD, RS PECKHAM, GE AF SANTEE, ML READ, WG WATERS, JW FROIDEVAUX, L MANNEY, GL FLOWER, DA JARNOT, RF HARWOOD, RS PECKHAM, GE TI INTERHEMISPHERIC DIFFERENCES IN POLAR STRATOSPHERIC HNO3, H2O, CIO, AND O-3 SO SCIENCE LA English DT Article ID ATMOSPHERE RESEARCH SATELLITE; TOTAL REACTIVE NITROGEN; MICROWAVE LIMB SOUNDER; ANTARCTIC STRATOSPHERE; SOUTHERN-HEMISPHERE; OZONE DEPLETION; WATER-VAPOR; LATE WINTER; VORTEX; DENITRIFICATION AB Simultaneous global measurements of nitric acid (HNO3), water (H2O), chlorine monoxide (ClO), and ozone (O-3) in the stratosphere have been obtained over complete annual cycles in both hemispheres by the Microwave Limb Sounder on the Upper Atmosphere Research Satellite. A sizeable decrease in gas-phase HNO3 was evident in the lower stratospheric vortex over Antarctica by early June 1992, followed by a significant reduction in gas-phase H2O after mid-July. By mid-August, near the time of peak ClO, abundances of gas-phase HNO3 and H2O were extremely low. The concentrations of HNO3 and H2O over Antarctica remained depressed into November, well after temperatures in the lower stratosphere had risen above the evaporation threshold for polar stratospheric clouds, implying that denitrification and dehydration had occurred. No large decreases in either gas-phase HNO3 or H2O were observed in the 1992-1993 Arctic winter vortex. Although ClO was enhanced over the Arctic as it was over the Antarctic, Arctic O-3 depletion was substantially smaller than that over Antarctica, A major factor currently limiting the formation of an Arctic ozone ''hole'' is the lack of denitrification in the northern polar vortex, but future cooling of the lower stratosphere could lead to more intense denitrification and consequently larger losses of Arctic ozone. C1 UNIV EDINBURGH,DEPT METEOROL,EDINBURGH EH9 3JZ,MIDLOTHIAN,SCOTLAND. HERIOT WATT UNIV,DEPT PHYS,EDINBURGH EH14 4AS,MIDLOTHIAN,SCOTLAND. RP SANTEE, ML (reprint author), CALTECH,JET PROP LAB,MAIL STOP 183-701,PASADENA,CA 91109, USA. NR 45 TC 87 Z9 87 U1 1 U2 12 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD FEB 10 PY 1995 VL 267 IS 5199 BP 849 EP 852 DI 10.1126/science.267.5199.849 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA QG207 UT WOS:A1995QG20700047 PM 17813911 ER PT J AU GLOERSEN, P AF GLOERSEN, P TI MODULATION OF HEMISPHERIC SEA-ICE COVER BY ENSO EVENTS SO NATURE LA English DT Article ID TERRESTRIAL FREE OSCILLATIONS; TAPER SPECTRAL-ANALYSIS AB THE El Nino/Southern Oscillation (ENSO) is a quasiperiodic variation in climate which arises from a complex interaction between the tropical Pacific Ocean and the atmosphere(1). ENSO events, which occur every two to seven years, are the largest source of interannual variability of temperature and precipitation on a global scale, although their effects are most profound in the tropics(1). Observations of sea-ice margins have been used to monitor global climate changes on timescales of greater than a decade(2), and there is some evidence for interannual variations in records of sea-ice cover(3). But short-term changes in sea-ice cover are masked by pronounced seasonal variations, making it difficult to correlate them with specific climate phenomena. Using a multiple-window harmonic analysis technique(4-8), I show here that time series of sea-ice cover from the Arctic and Antarctic contain statistically significant quasi-biennial and quasi-quadrennial periodicities that agree well with variations in the ENSO index. The response of sea ice to these two frequency components varies greatly for different regions. RP GLOERSEN, P (reprint author), NASA,GODDARD SPACE FLIGHT CTR,OCEANS & ICE BRANCH,HYDROSPHER RES LAB,GREENBELT,MD 20771, USA. NR 16 TC 97 Z9 103 U1 1 U2 11 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD FEB 9 PY 1995 VL 373 IS 6514 BP 503 EP 506 DI 10.1038/373503a0 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA QF724 UT WOS:A1995QF72400053 ER PT J AU MCCORMICK, MP THOMASON, LW TREPTE, CR AF MCCORMICK, MP THOMASON, LW TREPTE, CR TI ATMOSPHERIC EFFECTS OF THE MT-PINATUBO ERUPTION SO NATURE LA English DT Review ID POLAR STRATOSPHERIC CLOUD; MOUNT-PINATUBO; VOLCANIC AEROSOLS; OZONE DEPLETION; TROPICAL OZONE; INSITU MEASUREMENTS; LIDAR OBSERVATIONS; SULFATE AEROSOLS; GLOBAL OZONE; EL-CHICHON AB The eruption of Mt Pinatubo in June 1991 caused the largest perturbation this century to the particulate content of the stratosphere. The radiative influence of the injected particles put an end to several years of globally warm surface temperatures. At the same time, the combined effect of volcanic particles and anthropogenic reactive chlorine has led to record low levels of stratospheric ozone. C1 SCI APPLICAT INT CORP,HAMPTON,VA 23666. RP MCCORMICK, MP (reprint author), NASA,LANGLEY RES CTR,DIV ATMOSPHER SCI,HAMPTON,VA 23681, USA. OI Thomason, Larry/0000-0002-1902-0840 NR 79 TC 470 Z9 490 U1 21 U2 119 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD FEB 2 PY 1995 VL 373 IS 6513 BP 399 EP 404 DI 10.1038/373399a0 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA QE670 UT WOS:A1995QE67000047 ER PT J AU SANDLER, H VERNIKOS, J WEGMANN, HM KLEIN, KE AF SANDLER, H VERNIKOS, J WEGMANN, HM KLEIN, KE TI COUNTERMEASURES - EXTENDING MANNED SPACEFLIGHT - INTRODUCTION SO ACTA ASTRONAUTICA LA English DT Editorial Material C1 NASA,LIFE & BIOMED SCI APPLICAT,WASHINGTON,DC 20546. DLR,INST AEROSP MED,COLOGNE,GERMANY. RP SANDLER, H (reprint author), WRIGHT STATE UNIV,DEPT COMMUNITY MED,DAYTON,OH 45401, USA. NR 0 TC 3 Z9 9 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD FEB-MAR PY 1995 VL 35 IS 4-5 BP 247 EP 251 DI 10.1016/0094-5765(95)90004-7 PG 5 WC Engineering, Aerospace SC Engineering GA QR996 UT WOS:A1995QR99600001 PM 11541469 ER PT J AU VERNIKOS, J AF VERNIKOS, J TI PHARMACOLOGICAL APPROACHES SO ACTA ASTRONAUTICA LA English DT Review AB ''The place of drugs in manned space flight must now be carefully considered, because a number of physical and physiological consequences of space flight appear unlikely to be resolved by engineering methods alone.'' RP VERNIKOS, J (reprint author), NASA,LIFE & BIOMED SCI APPLICAT,WASHINGTON,DC 20546, USA. NR 0 TC 2 Z9 4 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD FEB-MAR PY 1995 VL 35 IS 4-5 BP 281 EP 295 DI 10.1016/0094-5765(95)98733-P PG 15 WC Engineering, Aerospace SC Engineering GA QR996 UT WOS:A1995QR99600004 PM 11541472 ER PT J AU FINNERAN, M AF FINNERAN, M TI A FORWARD-LOOKING TECHNOLOGY GOES COMMERCIAL SO AEROSPACE AMERICA LA English DT Article RP FINNERAN, M (reprint author), NASA,LANGLEY RES CTR,HAMPTON,VA 23665, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0740-722X J9 AEROSPACE AM JI Aerosp. Am. PD FEB PY 1995 VL 33 IS 2 BP 28 EP 32 PG 5 WC Engineering, Aerospace SC Engineering GA QF563 UT WOS:A1995QF56300011 ER PT J AU LOCKARD, DP BRENTNER, KS ATKINS, HL AF LOCKARD, DP BRENTNER, KS ATKINS, HL TI HIGH-ACCURACY ALGORITHMS FOR COMPUTATIONAL AEROACOUSTICS SO AIAA JOURNAL LA English DT Article AB This paper presents an analysis of high-bandwidth operators developed for use with an essentially nonoscillatory (ENO) method, The spatial operators of a sixth-order ENO code are modified to resolve waves with as few as 7 points per wavelength (PPW) by decreasing the formal order of the algorithm, Numerical and analytical solutions are compared for the model problems of plane-wave propagation and sound generation by an oscillating sphere. These problems involve linear propagation, wave steepening, and shock formation, An analysis of the PPW required for sufficient accuracy shows that low-order algorithms need an excessive number of grid points to produce acceptable solutions, In contrast, high-order codes provide good predictions on relatively coarse grids. The high-bandwidth operators produce only modest improvements over the original sixth-order operators for nonlinear problems in which wave steepening is significant; however, they clearly outperform the original operators for long-distance linear propagation. Because the high-bandwidth operators have the same stencil as the original sixth-order operators, these gains are achieved with no additional computational work. C1 GEORGE WASHINGTON UNIV,JOINT INST ADVANCEMENT FLIGHT SCI,HAMPTON,VA 23681. NASA,LANGLEY RES CTR,DIV FLUID MECH & ACOUST,AERODYNAM & ACOUST METHODS BRANCH,HAMPTON,VA 23681. NR 10 TC 44 Z9 44 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0001-1452 J9 AIAA J JI AIAA J. PD FEB PY 1995 VL 33 IS 2 BP 246 EP 251 DI 10.2514/3.12436 PG 6 WC Engineering, Aerospace SC Engineering GA QK492 UT WOS:A1995QK49200008 ER PT J AU RAMAN, G CORNELIUS, D AF RAMAN, G CORNELIUS, D TI JET MIXING CONTROL USING EXCITATION FROM MINIATURE OSCILLATING JETS SO AIAA JOURNAL LA English DT Note ID TURBULENCE C1 STANFORD UNIV, DEPT AERONAUT & ASTRONAUT, STANFORD, CA 94305 USA. RP NYMA INC, NASA, LEWIS RES CTR GRP, EXPTL FLUID DYNAM SECT, BROOKPARK, OH 44142 USA. NR 11 TC 25 Z9 25 U1 0 U2 0 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD FEB PY 1995 VL 33 IS 2 BP 365 EP 368 DI 10.2514/3.12444 PG 4 WC Engineering, Aerospace SC Engineering GA QK492 UT WOS:A1995QK49200026 ER PT J AU GURUSWAMY, GP BYUN, C AF GURUSWAMY, GP BYUN, C TI DIRECT COUPLING OF EULER PLOW EQUATIONS WITH PLATE FINITE-ELEMENT STRUCTURES SO AIAA JOURNAL LA English DT Note RP GURUSWAMY, GP (reprint author), NASA,AMES RES CTR,COMPUTAT AEROSCI BRANCH,MCAT INST,MOFFETT FIELD,CA 94035, USA. NR 9 TC 4 Z9 4 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0001-1452 J9 AIAA J JI AIAA J. PD FEB PY 1995 VL 33 IS 2 BP 375 EP 377 DI 10.2514/3.12378 PG 3 WC Engineering, Aerospace SC Engineering GA QK492 UT WOS:A1995QK49200030 ER PT J AU RYER, CH OLLA, BL AF RYER, CH OLLA, BL TI INFLUENCES OF FOOD DISTRIBUTION ON FISH FORAGING BEHAVIOR SO ANIMAL BEHAVIOUR LA English DT Article ID JUVENILE WALLEYE POLLOCK; THERAGRA-CHALCOGRAMMA; VERTICAL-DISTRIBUTION; INFORMATION-TRANSFER; LOCAL ENHANCEMENT; AGGREGATIONS; FACILITATION; ENVIRONMENT; STRATEGIES; PREDATORS AB Juvenile walleye pollock, Theragra chalcogramma, use group foraging, mediated by local enhancement, when searching for prey that are clumped in time and space. Local enhancement occurs when fish are attracted to the site where another fish has discovered food. Experiments were conducted to determine whether fish forage as individuals when food is widely dispersed in time and space. When acclimatized to dispersed food, juvenile walleye pollock foraged as individuals and did not respond to the food discovery of others. Some fish appeared to aggressively defend areas of their tank, a behaviour not seen in fish foraging for clumped food. In a second experiment, examining the role of prior experience in fish foraging, fish were first acclimatized to clumped food and then suddenly switched to dispersed food. Fish continued to use group foraging, mediated by local enhancement, with no change over 20 food discovery events. These results indicate that social aspects of fish foraging strategies are flexible, but are also influenced by prior experience with resource distribution. RP RYER, CH (reprint author), OREGON STATE UNIV,HATFIELD MARINE SCI CTR,NOAA,NATL MARINE FISHERIES SERV,ALASKA FISHERIES SCI C,NEWPORT,OR 97365, USA. NR 44 TC 36 Z9 37 U1 0 U2 5 PU ACADEMIC PRESS (LONDON) LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD FEB PY 1995 VL 49 IS 2 BP 411 EP 418 DI 10.1006/anbe.1995.0054 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA QH123 UT WOS:A1995QH12300012 ER PT J AU LAAKSO, H AGGSON, TL PFAFF, RF AF LAAKSO, H AGGSON, TL PFAFF, RF TI PLASMA GRADIENT EFFECTS ON DOUBLE-PROBE MEASUREMENTS IN THE MAGNETOSPHERE SO ANNALES GEOPHYSICAE-ATMOSPHERES HYDROSPHERES AND SPACE SCIENCES LA English DT Article ID ELECTRIC-FIELD MEASUREMENTS; MAGNETOPAUSE AB The effects on double-probe electric field measurements induced by electron density and temperature gradients are investigated. We show that on some occasions such gradients may lead to marked spurious electric fields if the probes are assumed to lie at the same probe potential with respect to the plasma. The use of a proper bias current will decrease the magnitude of such an error. When the probes are near the plasma potential, the magnitude of these error signals, delta E, can vary as delta E similar to T-e(Delta n(e)/n(e)) + 0.5 Delta T-e where T-e is the electron temperature, Delta n(e)/n(e) the relative electron density variation between the two sensors, and Delta T-e the electron temperature difference between the two sensors. This not only implies that the error signals will increase linearly with the density variations but also that such signatures grow with T-e, i.e., such effects are 10 times larger in a 10-eV plasma than in a 1-eV plasma. This type of error is independent of the probe separation distance provided the gradient scale length is much larger than this distance. The largest errors occur when the probes are near to the plasma potential. At larger positive probe potentials with respect to the plasma potential, the error becomes smaller if the probes are biased, as is usually the case with spherical double-probe experiments in the tenuous magnetospheric plasmas. The crossing of a plasma boundary (like the plasmapause or magnetopause) yields an error signal of a single peak. During the crossing of a small structure (e.g., a double layer) the error signal appears as a bipolar signature. Our analysis shows that errors in double-probe measurements caused by plasma gradients are not significant at large scale (much greater than 1 km) plasma boundaries, and may only be important in cases where small-scale (< 1 km), internal gradient structures exist. Bias currents tailored for each plasma parameter regime (i.e., variable bias current) would improve the double-probe response to gradient effects considerably. C1 NASA,GODDARD SPACE FLIGHT CTR,EXTRATERR PHYS LAB,GREENBELT,MD 20771. RI Pfaff, Robert/F-5703-2012 OI Pfaff, Robert/0000-0002-4881-9715 NR 20 TC 16 Z9 16 U1 0 U2 3 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0992-7689 J9 ANN GEOPHYS JI Ann. Geophys.-Atmos. Hydrospheres Space Sci. PD FEB PY 1995 VL 13 IS 2 BP 130 EP 146 DI 10.1007/s00585-995-0130-z PG 17 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA QK495 UT WOS:A1995QK49500003 ER PT J AU LESTER, M LOCKWOOD, M YEOMAN, TK COWLEY, SWH LUHR, H BUNTING, R FARRUGIA, CJ AF LESTER, M LOCKWOOD, M YEOMAN, TK COWLEY, SWH LUHR, H BUNTING, R FARRUGIA, CJ TI THE RESPONSE OF IONOSPHERIC CONVECTION IN THE POLAR-CAP TO SUBSTORM ACTIVITY SO ANNALES GEOPHYSICAE-ATMOSPHERES HYDROSPHERES AND SPACE SCIENCES LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; RADAR AURORAL BACKSCATTER; BOUNDARY-LAYER MODEL; CENTRAL PLASMA SHEET; MAGNETOSPHERIC SUBSTORMS; POLARIZATION PATTERNS; ION FLOWS; IMF-BY; EISCAT; MAGNETOTAIL AB We report multi-instrument observations during an isolated substorm on 17 October 1989. The EISCAT radar operated in the SP-UK-POLI mode measuring ionospheric convection at latitudes 71 degrees Lambda-78 degrees Lambda. SAMNET and the EISCAT magnetometer Cross provide information on the timing of substorm expansion phase onset and subsequent intensifications, as well as the location of the field aligned and ionospheric currents associated with the substorm current wedge. IMP-8 magnetic field data are also included. Evidence of a substorm growth phase is provided by the equatorward motion of a flow reversal boundary across the EISCAT radar field of view at 2130 MLT, following a southward turning of the interplanetary magnetic field (IMF). We infer that the polar cap expanded as a result of the addition of open magnetic flux to the tail lobes during this interval. The flow reversal boundary, which is a lower limit to the polar cap boundary, reached an invariant latitude equator-ward of 71 degrees Lambda by the time of the expansion phase onset. A westward electrojet, centred at 65.4 degrees Lambda, occurred at the onset of the expansion phase. This electrojet subsequently moved poleward to a maximum of 68.1 degrees Lambda at 2000 UT and also widened. During the expansion phase, there is evidence of bursts of plasma flow which are spatially localised at longitudes within the substorm current wedge and which occurred well poleward of the westward electrojet. We conclude that the substorm onset region in the ionosphere, defined by the westward electrojet, mapped to a part of the tail radially earthward of the boundary between open and closed magnetic flux, the ''distant'' neutral line. Thus the substorm was not initiated at the distant neutral line, although there is evidence that it remained active during the expansion phase. It is not obvious whether the electrojet mapped to a near-Earth neutral line, but at its most poleward, the expanded electrojet does not reach the estimated latitude of the polar cap boundary. C1 RUTHERFORD APPLETON LAB,DIDCOT OX11 0QX,OXON,ENGLAND. UNIV LONDON IMPERIAL COLL SCI TECHNOL & MED,BLACKETT LAB,LONDON SW7 2BZ,ENGLAND. TECH UNIV CAROLO WILHELMINA BRAUNSCHWEIG,INST GEOPHYS & METEOROL,D-38106 BRAUNSCHWEIG,GERMANY. UNIV YORK,DEPT PHYS,YORK YO1 5DD,N YORKSHIRE,ENGLAND. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP LESTER, M (reprint author), UNIV LEICESTER,DEPT PHYS & ASTRON,LEICESTER LE1 7RH,LEICS,ENGLAND. RI Lockwood, Mike/G-1030-2011; Yeoman, Timothy/L-9105-2014 OI Lockwood, Mike/0000-0002-7397-2172; Yeoman, Timothy/0000-0002-8434-4825 NR 42 TC 6 Z9 6 U1 0 U2 2 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0992-7689 J9 ANN GEOPHYS JI Ann. Geophys.-Atmos. Hydrospheres Space Sci. PD FEB PY 1995 VL 13 IS 2 BP 147 EP 158 DI 10.1007/s00585-995-0147-3 PG 12 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA QK495 UT WOS:A1995QK49500004 ER PT J AU JAHNKE, LL SUMMONS, RE DOWLING, LM ZAHIRALIS, KD AF JAHNKE, LL SUMMONS, RE DOWLING, LM ZAHIRALIS, KD TI IDENTIFICATION OF METHANOTROPHIC LIPID BIOMARKERS IN COLD-SEEP MUSSEL GILLS - CHEMICAL AND ISOTOPIC ANALYSIS SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID BACTERIUM METHYLOCOCCUS-CAPSULATUS; MONOUNSATURATED FATTY-ACID; METHANE-UTILIZING BACTERIA; DEEP-SEA MUSSELS; STEROL COMPOSITION; METHYL STEROL; BIOSYNTHESIS; CARBON; SYMBIOSIS; PATHWAY AB A lipid analysis of the tissues of a cold-seep mytilid mussel collected from the Louisiana slope of the Gulf of Mexico was used in conjunction with a compound-specific isotope analysis to demonstrate the presence of methanotrophic symbionts in the mussel gill tissue and to demonstrate the host's dependence on bacterially synthesized metabolic intermediates. The gill tissue contained large amounts of group-specific methanotrophic biomarkers, bacteriohopanoids, 4-methylsterols, lipopolysaccharide-associated hydroxy fatty acids, and type I-specific 16:1 fatty acid isomers with bond positions at Delta 8, Delta 10, and Delta 11. Only small amounts of these compounds were detected in the mantle or other tissues of the host animal. A variety of cholesterol and 4-methylsterol isomers were identified as both free and steryl esters, and the sterol double bond positions suggested that the major bacterially derived gill sterol [11.0% 4 alpha-methyl-cholesta-8(14),24-dien-3 beta-ol] was converted to host cholesterol (64.2% of the gill sterol was cholest-5-en-3 beta-ol). The stable carbon isotope values for gill and mantle preparations were, respectively, -59.0 and -60.4 parts per thousand for total tissue, -60.6 and -62.4 parts per thousand for total lipids, -60.2 and -63.9 parts per thousand for phospholipid fatty acids, and -71.8 and -73.8 parts per thousand for sterols. These stable carbon isotope values revealed that the relative fractionation pattern was similar to the patterns obtained in pure culture experiments with methanotrophic bacteria (R. E. Summons, L. L. Jahnke, and Z. Roksandic, Geochim. Cosmochim. Acta 58:2853-2863, 1994) further supporting the conversion of the bacterial methylsterol pool. C1 AUSTRALIAN GEOL SURVEY ORG,CANBERRA,ACT 2601,AUSTRALIA. SETI INST,MT VIEW,CA 94043. RP JAHNKE, LL (reprint author), NASA,AMES RES CTR,M-S 239-4,MOFFETT FIELD,CA 94035, USA. FU NINDS NIH HHS [NSF-EAR-9158113] NR 54 TC 65 Z9 66 U1 1 U2 5 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1325 MASSACHUSETTS AVENUE, NW, WASHINGTON, DC 20005-4171 SN 0099-2240 J9 APPL ENVIRON MICROB JI Appl. Environ. Microbiol. PD FEB PY 1995 VL 61 IS 2 BP 576 EP 582 PG 7 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA QF428 UT WOS:A1995QF42800028 PM 11536707 ER PT J AU WERNICKE, JT MEIER, D MIZUGUCHI, K DAMM, G ABER, G BENKOWSKI, R NOSE, Y NOON, GP DEBAKEY, ME AF WERNICKE, JT MEIER, D MIZUGUCHI, K DAMM, G ABER, G BENKOWSKI, R NOSE, Y NOON, GP DEBAKEY, ME TI FLUID DYNAMIC ANALYSIS USING FLOW VISUALIZATION OF THE BAYLOR/NASA IMPLANTABLE AXIAL-FLOW BLOOD PUMP FOR DESIGN IMPROVEMENT SO ARTIFICIAL ORGANS LA English DT Article DE FLOW VISUALIZATION; FLUID DYNAMIC ANALYSIS; AXIAL FLOW VENTRICULAR ASSIST; HEMOLYSIS AB The Baylor/NASA Axial Blood Flow Pump has been developed for use as an implantable left ventricular assist device (LVAD). The pump is intended as an assist device for either pulmonary or systemic circulatory support for more than 3-months' duration. To date the pump provides acceptable results in terms of thrombus formation and hemolysis (IH of 0.018 g/100 L). A fluid dynamics analysis using flow visualization was performed to investigate the flow fields and to determine areas within the pump that could be improved. These studies focused upon the inflow area in front of the pump. A prototype axial flow pump assembly was constructed to facilitate the flow visualization studies. Particle image tracking velocimetry techniques were used to measure Amberlite particles suspended in a blood analog fluid composed of 63% water and 37% glycerin. This method used a pulsed (612 Hz) laser light to determine flow velocity profiles, shear stress, Reynolds numbers, and stagnant areas within the axial pump. These studies showed that the flow straightener (a vaned assembly in the pump inflow) reduced Reynolds numbers from 4,640 to 2,540 (at 8.5 L/min) and that the flow straightener exacerbates a discontinuity found between it and the impeller. Within the inflow area, a maximum of 80 N/m(2) shear stress was measured, which is well below published blood damage thresholds. Design variations were investigated resulting in a smoother flow transition between flow straightener and impeller. These variations must be investigated further to establish a correlation with hemolysis and thrombus formation. C1 UNIV ROSTOCK,INST BIOMED ENGN & MED INFORMAT,O-2500 ROSTOCK,GERMANY. NASA,LYNDON B JOHNSON SPACE CTR,HOUSTON,TX 77058. RP WERNICKE, JT (reprint author), BAYLOR COLL MED,DEPT SURG,1 BAYLOR PLAZA,HOUSTON,TX 77030, USA. NR 15 TC 21 Z9 22 U1 0 U2 5 PU BLACKWELL SCIENCE PUBL INC CAMBRIDGE PI CAMBRIDGE PA 238 MAIN ST, CAMBRIDGE, MA 02142 SN 0160-564X J9 ARTIF ORGANS JI Artif. Organs PD FEB PY 1995 VL 19 IS 2 BP 161 EP 177 DI 10.1111/j.1525-1594.1995.tb02306.x PG 17 WC Engineering, Biomedical; Transplantation SC Engineering; Transplantation GA QK491 UT WOS:A1995QK49100008 PM 7763196 ER PT J AU NEMEC, JM MATEO, M SCHOMBERT, JM AF NEMEC, JM MATEO, M SCHOMBERT, JM TI B,V-PHOTOMETRY OF THE RR-LYRAE STARS IN THE VERY METAL-POOR GLOBULAR-CLUSTER NGC-5053 SO ASTRONOMICAL JOURNAL LA English DT Article ID PHASE-DISPERSION-MINIMIZATION; OOSTERHOFF PERIOD GROUPS; HORIZONTAL-BRANCH; EVOLUTION; NGC-5053; PROGRAM; GALAXY; SYSTEM; AGE C1 YORK UNIV,DEPT PHYS & ASTRON,N YORK,ON M3J 1P3,CANADA. UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. CALTECH,JET PROP LAB,IPAC,PASADENA,CA 91125. PALOMAR OBSERV,PASADENA,CA. CANADA FRANCE HAWAII TELESCOPE CORP,KAMUELA,HI 96743. NATL RES COUNCIL CANADA,HERZBERG INST ASTROPHYS,DOMINION ASTROPHYS OBSERV,OTTAWA,ON,CANADA. NR 34 TC 10 Z9 10 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 1995 VL 109 IS 2 BP 618 EP 638 DI 10.1086/117306 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD967 UT WOS:A1995QD96700016 ER PT J AU SHURE, M SELLGREN, K JONES, TJ KLEBE, D AF SHURE, M SELLGREN, K JONES, TJ KLEBE, D TI NEAR-INFRARED POLARIZATION IN THE BIPOLAR OUTFLOW OH-0739-14 SO ASTRONOMICAL JOURNAL LA English DT Article ID RADIATIVE-TRANSFER; OPTICAL-PROPERTIES; COOL STARS; OH-0739-14; NEBULAE; OBJECTS; GRAINS; DUST; OH231.8+4.2; NEBULOSITY C1 OHIO STATE UNIV,DEPT ASTRON,COLUMBUS,OH 43210. UNIV MINNESOTA,DEPT ASTRON,MINNEAPOLIS,MN 55455. UNIV DENVER,DEPT PHYS,DENVER,CO 80208. RP SHURE, M (reprint author), UNIV HAWAII,NASA,INST ASTRON,INFRARED TELESCOPE FACIL,HONOLULU,HI 96822, USA. NR 46 TC 21 Z9 21 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 1995 VL 109 IS 2 BP 721 EP 728 DI 10.1086/117314 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD967 UT WOS:A1995QD96700024 ER PT J AU INDEBETOUW, R NORIEGACRESPO, A AF INDEBETOUW, R NORIEGACRESPO, A TI THEORETICAL POSITION-VELOCITY DIAGRAMS OF FLUX, ELECTRON-DENSITY, AND ELECTRON-TEMPERATURE IN HERBIG-HARO OBJECTS SO ASTRONOMICAL JOURNAL LA English DT Article ID INTERSTELLAR BOW SHOCKS; EMISSION-LINE PROFILES; PREDICTED LONG-SLIT; HIGH-RESOLUTION; STELLAR JET; MODELS; EXCITATION; HH-1 C1 CALTECH,CTR INFRARED PROC & ANAL,JET PROPULS LAB,PASADENA,CA 91125. RP INDEBETOUW, R (reprint author), MARIA MITCHELL OBSERV,3 VESTAL ST,NANTUCKET,MA 02554, USA. NR 25 TC 10 Z9 10 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 1995 VL 109 IS 2 BP 752 EP 761 DI 10.1086/117318 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD967 UT WOS:A1995QD96700028 ER PT J AU CASTETS, A LANGER, WD AF CASTETS, A LANGER, WD TI PHYSICAL-PROPERTIES OF THE OMC-2 AND OMC-3 CORES FROM CS AND C18O OBSERVATIONS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE INTERSTELLAR MEDIUM, CLOUDS; JETS AND OUTFLOWS; STRUCTURE; INDIVIDUAL OBJECTS, OMC-2, OMC-3 ID ORION MOLECULAR CLOUD-2; STAR-FORMING REGION; CARBON-MONOXIDE; DENSE CORES; DARK CLOUDS; MULTITRANSITION; EXCITATION; EMISSION; LINE; CO AB We have investigated the properties of the OMC-2 and OMC-3 cores in the Orion giant molecular cloud using high spatial and spectral resolution observations of several transitions of the CO-13, C-18O, C-32S and C-34S molecules taken with the SEST telescope. The OMC-2 core consists of one clump (22 M(.)) with a radius of 0.11 pc surrounded by a cluster of 11 discrete infrared sources. The H2 column density and volume density in the center of this clump are 2 10(22) cm-2 and 9 10(5) cm-3 respectively. From a comparison between physical parameters derived from C-18O and C-32S observations we conclude that the molecular envelope around the core has been completely removed by these sources and that only the very dense gas is left. OMC-3 shows a more complex elongated structure in C-18O and CS than OMC-2. The C-32S and C34S maps show that the denser region can be separated into at least three sub-cores of roughly equal sizes (radius almost-equal-to 0.13 pc), with n(H2) = 6 10(5) cm-3, and a mass of 10M(.) (from C32S). The very different masses obtained for the central core from C-18-O and C-32S (35 and 12M(.)respectively) indicate that a massive envelope is still present around the very dense sub-cores. We report the first detection of several molecular outflows in OMC-3. The presence of an IRAS source and the first detection of these outflows confirm that star formation is going on in OMC-3. Based on the different physical properties of these regions compared with OMC-1, OMC-2 appears to be in an intermediate evolutionary stage between OMC-1 and OMC-3. C1 JET PROP LAB, PASADENA, CA 91109 USA. RP CASTETS, A (reprint author), OBSERV GRENOBLE, ASTROPHYS LAB, BP 53, F-38041 GRENOBLE 9, FRANCE. NR 39 TC 32 Z9 33 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 FEB PY 1995 VL 294 IS 3 BP 835 EP 854 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QJ325 UT WOS:A1995QJ32500025 ER PT J AU DODELSON, S JUBAS, JM AF DODELSON, S JUBAS, JM TI REIONIZATION AND ITS IMPRINT ON THE COSMIC MICROWAVE BACKGROUND SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC MICROWAVE BACKGROUND; COSMOLOGY, THEORY; EARLY UNIVERSE ID DARK-MATTER; RADIATION ANISOTROPIES; SCALE; UNIVERSE; FLUCTUATIONS; CONSTRAINTS AB Early reionization changes the pattern of anisotropies expected in the cosmic microwave background. To explore these changes, we derive from first principles the equations governing anisotropies, focusing on the interactions of photons with electrons. Vishniac (1987) claimed that second-order terms can be large in a reionized universe, so we derive equations correct to second order in the perturbations. There are many more second-order terms than were considered by Vishniac. To understand the basic physics involved, we present a simple analytic approximation to the first-order equation. Then, turning to the second order equation, we show that the Vishniac term is indeed the only important one. We also present numerical results for a variety of ionization histories (in a standard cold dark matter universe) and show quantitatively how the signal in several experiments depends on the ionization history. The most pronounced indication of a reionized universe would be seen in very small scale experiments; the expected signal in the Owens Valley experiment is smaller by a factor of order 10 if the last scattering surface is at a redshift z similar or equal to 100 as it would be if the universe were reionized very early. On slightly larger scales, the expected signal in a reionized universe is smaller than it would be with standard recombination, but only by a factor of 2 or so. The signal is even smaller in these experiments in the intermediate case where some photons last scattered at the standard recombination epoch. C1 MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. RP DODELSON, S (reprint author), FERMILAB NATL ACCELERATOR LAB, NASA, FERMILAB ASTROPHYS CTR, POB 500, BATAVIA, IL 60510 USA. NR 32 TC 83 Z9 83 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 1 PY 1995 VL 439 IS 2 BP 503 EP 516 DI 10.1086/175191 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500001 ER PT J AU NORRIS, JP BONNELL, JT NEMIROFF, RJ SCARGLE, JD KOUVELIOTOU, C PACIESAS, WS MEEGAN, CA FISHMAN, GJ AF NORRIS, JP BONNELL, JT NEMIROFF, RJ SCARGLE, JD KOUVELIOTOU, C PACIESAS, WS MEEGAN, CA FISHMAN, GJ TI DURATION DISTRIBUTIONS OF BRIGHT AND DIM BATSE GAMMA-RAY BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMOLOGY, THEORY; GAMMA RAYS, BURSTS AB We have measured the T-90 and T-50 durations of bright and dim gamma-ray bursts detected by the Compton Gamma-Ray Observatory's Burst and Transient Source Experiment (BATSE). The T-90 (T-50) duration is defined as the interval over which 5% (25%) to 95% (75%) of the burst counts accumulate. Out of 775 bursts observed by BATSE, 159 bursts were analyzed; bursts with durations shorter than 1.5 s were excluded. A Kolmogorov-Smirnov test yields a probability of 6 x 10(-5) that the T-50 durations of the dim and bright samples are drawn from the same parent population. We find that the centroid and extent of the duration distribution for the dim sample are scaled by approximately a factor of 2 relative to those of the bright sample. The measured time-dilation factor is not sensitive to choice of energy band. These results are quantitatively consistent with previous tests for time dilation in a smaller sample of BATSE bursts. The sources of dimmer bursts, if cosmological, would lie at redshifts of order 2. C1 GEORGE MASON UNIV,FAIRFAX,VA 22030. NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. UNIV ALABAMA,HUNTSVILLE,AL 35899. RP NORRIS, JP (reprint author), NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771, USA. NR 30 TC 76 Z9 77 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 1995 VL 439 IS 2 BP 542 EP 547 DI 10.1086/175194 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500004 ER PT J AU MICHALITSIANOS, AG OLIVERSEN, RJ AF MICHALITSIANOS, AG OLIVERSEN, RJ TI THE ULTRAVIOLET-SPECTRUM OF THE GRAVITATIONAL LENS CANDIDATE UM-425=QSO-1120+019 - EVIDENCE FOR BROAD ABSORPTION-LINE (BAL) STRUCTURE SO ASTROPHYSICAL JOURNAL LA English DT Article DE GRAVITATIONAL LENSING; QUASARS, ABSORPTION LINES; QUASARS, INDIVIDUAL (QSO 1120+019); ULTRAVIOLET, GALAXIES AB The UV line profile structure of high-ionization resonance lines found with the International Ultraviolet Explorer (IUE) in the brightest of four multiply imaged sources (image-A) in the candidate gravitational lens UM 425 = QSO 1120 + 019 indicates broad absorption line (BAL) structure. The deep-broad trough associated with the O VI line extends to velocities similar to -12,000 km s(-1), and contains discrete features that suggest multicomponent velocity structure. This structure may include contributions from C IV absorption from the early-type galaxy that is believed to lens UM 425. A strong absorption feature in the blue wing of the Lyman-alpha lambda 1216 emission line may be a Lyman-alpha absorption system at a z(Ly alpha) = 1.437 +/- 0.003, or it may be formed by the superposition of the broad N V lambda lambda 1238, 1242 absorption trough on the extended blue emission wing of the QSO Lyman-alpha line. We obtained a redshift of z(QSO) = 1.471 +/- 0.003 from Lyman-alpha lambda 1215, consistent with the redshift found by Meylan and Djorgovski in the optical. The Lyman-alpha line appears unusually weak due to the presence of N V lambda 1240 BAL absorption. A Lyman-limit absorption system at lambda 912 was not observed in the QSO rest frame. The detection of BAL structure in the other weaker ground-state resonance lines of N II (1) and S IV (I) was not found, suggesting these lines are formed in a region that is distinct from the BAL component. Detection of BAL structure in the other fainter images in this system with HST instrumentation, similar to structure observed here in image A, could provide evidence that UM 425 is a gravitational lens. RP MICHALITSIANOS, AG (reprint author), NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,CODE 6841,GREENBELT,MD 20771, USA. NR 20 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 FEB 1 PY 1995 VL 439 IS 2 BP 599 EP 603 DI 10.1086/175200 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500010 ER PT J AU SMITH, DA HERTER, T HAYNES, MP BEICHMAN, CA GAUTIER, TN AF SMITH, DA HERTER, T HAYNES, MP BEICHMAN, CA GAUTIER, TN TI THE LUMINOUS STARBURST GALAXY UGC-8387 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL, (UGC 8387); GALAXIES, INTERACTIONS; GALAXIES, PHOTOMETRY; GALAXIES, STARBURST; INFRARED, GALAXIES ID ULTRALUMINOUS INFRARED GALAXIES; H II REGIONS; STAR FORMATION; INTERACTING GALAXIES; MOLECULAR CLOUDS; STANDARD STARS; IMAGING SURVEY; IRAS GALAXIES; M82; SPECTROSCOPY AB We present broad-band J, H, and K images and K-band spectroscopy of the luminous starburst galaxy UGC 8387. The images show a disturbed morphology, tidal tails, and a single elongated nucleus. Near-infrared color maps constructed from the images reveal that the nuclear region is highly reddened. Strong emission from the central 3.''0 in the 2.166 mu m Brackett gamma, 2.122 mu m H-2 nu = 1-0 S(1), and 2.058 mu m He I lines is present in the K-band spectrum. From the Brackett gamma and published radio fluxes, we find an optical depth toward the nucleus of tau(V) similar to 24. The CO band heads produce strong absorption in the spectral region longward of 2.3 mu m. We measure a ''raw'' CO index of 0.17 +/- 0.02 mag, consistent with a population of K2 supergiants or K4 giants. The nuclear colors, however, are not consistent with an obscured population of evolved stars. Instead, the red colors are best explained by an obscured mixture of stellar and warm dust emission. The amount of dust emission predicted by the near-infrared colors exceeds that expected from comparisons to galactic H II regions. After correcting the spectrum of UGC 8387 for dust emission and extinction, we obtain a CO index of greater than or equal to 0.25 mag. This value suggests the stellar component of the 2.2 mu m light is dominated by young supergiants. The infrared excess, L(IR)/L(Ly alpha), derived for UGC 8387 is lower than that observed in galactic H II regions and M82. This implies that either the lower or upper mass cutoff of the initial mass function must be higher than those of local star-forming regions and M82. The intense nuclear starburst in this galaxy is presumably the result of merger activity, and we estimate the starburst age to be at least a few times 10(7) yr. C1 CORNELL UNIV,CTR RADIOPHYS & SPACE RES,ITHACA,NY 14853. CALTECH,CTR INFRARED PROC & ANAL,PASADENA,CA 91125. CALTECH,JET PROP LAB,PASADENA,CA 91109. KITT PEAK NATL OBSERV,NATL OPT ASTRON OBSERV,TUCSON,AZ 85726. RP SMITH, DA (reprint author), CORNELL UNIV,DEPT ASTRON,SPACE SCI BLDG,ITHACA,NY 14853, USA. NR 62 TC 23 Z9 23 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 1995 VL 439 IS 2 BP 623 EP 636 DI 10.1086/175202 PN 1 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500012 ER PT J AU SEWARD, FD VELUSAMY, T AF SEWARD, FD VELUSAMY, T TI A ROSAT OBSERVATION OF THE SUPERNOVA REMNANT KES-79 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (KES 79); SUPERNOVA REMNANTS; X-RAYS, ISM ID X-RAY OBSERVATIONS; EVOLUTION; G33.6+0.1 AB Kes 79 was observed with the ROSAT PSPC and HRI. Some X-ray emission comes from a faint outer region, well correlated with the outer shell. Most emission is from a bright diffuse inner region where there are also bright radio filaments. The X-fay spectrum is fitted with a thermal model with temperature 1.3 keV. Variations in spectra from different regions are small. There is no X-ray evidence for an internal neutron star. Remnant characteristics are derived using a simple blast-wave model. The observed X-ray absorption is less than expected. It is possible that the remnant is closer than the published distance of 10 kpc. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. RP SEWARD, FD (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,60 GARDEN ST,CAMBRIDGE,MA 02138, USA. NR 13 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 FEB 1 PY 1995 VL 439 IS 2 BP 715 EP 721 DI 10.1086/175211 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500021 ER PT J AU KINGDON, J FERLAND, GJ FEIBELMAN, WA AF KINGDON, J FERLAND, GJ FEIBELMAN, WA TI GRAINS IN IONIZED NEBULAE - SPECTRAL-LINE DIAGNOSTICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE DUST, EXTINCTION; ISM, ABUNDANCES; LINE, PROFILES ID PLANETARY-NEBULAE; ORION NEBULA; PHYSICAL CONDITIONS; INTERSTELLAR ABSORPTION; II EMISSION; ABUNDANCES; MODEL; EXTINCTION; MAGNESIUM; ELEMENTS AB The depletion of condensable elements onto grains in gaseous nebulae can provide evidence that dust is well mixed with the ionized gas. Al and Ca are two of the most depleted elements in the general interstellar medium, and it is therefore important to measure their abundances within the ionized region of nebulae. We compute a large grid of photoionization models and identify sets of line ratios which are relatively insensitive to stellar and nebular parameters, and are thus excellent diagnostics for determining relative abundances. Based on the absence of the [Ca II] lambda lambda 7291, 7324 doublet and the detection of Al II] lambda lambda 2660, 2669 in the ultraviolet, we determine the extent of aluminum and calcium depletion onto grains in NGC 7027 and the Orion Nebula. Our results show a similar to 0.3 dex depletion for Al, but a depletion of more than two and a half orders of magnitude for Ca. A similar calculation based on Mg II lambda 2798 yields roughly a 0.8 dex depletion for Mg. This reaffirms the discrepancy between depletions determined from high and low ionization Mg lines. We also find evidence for a ''depletion gradient'' in Ca in NGC 7027, since the calcium depletion we infer for the outer, more neutral regions using [Ca II] is somewhat higher than that inferred for the inner high-ionization region, using [Ca V]. This gradient can test current models of the survival of grains within hot ionized gas. C1 NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. RP KINGDON, J (reprint author), UNIV KENTUCKY,DEPT PHYS & ASTRON,LEXINGTON,KY 40506, USA. OI Ferland, Gary/0000-0003-4503-6333 NR 42 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 FEB 1 PY 1995 VL 439 IS 2 BP 793 EP 799 DI 10.1086/175217 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500027 ER PT J AU FIELDS, BD OLIVE, KA SCHRAMM, DN AF FIELDS, BD OLIVE, KA SCHRAMM, DN TI IMPLICATIONS OF A HIGH POPULATION-II B/BE RATIO SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC RAYS; NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES; STARS, POPULATION II ID EARLY GALAXY; PRIMORDIAL LITHIUM; NUCLEOSYNTHESIS; BERYLLIUM; ABUNDANCES; EVOLUTION; STARS; LI; ELEMENTS; ORIGIN AB The observed boron/beryllium ratio in extreme Population II stars has been interpreted as evidence of Be and B synthesis by early Galactic cosmic rays. However, a recent reanalysis of the boron abundance in the Population II halo star HD 140283 suggests that B/H may be larger than previously reported, by as much as a factor of 4. This would yield a B/Be ratio lying in the range 14 less than or similar to B/Be less than or similar to 50. The possibility of a high Population II B/Be ratio stresses the importance of the upper limit to the B/Be ratio arising from cosmic-ray production. It is found that the limit to cosmic-ray-produced B/Be depends upon the assumed cosmic-ray spectrum. For any Population II comic-ray spectrum that is a single power law in either total energy per nucleon or in momentum, the B/Be ratio is constrained to lie in the range 7.6 less than or similar to B/Be less than or similar to 14. Thus, if the new B/Be ratio is correct, it requires either a bimodal cosmic-ray flux with a large low-energy component, or, for another B source, possibly the proposed v-process in supernovae, either of which may be helpful in explaining the observed B-11/B-10 ratio. Finally, it is noted that the boron reanalysis highlights the uncertainty in our knowledge of the B/Be ratio, and the need for additional data on Be and B abundances. C1 UNIV MINNESOTA,SCH PHYS & ASTRON,MINNEAPOLIS,MN 55455. FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. RP FIELDS, BD (reprint author), UNIV CHICAGO,CHICAGO,IL 60637, USA. NR 37 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 FEB 1 PY 1995 VL 439 IS 2 BP 854 EP 859 DI 10.1086/175224 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500034 ER PT J AU HUBENY, I LANZ, T AF HUBENY, I LANZ, T TI NON-LTE LINE-BLANKETED MODEL ATMOSPHERES OF HOT STARS .1. HYBRID COMPLETE LINEARIZATION ACCELERATED LAMBDA-ITERATION METHOD SO ASTROPHYSICAL JOURNAL LA English DT Article DE METHODS, NUMERICAL; RADIATIVE TRANSFER; STARS, ATMOSPHERES; STARS, EARLY-TYPE ID MULTILEVEL RADIATIVE-TRANSFER; STELLAR ATMOSPHERES; QUADRATURE PERTURBATIONS; STATISTICAL METHOD; OPERATORS; EQUILIBRIUM; CONTINUUM; HYDROGEN; HELIUM; CARBON AB A new numerical method for computing sophisticated non-LTE model stellar atmospheres is presented. The method, called the hybrid complete linearization/accelerated lambda iteration (CL/ALI) method, combines advantages of both its constituents. Its rate of convergence is virtually as high as for the standard CL method, while the computer time per iteration is almost as low as for the standard ALI method. The method is formulated as the standard complete linearization, the only difference being that the radiation intensity at selected frequency points is not explicitly linearized; instead, it is treated by means of the ALI approach. The scheme offers a wide spectrum of options, ranging from the full CL to the full ALI method. We demonstrate that the method works optimally if the majority of frequency points are treated in the ALI mode, while the radiation intensity at a few (typically two to 30) frequency points is explicitly linearized. We show how this method can be applied to calculate metal line-blanketed non-LTE model atmospheres, by using the idea of ''superlevels'' and ''superlines'' introduced originally by Anderson (1989). We calculate several illustrative models taking into account several tens of thousand of lines of Fe III to Fe VI and show that the hybrid CL/ALI method provides a robust method for calculating non-LTE line-blanketed model atmospheres for a wide range of stellar parameters. The results for individiual stellar types will be presented in subsequent papers in this series. C1 NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. NR 52 TC 820 Z9 821 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 1995 VL 439 IS 2 BP 875 EP 904 DI 10.1086/175226 PN 1 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500036 ER PT J AU LANZ, T HUBENY, I AF LANZ, T HUBENY, I TI NON-LTE LINE-BLANKETED MODEL ATMOSPHERES OF HOT STARS .2. HOT, METAL-RICH WHITE-DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE LINE, FORMATION; STARS, ABUNDANCES; STARS, ATMOSPHERES; ULTRAVIOLET; STARS WHITE DWARFS ID APPROXIMATE LAMBDA OPERATORS; ULTRAVIOLET-SPECTRUM; STELLAR ATMOSPHERES; EUV SPECTRUM; FEIGE 24; HYDROGEN; ACCRETION; EMISSION; OPACITY; CARBON AB We present several model atmospheres for a typical hot metal-rich DA white dwarf, T-eff = 60,000 K, log g = 7.5. We consider pure hydrogen models, as well as models with various abundances of two typical ''trace'' elements-carbon and iron. We calculate a number of LTE and non-LTE models, taking into account the effect of numerous lines of these elements on the atmospheric structure. We demonstrate that while the non-LTE effects are not very significant for pure hydrogen models, except for describing correctly the central emission in Ha, they are essential for predicting correctly the ionization balance of metals, such as carbon and iron. Previously reported discrepancies in LTE abundance determinations using CIII and CIV lines are easily explained by non-LTE effects. We show that if the iron abundance is larger than 10(-5), the iron line opacity has to be considered not only for the spectrum synthesis, but also in the model construction itself. For such metal abundances, non-LTE metal line-blanketed models are needed for detailed abundance studies of hot, metal-rich white dwarfs. We also discuss the predicted EUV spectrum and show that it is very sensitive to metal abundances, as well as to non-LTE effects. RP LANZ, T (reprint author), NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, GREENBELT, MD 20771 USA. NR 44 TC 74 Z9 74 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 1 PY 1995 VL 439 IS 2 BP 905 EP 916 DI 10.1086/175227 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500037 ER PT J AU SION, EM CHENG, FH LONG, KS SZKODY, P GILLILAND, RL HUANG, M HUBENY, I AF SION, EM CHENG, FH LONG, KS SZKODY, P GILLILAND, RL HUANG, M HUBENY, I TI HUBBLE-SPACE-TELESCOPE FOS SPECTROSCOPY OF THE ULTRASHORT-PERIOD DWARF NOVA WZ SAGITTAE - THE UNDERLYING DEGENERATE SO ASTROPHYSICAL JOURNAL LA English DT Article DE NOVAE, CATACLYSMIC VARIABLES; STARS, INDIVIDUAL (WZ SAGITTAE); ULTRAVIOLET, STARS; WHITE DWARFS ID WHITE-DWARF; ATMOSPHERIC ANALYSIS; CARBON; QUIESCENCE; G35-26; SGE AB Two consecutive Hubble Space Telescope Faint Object Spectrograph (FOS) spectra of the exposed white dwarf in the ultrashort-period, high-amplitude, dwarf nova WZ Sge, reveal a rich absorption line spectrum of neutral carbon and ionized metals, the Stark-broadened Ly alpha absorption wing, the H-2 quasi-molecular Ly alpha ''satellite'' absorption line, and a double-peaked C IV emission line which is variable with orbital phase. A synthetic spectral analysis of the white dwarf yields T-eff = 14,900 K +/- 250 K, log g = 8.0. In order to fit the strongest C I absorption lines and account for the weakness of the silicon absorption lines, the abundance of carbon in the photosphere must be similar to 0.5 solar, silicon abundance is 5 x 10(-3) solar, with all other metal species appearing to be 0.1-0.001 times solar. The H-2 quasi-molecular absorption is fitted very successfully. The photospheric metals have diffusion timescales of fractions of a year, and thus they must have been accreted long after the 1978 December outburst. The source of the most abundant metal, carbon, is considered. If the time-averaged accretion rate during quiescence is low enough for diffusive equilibrium to prevail, then the equilibrium accretion rate of neutral carbon is 7 x 10(-16) M. yr(-1). A convective dredge-up origin for the concentration of carbon is extremely unlikely, given that the white dwarf atmosphere is H-rich while in single degenerates showing carbon and hydrogen, the C and H are trace elements in a helium background. Additional implications are explored. C1 UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742. UNIV SCI & TECHNOL CHINA,CTR ASTROPHYS,HEFEI 230026,PEOPLES R CHINA. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98195. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP SION, EM (reprint author), VILLANOVA UNIV,DEPT ASTRON & ASTROPHYS,VILLANOVA,PA 19085, USA. NR 30 TC 44 Z9 44 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 1995 VL 439 IS 2 BP 957 EP 962 DI 10.1086/175232 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500042 ER PT J AU PENDLETON, GN PACIESAS, WS FISHMAN, GJ MEEGAN, CA WILSON, RB AF PENDLETON, GN PACIESAS, WS FISHMAN, GJ MEEGAN, CA WILSON, RB TI BALLOON-BORNE MEASUREMENTS OF THE SN 1987A HARD X-RAY CONTINUUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE BALLOONS; GAMMA RAYS, OBSERVATIONS; SUPERNOVAE, INDIVIDUAL (SN 1987A); X-RAYS, STARS ID SUPERNOVA 1987A; SN-1987A; LIGHT; SPECTRUM; EMISSION AB SN 1987A hard X-ray continuum spectra obtained on 1987 October 29, 1988 April 9-10, and 1988 November 11 from balloon-flight measurements are presented. The spectra, spanning the energy range from 25 keV to 300 keV, have been analyzed using a detector response matrix inversion technique that converts the spectra from counts s(-1) cm(2) keV to photons s(-1) cm(2) keV allowing direct comparison with theoretical models. The results indicate that the bulk of the Co-56 is mixed moderately through the inner regions of the supernova envelope but they do not preclude the mixing of a small amount of the Co-56 farther out into the envelope necessary to account for the observed Co-56 line fluxes. The effect of the ratio Co-57 to (CO)-C-56 on the 1988 November 11 continuum spectrum is discussed. C1 NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. RP PENDLETON, GN (reprint author), UNIV ALABAMA,DEPT PHYS,HUNTSVILLE,AL 35899, USA. NR 21 TC 4 Z9 4 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 1995 VL 439 IS 2 BP 963 EP 975 DI 10.1086/175233 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500043 ER PT J AU FERRERO, RF GOUTTEBROZE, P CATALANO, S MARILLI, E BRUHWEILER, F KONDO, Y VANDERHUCHT, K TALAVERA, A AF FERRERO, RF GOUTTEBROZE, P CATALANO, S MARILLI, E BRUHWEILER, F KONDO, Y VANDERHUCHT, K TALAVERA, A TI CHROMOSPHERIC MODELS FOR ALTAIR (A7 IV-V) SO ASTROPHYSICAL JOURNAL LA English DT Article DE STARS, CHROMOSPHERES; STARS, INDIVIDUAL (ALPHA AQUILLAE); ULTRAVIOLET, STARS ID LOCAL INTERSTELLAR-MEDIUM; EARLY-TYPE STARS; CONVECTION ZONES; MASS-LOSS; EMISSION; REDISTRIBUTION; TEMPERATURES; RADIATION; SPECTRUM; SIRIUS AB The star, Altair (A7 IV-V), is clearly shown to have Ly alpha emission of chromospheric origin, while no evidence is found for the Mg II emission reported in previous investigations. We present non-LTE semiempirical models incorporating partial redistribution of the chromosphere of Altair that reproduce the observed Ly alpha emission and the Mg II resonance absorption at 2800 Angstrom. We unambiguously establish that chromospheres exist at spectral types as early as A7 on the main sequence, and we also demonstrate that it is very unlikely that the observed emission originates in a corotating expanding wind. This result represents a new challenge for chromospheric heating theories. It may indicate that both differential rotation and convective layers, at least near the equator, exist in this fast rotating (v sin i = 220 km s(-1)) star. C1 UNIV PARIS 11, INST ASTROPHYS SPATIALE, F-91405 ORSAY, FRANCE. OSSERV ASTROFIS CATANIA, I-95125 CATANIA, ITALY. CATHOLIC UNIV AMER, DEPT PHYS, WASHINGTON, DC 20064 USA. NASA, GODDARD SPACE FLIGHT CTR, GREENBELT, MD 20771 USA. SRON, 3584 CA UTRECHT, NETHERLANDS. ESA IUE OBSERV, E-28080 MADRID, SPAIN. RP FERRERO, RF (reprint author), OBSERV ASTRON, 11 RUE UNIV, F-67000 STRASBOURG, FRANCE. NR 63 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 1 PY 1995 VL 439 IS 2 BP 1011 EP 1020 DI 10.1086/175238 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD405 UT WOS:A1995QD40500048 ER PT J AU KOGUT, A BANDAY, AJ BENNETT, CL HINSHAW, G LUBIN, PM SMOOT, GF AF KOGUT, A BANDAY, AJ BENNETT, CL HINSHAW, G LUBIN, PM SMOOT, GF TI GAUSSIAN STATISTICS OF THE COSMIC MICROWAVE BACKGROUND - CORRELATION OF TEMPERATURE EXTREMA IN THE COBE DMR 2-YEAR SKY MAPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COSMIC MICROWAVE BACKGROUND; METHODS, STATISTICAL ID FLUCTUATIONS; RADIOMETER; RADIATION AB We use the two-point correlation function of the extrema points (peaks and valleys) in the COBE Differential Microwave Radiometers (DMR) 2 year sky maps as a test for non-Gaussian temperature distribution in the cosmic microwave background anisotropy. A maximum-likelihood analysis compares the DMR data to n = 1 toy models whose random-phase spherical harmonic components a(lm) are drawn from either Gaussian, chi(2), or log-normal parent populations. The likelihood of the 53 GHz (A+B)/2 data is greatest for the exact Gaussian model. There is less than 10% chance that the non-Gaussian models tested describe the DMR data, limited primarily by type II errors in the statistical inference. The extrema correlation function is a stronger test for this class of non-Gaussian models than topological statistics such as the genus. C1 NASA,GODDARD SPACE FLIGHT CTR,UNIV SPACE RES ASSOC,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. UNIV CALIF SANTA BARBARA,DEPT PHYS,SANTA BARBARA,CA 93106. UNIV CALIF BERKELEY,LAWRENCE BERKELEY LAB,SSL,BERKELEY,CA 94720. UNIV CALIF BERKELEY,CIPA,BERKELEY,CA 94720. RP KOGUT, A (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HUGHES STX CORP,ASTRON & SOLAR PHYS LAB,CODE 685,GREENBELT,MD 20771, USA. RI Kogut, Alan/D-6293-2012 NR 13 TC 23 Z9 23 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 1995 VL 439 IS 2 BP L29 EP L32 DI 10.1086/187737 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD407 UT WOS:A1995QD40700001 ER PT J AU WALBORN, NR MACKENTY, JW SAHA, A WHITE, RL PARKER, JW AF WALBORN, NR MACKENTY, JW SAHA, A WHITE, RL PARKER, JW TI RESOLUTION OF MASSIVE COMPACT CLUSTERS IN THE 30-DORADUS PERIPHERY WITH THE HUBBLE-SPACE-TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE OPEN CLUSTERS AND ASSOCIATIONS, INDIVIDUAL (MAGELLANIC CLOUDS); STARS, EARLY-TYPE ID LARGE MAGELLANIC CLOUD; STELLAR CONTENT; STARS AB Hubble Space Telescope Wide Field/Planetary Camera UBV images of three massive, compact multiple systems within the SNR 30 Dor B/NGC 2060 and 30 Dor C/NGC 2044 are discussed and illustrated. In two cases, WN+OB objects have been resolved into additional components to those previously known from ground-based observations, substantially reducing the luminosities of the WN stars and rendering them currently unidentified; in the third case, the components of a B+K composite-spectrum object have been clearly identified. The results are of significance for evolutionary interpretations of these massive stars and for determinations of the upper IMF in extragalactic systems. C1 NASA,GODDARD SPACE FLIGHT CTR,HUGHES STX CORP,CODE 681,GREENBELT,MD 20771. RP WALBORN, NR (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 13 TC 16 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 FEB 1 PY 1995 VL 439 IS 2 BP L47 EP L50 DI 10.1086/187741 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD407 UT WOS:A1995QD40700005 ER PT J AU COLOMBI, S BOUCHET, FR SCHAEFFER, R AF COLOMBI, S BOUCHET, FR SCHAEFFER, R TI A COUNT PROBABILITY COOKBOOK - SPURIOUS EFFECTS AND THE SCALING MODEL SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE GALAXIES, CLUSTERS, GENERAL; METHODS, NUMERICAL; METHODS, STATISTICAL ID INVARIANT MATTER DISTRIBUTION; POINT CORRELATION-FUNCTIONS; GALAXY CORRELATION-FUNCTION; CFA REDSHIFT SURVEY; STATISTICAL-ANALYSIS; EXTRAGALACTIC OBJECTS; EXPANDING UNIVERSE; VOID STATISTICS; CATALOG; FLUCTUATIONS AB We study the errors brought by finite volume effects and dilution effects on the practical determination of the count probability distribution function P-N(n,l), which is the probability of having N objects in a cell of volume l(3) for a set of average number density n. Dilution effects are particularly relevant to the so-called sparse sampling strategy. This work is mainly done in the framework of the Balian and Schaeffer scaling model, which assumes that the e-body correlation functions obey the scaling relation xi(Q)(lambda r(1),...,lambda r(Q)) = lambda (-(Q-1)gamma)xi(Q)(r(1),...,r(Q)). We use three synthetic samples as references to perform our analysis: a fractal generated by a Rayleigh-Levy random walk with similar to 3 X 10(4) objects, a sample dominated by a spherical power-law cluster with similar to 3 X 10(4) objects and a cold dark matter (CDM) universe involving similar to 3 X 10(5) matter particles. The void probability, P-0, is seen to be quite weakly sensitive to finite sample effects, if P(0)Vl(-3)greater than or similar to 1, where Vis the volume of the sample (but P-0 is not immune to spurious grid effects in the case of numerical simulations from such quiet initial conditions). If this condition is met, the scaling model can be tested with a high degree of accuracy. Still, the most interesting regime, when the scaling predictions are quite unambiguous, is reached only when nl(0)(3) greater than or similar to 30-50, where l(0) is the (pseudo-)correlation length at which the averaged two-body correlation function over a cell is unity. For the galaxy distribution, this corresponds to n greater than or similar to 0.02-0.03 h(3)Mpc(-3). The count probability distribution for N not equal 0 is quite sensitive to discreteness effects. Furthermore, the measured large N tail appears increasingly irregular with N, until a sharp cutoff is reached. These wiggles and the cutoff are finite volume effects. It is still possible to use the measurements to test the scaling model properties with a good accuracy, but the sample has to be as dense and large as possible. Indeed the condition nl(0)(3) greater than or similar to 80-120 is required, or equivalently n greater than or similar to 0.04-0.06 h(3) Mpc(-3). The number densities of the current three-dimensional galaxy catalogs are thus not large enough to test fairly the predictions of the scaling model. Of course, these results strongly argue against sparse sampling strategies. C1 INST ASTROPHYS,F-75014 PARIS,FRANCE. CENS,CEA,INST RECH FONDAMENTALE LAB,SERV PHYS THEOR,F-91191 GIF SUR YVETTE,FRANCE. RP COLOMBI, S (reprint author), FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,POB 500,BATAVIA,IL 60510, USA. RI Bouchet, Francois/B-5202-2014 NR 63 TC 44 Z9 44 U1 1 U2 1 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 FEB PY 1995 VL 96 IS 2 BP 401 EP 428 DI 10.1086/192125 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QD876 UT WOS:A1995QD87600004 ER PT J AU BUTNER, HM MORIARTYSCHIEVEN, GH RESSLER, ME WERNER, MW AF BUTNER, HM MORIARTYSCHIEVEN, GH RESSLER, ME WERNER, MW TI MODELING FAR-INFRARED OBSERVATIONS OF YOUNG STELLAR OBJECTS SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Circumstellar Matter 1994, Celebrating the Centenary of the Royal-Observatory, Edinburgh CY AUG 29-SEP 02, 1994 CL HERIOT WATT UNIV, RICCARTON, SCOTLAND SP PARTICLE PHYS & ASTRON RES COUNCIL, LOTHIAN & EDINBURGH ENTERPRISE LTD, HERZBERG INST ASTROPHYS, KLUWER ACAD PUBLISHERS LTD, CAMBRIDGE UNIV PRESS, JOHN WILEY & SONS LTD, ROYAL ASTRON SOC HO HERIOT WATT UNIV DE STAR FORMATION, THEORY; FAR INFRARED, OBSERVATIONS; RADIATIVE TRANSPORT, MODELS; YOUNG STELLAR OBJECTS, TAURUS AB We discuss high-resolution, far-infrared spatial observations of low mass embedded young stellar objects in the Taurus molecular complex. By comparing the observed spatial extent with the results of radiative transport models, we can estimate the density distribution of the envelopes, We compare the initial results for 4 objects (L1551-IRS 5, L1489-IR, L1551-NE, and L1527-IR) with star formation theories. C1 DOMINION RADIO ASTROPHYS OBSERV,PENTICTON,BC V2A 6K3,CANADA. CALTECH,JET PROP LAB,PASADENA,CA 91109. RP BUTNER, HM (reprint author), CARNEGIE INST WASHINGTON,DEPT TERR MAGNETISM,5241 BROAD BRANCH RD NW,WASHINGTON,DC 20015, USA. OI Butner, Harold/0000-0003-4899-2064 NR 11 TC 1 Z9 1 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 1995 VL 224 IS 1-2 BP 77 EP 80 DI 10.1007/BF00667825 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RB007 UT WOS:A1995RB00700016 ER PT J AU CHANDLER, CJ TEREBEY, S BARSONY, M MOORE, TJT AF CHANDLER, CJ TEREBEY, S BARSONY, M MOORE, TJT TI THE SMALL-SCALE OUTFLOW STRUCTURE OF EMBEDDED SOURCES IN TAURUS SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Circumstellar Matter 1994, Celebrating the Centenary of the Royal-Observatory, Edinburgh CY AUG 29-SEP 02, 1994 CL HERIOT WATT UNIV, RICCARTON, SCOTLAND SP PARTICLE PHYS & ASTRON RES COUNCIL, LOTHIAN & EDINBURGH ENTERPRISE LTD, HERZBERG INST ASTROPHYS, KLUWER ACAD PUBLISHERS LTD, CAMBRIDGE UNIV PRESS, JOHN WILEY & SONS LTD, ROYAL ASTRON SOC HO HERIOT WATT UNIV DE JETS AND OUTFLOWS; REFLECTION NEBULAE; TMC1; TMC1A ID CO LINE FORMATION; BIPOLAR FLOWS AB High resolution interferometric CO J=1-0 observations of the outflows from two young embedded sources, TMC1 and TMC1A, show the high-velocity gas to have a conical structure, with a constant opening angle of similar to 45 degrees extending to within 1000 AU of the central stars. The correspondence of near infrared reflection nebulosity at K band with blueshifted CO emission in both objects suggests the lobes are partially evacuated, as do position-velocity diagrams from single-dish CO J=2-1 data. We suggest that the outflows are driven by jets which impart momentum to the ambient medium through shocks, rather than through the entrainment of molecular material along the edges of the jet. C1 CALTECH,JET PROP LAB,CTR INFRARED PROC & ANAL,PASADENA,CA 91109. UNIV CALIF RIVERSIDE,DEPT PHYS,RIVERSIDE,CA 92521. AFDA,UNIV COLL,DEPT PHYS,CANBERRA,ACT,AUSTRALIA. RP CHANDLER, CJ (reprint author), NATL RADIO ASTRON OBSERV,SOCORRO,NM 87801, USA. NR 8 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 1995 VL 224 IS 1-2 BP 109 EP 112 DI 10.1007/BF00667831 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RB007 UT WOS:A1995RB00700022 ER PT J AU CHARNLEY, SB AF CHARNLEY, SB TI HOT CORE CHEMISTRY SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Circumstellar Matter 1994, Celebrating the Centenary of the Royal-Observatory, Edinburgh CY AUG 29-SEP 02, 1994 CL HERIOT WATT UNIV, RICCARTON, SCOTLAND SP PARTICLE PHYS & ASTRON RES COUNCIL, LOTHIAN & EDINBURGH ENTERPRISE LTD, HERZBERG INST ASTROPHYS, KLUWER ACAD PUBLISHERS LTD, CAMBRIDGE UNIV PRESS, JOHN WILEY & SONS LTD, ROYAL ASTRON SOC HO HERIOT WATT UNIV DE ISM, MOLECULES; STARS, FORMATION ID MOLECULAR LINE SURVEY; ABUNDANCES AB Recent theoretical work on the chemistry in regions of massive star formation is summarised. C1 NASA,AMES RES CTR,DIV SPACE SCI,MOFFETT FIELD,CA 94035. RP CHARNLEY, SB (reprint author), UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720, USA. RI Charnley, Steven/C-9538-2012 NR 21 TC 15 Z9 15 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 1995 VL 224 IS 1-2 BP 251 EP 254 DI 10.1007/BF00667853 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RB007 UT WOS:A1995RB00700043 ER PT J AU JUSTTANONT, K TIELENS, AGGM SKINNER, CJ HAAS, MR AF JUSTTANONT, K TIELENS, AGGM SKINNER, CJ HAAS, MR TI OBSERVATIONS OF HIGH CO ROTATIONAL LINES IN POST-AGBS AND PN SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Circumstellar Matter 1994, Celebrating the Centenary of the Royal-Observatory, Edinburgh CY AUG 29-SEP 02, 1994 CL HERIOT WATT UNIV, RICCARTON, SCOTLAND SP PARTICLE PHYS & ASTRON RES COUNCIL, LOTHIAN & EDINBURGH ENTERPRISE LTD, HERZBERG INST ASTROPHYS, KLUWER ACAD PUBLISHERS LTD, CAMBRIDGE UNIV PRESS, JOHN WILEY & SONS LTD, ROYAL ASTRON SOC HO HERIOT WATT UNIV DE MOLECULAR PROCESSES; SHOCK WAVES; STARS, AGE AND POST-AGE AB We present a preliminary interpretation of high CO rotational line data obtained from KAO. The possibility of either a PDR or a shock model is considered in order to explain the observations. C1 LAWRENCE LIVERMORE NATL LAB,IGPP,LIVERMORE,CA 94551. RP JUSTTANONT, K (reprint author), NASA,AMES RES CTR,MS 245-3,MOFFETT FIELD,CA 94035, USA. OI /0000-0003-1689-9201 NR 8 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 1995 VL 224 IS 1-2 BP 305 EP 308 DI 10.1007/BF00667862 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RB007 UT WOS:A1995RB00700052 ER PT J AU CHARNLEY, SB AF CHARNLEY, SB TI GAS-GRAIN PROCESSES IN THE ENVELOPES OF LATE-TYPE STARS SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Circumstellar Matter 1994, Celebrating the Centenary of the Royal-Observatory, Edinburgh CY AUG 29-SEP 02, 1994 CL HERIOT WATT UNIV, RICCARTON, SCOTLAND SP PARTICLE PHYS & ASTRON RES COUNCIL, LOTHIAN & EDINBURGH ENTERPRISE LTD, HERZBERG INST ASTROPHYS, KLUWER ACAD PUBLISHERS LTD, CAMBRIDGE UNIV PRESS, JOHN WILEY & SONS LTD, ROYAL ASTRON SOC HO HERIOT WATT UNIV DE STARS, LATE-TYPE; STARS, CIRCUMSTELLAR MATTER AB Some results from studies of the gas-grain chemistry in oxygen-rich circumstellar envelopes (CSEs) are presented. C1 NASA,AMES RES CTR,DIV SPACE SCI,MOFFETT FIELD,CA 94035. RP CHARNLEY, SB (reprint author), UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720, USA. RI Charnley, Steven/C-9538-2012 NR 7 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 1995 VL 224 IS 1-2 BP 439 EP 440 DI 10.1007/BF00667894 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RB007 UT WOS:A1995RB00700082 ER PT J AU CHARNLEY, SB AF CHARNLEY, SB TI THE INTERSTELLAR CHEMISTRY OF PROTOSTELLAR DISKS SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Circumstellar Matter 1994, Celebrating the Centenary of the Royal-Observatory, Edinburgh CY AUG 29-SEP 02, 1994 CL HERIOT WATT UNIV, RICCARTON, SCOTLAND SP PARTICLE PHYS & ASTRON RES COUNCIL, LOTHIAN & EDINBURGH ENTERPRISE LTD, HERZBERG INST ASTROPHYS, KLUWER ACAD PUBLISHERS LTD, CAMBRIDGE UNIV PRESS, JOHN WILEY & SONS LTD, ROYAL ASTRON SOC HO HERIOT WATT UNIV DE ISM, MOLECULES; SOLAR SYSTEM, FORMATION AB A study has been undertaken of the gas-grain chemistry of protostellar disks which are sufficiently cool that in the outer regions, where the gas density is less than similar to 10(13)cm(-3) and the ionization rate highest, a bimolecular chemistry resembling that of dark clouds can occur. Since the gas-grain collision rate is so high, outgassing mantle molecules effectively determine the gas phase composition at any position in the disk. Ln contrast to previous work, a detailed gas phase chemistry is considered dong with the accretion and desorption of mantle species which is controlled locally by the dust temperature. C1 NASA,AMES RES CTR,DIV SPACE SCI,MOFFETT FIELD,CA 94035. RP CHARNLEY, SB (reprint author), UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720, USA. RI Charnley, Steven/C-9538-2012 NR 7 TC 2 Z9 2 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 1995 VL 224 IS 1-2 BP 441 EP 442 DI 10.1007/BF00667895 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RB007 UT WOS:A1995RB00700083 ER PT J AU CHARNLEY, SB BUTNER, H AF CHARNLEY, SB BUTNER, H TI MOLECULAR SIGNATURES OF MHD WAVES SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Circumstellar Matter 1994, Celebrating the Centenary of the Royal-Observatory, Edinburgh CY AUG 29-SEP 02, 1994 CL HERIOT WATT UNIV, RICCARTON, SCOTLAND SP PARTICLE PHYS & ASTRON RES COUNCIL, LOTHIAN & EDINBURGH ENTERPRISE LTD, HERZBERG INST ASTROPHYS, KLUWER ACAD PUBLISHERS LTD, CAMBRIDGE UNIV PRESS, JOHN WILEY & SONS LTD, ROYAL ASTRON SOC HO HERIOT WATT UNIV DE ISM, MOLECULES; ISM, KINEMATICS AND DYNAMICS ID CLOUDS AB The small ion-neutral drift speeds attained in MHD waves lead to a significant increase in the rates of several important ion-molecule reactions. The effect on the deuterium chemistry of dark clouds could allow MHD wave motion to be observed directly. The results of some recent observations to test this theory are outlined. C1 NASA, AMES RES CTR, DIV SPACE SCI, MOFFETT FIELD, CA 94035 USA. CARNEGIE INST WASHINGTON, DEPT TERR MAGNETISM, WASHINGTON, DC 20005 USA. RP CHARNLEY, SB (reprint author), UNIV CALIF BERKELEY, DEPT ASTRON, BERKELEY, CA 94720 USA. RI Charnley, Steven/C-9538-2012; OI Butner, Harold/0000-0003-4899-2064 NR 7 TC 6 Z9 6 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 1995 VL 224 IS 1-2 BP 443 EP 444 DI 10.1007/BF00667896 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RB007 UT WOS:A1995RB00700084 ER PT J AU PHILLIPS, TR GREEN, S AF PHILLIPS, TR GREEN, S TI EXCITATION OF INTERSTELLAR WATER BY ORTHO-HYDROGEN AND PARA-HYDROGEN SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Circumstellar Matter 1994, Celebrating the Centenary of the Royal-Observatory, Edinburgh CY AUG 29-SEP 02, 1994 CL HERIOT WATT UNIV, RICCARTON, SCOTLAND SP PARTICLE PHYS & ASTRON RES COUNCIL, LOTHIAN & EDINBURGH ENTERPRISE LTD, HERZBERG INST ASTROPHYS, KLUWER ACAD PUBLISHERS LTD, CAMBRIDGE UNIV PRESS, JOHN WILEY & SONS LTD, ROYAL ASTRON SOC HO HERIOT WATT UNIV ID MASER C1 NASA,GODDARD INST SPACE STUDIES,NEW YORK,NY 10025. RP PHILLIPS, TR (reprint author), HUGHES STX CORP,NEW YORK,NY, USA. NR 8 TC 8 Z9 8 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 1995 VL 224 IS 1-2 BP 537 EP 538 DI 10.1007/BF00667943 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RB007 UT WOS:A1995RB00700126 ER PT J AU SCHLEGEL, EM COLBERT, E PETRE, R AF SCHLEGEL, EM COLBERT, E PETRE, R TI CIRCUMSTELLAR X-RAY-EMISSION FROM SN1978K SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Circumstellar Matter 1994, Celebrating the Centenary of the Royal-Observatory, Edinburgh CY AUG 29-SEP 02, 1994 CL HERIOT WATT UNIV, RICCARTON, SCOTLAND SP PARTICLE PHYS & ASTRON RES COUNCIL, LOTHIAN & EDINBURGH ENTERPRISE LTD, HERZBERG INST ASTROPHYS, KLUWER ACAD PUBLISHERS LTD, CAMBRIDGE UNIV PRESS, JOHN WILEY & SONS LTD, ROYAL ASTRON SOC HO HERIOT WATT UNIV DE X-RAYS; CIRCUMSTELLAR MATTER; SUPERNOVAE AB We present the X-ray light curve in the 0.2-2.4 keV band based on five ROSAT observations of SN1978K in NGC 1313. The X-ray emission is believed to arise from the interaction of the reverse shock and the expanding debris from the supernova. The reverse shock becomes established after the outgoing shock runs into circumstellar matter. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NR 9 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 1995 VL 224 IS 1-2 BP 553 EP 554 DI 10.1007/BF00667951 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RB007 UT WOS:A1995RB00700134 ER PT J AU STEVENS, IR SKINNER, SL NAGASE, F CORCORAN, MF WILLIS, AJ POLLOCK, AMT KOYAMA, K AF STEVENS, IR SKINNER, SL NAGASE, F CORCORAN, MF WILLIS, AJ POLLOCK, AMT KOYAMA, K TI ASCA OBSERVATIONS OF COLLIDING STELLAR WINDS IN GAMMA-VELORUM SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT International Conference on Circumstellar Matter 1994, Celebrating the Centenary of the Royal-Observatory, Edinburgh CY AUG 29-SEP 02, 1994 CL HERIOT WATT UNIV, RICCARTON, SCOTLAND SP PARTICLE PHYS & ASTRON RES COUNCIL, LOTHIAN & EDINBURGH ENTERPRISE LTD, HERZBERG INST ASTROPHYS, KLUWER ACAD PUBLISHERS LTD, CAMBRIDGE UNIV PRESS, JOHN WILEY & SONS LTD, ROYAL ASTRON SOC HO HERIOT WATT UNIV DE STARS, WOLF-RAYET; STARS, X-RAYS; STARS, COLLIDING WINDS AB We present new high spectral resolution X-ray observations of the colliding wind binary gamma Vel taken with the ASCA satellite. We find two spectral components, one of which is post-shock emission from the colliding winds. Spectral variability is also seen, consistent with current notions of colliding wind phenomena. C1 NASA,GSFC,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD. INST SPACE & ASTRON SCI,TOKYO,JAPAN. COMP & SCI CO LTD,SHEFFIELD,S YORKSHIRE,ENGLAND. KYOTO UNIV,DEPT PHYS,KYOTO,JAPAN. RP STEVENS, IR (reprint author), UNIV BIRMINGHAM,SCH PHYS & SPACE RES,BIRMINGHAM B15 2TT,W MIDLANDS,ENGLAND. NR 2 TC 1 Z9 1 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD FEB PY 1995 VL 224 IS 1-2 BP 569 EP 570 DI 10.1007/BF00667959 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RB007 UT WOS:A1995RB00700142 ER PT J AU ACKER, JG BUSALACCHI, A AF ACKER, JG BUSALACCHI, A TI WORKSHOP ON SATELLITE AND IN-SITU OBSERVATIONS FOR CLIMATE PREDICTION SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Editorial Material AB Participants in this workshop, which convened in Venice, Italy, 6-8 May 1993, met to consider the current state of climate monitoring programs and instrumentation for the purpose of climatological prediction on short-term (seasonal to interannual) timescales. Data quality and coverage requirements for definition of oceanographic heat and momentum fluxes, scales of inter- and intra-annual variability, and land-ocean-atmosphere exchange processes were examined. Advantages and disadvantages of earth-based and spaceborne monitoring systems were considered, as were the structures for future monitoring networks, research programs, and modeling studies. C1 HUGHES STX CORP,LANHAM,MD. RP ACKER, JG (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HYDROSPHER PROC LAB,CODE 9702,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 SN 0003-0007 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD FEB PY 1995 VL 76 IS 2 BP 241 EP 249 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QQ923 UT WOS:A1995QQ92300007 ER PT J AU SOMERTON, DA KIKKAWA, BS AF SOMERTON, DA KIKKAWA, BS TI A STOCK SURVEY TECHNIQUE USING THE TIME TO CAPTURE INDIVIDUAL FISH ON LONGLINES SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article AB Longline catches per unit of effort (CPUE) from research surveys are often assumed to vary in proportion to fish abundance. This assumption, however, may be invalid if the abundance of the target species is high enough to saturate the gear or if the abundance of nontarget species is high enough to exclude the target species from capture. We examine a new approach to surveying fish populations with longlines that is based on time-to-capture data measured with small, fish-activated timing devices attached to every hook. A new measure of relative abundance, lambda, is developed that is immune to the effects of gear saturation and interspecific competition for hooks. Two estimators of lambda are compared by using capture-time data collected during summer 1987-1991 for pelagic armorhead (Pseudopentaceros wheeleri). Both estimators are shown to be unbiased if the underlying assumptions are true and fairly robust to the observed departures from these assumptions. C1 NOAA,NATL MARINE FISHERIES SERV,SW FISHERIES SCI CTR,HONOLULU LAB,HONOLULU,HI 96822. NR 12 TC 12 Z9 15 U1 1 U2 1 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA ON K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD FEB PY 1995 VL 52 IS 2 BP 260 EP 267 DI 10.1139/f95-026 PG 8 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA RM825 UT WOS:A1995RM82500004 ER PT J AU SWARTZMAN, G SILVERMAN, E WILLIAMSON, N AF SWARTZMAN, G SILVERMAN, E WILLIAMSON, N TI RELATING TRENDS IN WALLEYE POLLOCK (THERAGRA-CHALCOGRAMMA) ABUNDANCE IN THE BERING SEA TO ENVIRONMENTAL-FACTORS SO CANADIAN JOURNAL OF FISHERIES AND AQUATIC SCIENCES LA English DT Article ID TUNA CATCH; GULF; DISTRIBUTIONS; FEATURES; MEXICO; SHELF AB Generalized additive models (GAM), a nonparametric regression method with less restrictive statistical assumptions than traditional regression methods, were used to model the trend in mean abundance of Bering Sea walleye pollock (Theragra chalcogramma) as a function of ocean environmental conditions including water column depth, temperature at 50 m, and depth of the thermocline. Acoustic survey data collected in the summers of 1988 and 1991 were used to test these relationships. In both surveys, mean walleye pollock abundance was highest in areas having a 70-130 m depth range and where the 50-m temperature was close to 2.5 degrees C. Thermocline depth, while not itself significant, had a significant effect on walleye pollock abundance through interactions with both bottom depth and temperature at 50 m. Walleye pollock in the top 50 m of the water column (mostly juveniles) were influenced differently by temperature and thermocline depth than the adult walleye pollock, which were generally deeper in the water column. The depth, temperature, and thermocline preferences of walleye pollock are hypothesized to be linked to food availability which is, in turn, related to temperature regimes or fronts along the Bering Sea shelf slope. C1 UNIV WASHINGTON,CTR QUANTITAT SCI HR20,SEATTLE,WA 98105. NATL MARINE FISHERIES SERV,ALASKA FISHERIES SCI CTR,JUNEAU,AK. RP SWARTZMAN, G (reprint author), UNIV WASHINGTON,APPL PHYS LAB HN10,SEATTLE,WA 98105, USA. NR 34 TC 47 Z9 52 U1 2 U2 3 PU NATL RESEARCH COUNCIL CANADA PI OTTAWA PA RESEARCH JOURNALS, MONTREAL RD, OTTAWA ON K1A 0R6, CANADA SN 0706-652X J9 CAN J FISH AQUAT SCI JI Can. J. Fish. Aquat. Sci. PD FEB PY 1995 VL 52 IS 2 BP 369 EP 380 DI 10.1139/f95-039 PG 12 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA RM825 UT WOS:A1995RM82500017 ER PT J AU FARHAT, C LANTERI, S SIMON, HD AF FARHAT, C LANTERI, S SIMON, HD TI TOP/DOMDEC - A SOFTWARE TOOL FOR MESH PARTITIONING AND PARALLEL-PROCESSING SO COMPUTING SYSTEMS IN ENGINEERING LA English DT Article AB TOP/DOMDEC is an interactive software package for mesh partitioning and parallel processing. It offers several state-of-the-art graph decomposition algorithms in a user friendly environment. Generated mesh partitions can be smoothed and optimized for minimum interface and maximum load balance using one of several non-deterministic optimization algorithms. TOP/DOMDEC also provides real-time means for assessing a prior the quality of a mesh partition and discriminating between different partitioning algorithms. The user interface includes high speed three-dimensional graphics, an interprocessor communication simulator for today's massively parallel systems, and an output function with parallel I/O data structures. In this paper, we describe the basic features of TOP/DOMDEC and highlight their application to the parallel solution of computational fluid and solid mechanics problems. C1 UNIV COLORADO,CTR SPACE STRUCT & CONTROLS,BOULDER,CO 80309. NASA,AMES RES CTR,COMP SCI CORP,APPL RES BRANCH,MOFFETT FIELD,CA 94035. RP FARHAT, C (reprint author), UNIV COLORADO,DEPT AEROSP ENGN SCI,BOULDER,CO 80309, USA. NR 15 TC 41 Z9 41 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0956-0521 J9 COMPUT SYST ENG JI Comput. Syst. Eng. PD FEB PY 1995 VL 6 IS 1 BP 13 EP 26 DI 10.1016/0956-0521(94)00024-G PG 14 WC Computer Science, Interdisciplinary Applications; Engineering, Multidisciplinary SC Computer Science; Engineering GA RN804 UT WOS:A1995RN80400002 ER PT J AU GORNITZ, V AF GORNITZ, V TI SEA-LEVEL RISE - A REVIEW OF RECENT PAST AND NEAR-FUTURE TRENDS SO EARTH SURFACE PROCESSES AND LANDFORMS LA English DT Article DE SEA-LEVEL RISE; CLIMATE CHANGE; TIDE-GAUGE RECORDS; ICE SHEETS ID ANTARCTIC ICE-SHEET; SATELLITE ALTIMETRY; THERMAL-EXPANSION; LATE HOLOCENE; GLACIERS; CLIMATE; EARTHQUAKES; SUBSIDENCE; AMERICA; RECORDS AB Global mean sea level is a potentially sensitive indicator of climate change. Global warming will contribute to worldwide sea-level rise (SLR) from thermal expansion of ocean water, melting of mountain glaciers and polar ice sheets. A number of studies, mostly using tide-gauge data from the Permanent Service for Mean Sea Level, Bidston Observatory, England, have obtained rates of global SLR within the last 100 years that range between 0.3 and 3 mm yr(-1), with most values concentrated between 1 and 2 mm yr(-1). However, the reliability of these results has been questioned because of problems with data quality and physical processes that introduce a high level of spatial and temporal variability. Sources of uncertainty in the sealevel data include variations in winds, ocean currents, river runoff, vertical earth movements, and geographically uneven distribution of long-term records. Crustal motions introduce a major source of error. To a large extent, these can be filtered by employing palaeo-sea-level proxies, and geophysical modelling to remove glacio-isostatic changes. Ultimately, satellite geodesy will help resolve the inherent ambiguity between the land and ocean level changes recorded by tide gauges. Future sea level is expected to rise by similar to 1 m, with a 'best-guess' value of 48 cm by the year 2100. Such rates represent an acceleration of four to seven times over present rates. Local land subsidence could substantially increase the apparent SLR. For example, Louisiana is currently experiencing SLR trends nearly 10 times the global mean rate. These recently reduced SLR estimates are based on climate models that predict a zero to negative contribution to SLR from Antarctica. Most global climate models (GCMs) indicate an ice accumulation over Antarctica, because in a warmer world, precipitation will exceed ablation/snow-melt. However, the impacts of attritional processes, such as thinning of the ice shelves, have been downplayed according to some experts. Furthermore, not all climate models are in agreement. Opposite conclusions may be drawn from the results of other GCMs. In addition, the West Antarctic Ice Sheet is potentially subject to dynamic and volcanic instabilities that are difficult to predict. Because of the great uncertainty in SLR projections, careful monitoring of future sea-level trends by upgraded tide-gauge networks and satellite geodesy will become essential. Finally, because of the high spatial variability in crustal subsidence rates, wave climates and tidal regimes, it will be the set of local conditions (especially the relative sea-level rise), rather than a single global mean sea-level trend, that will determine each locality's vulnerability to future SLR. C1 NASA,GODDARD SPACE FLIGHT CTR,INST SPACE STUDIES,NEW YORK,NY 10025. RP GORNITZ, V (reprint author), COLUMBIA UNIV,NEW YORK,NY 10025, USA. NR 90 TC 104 Z9 106 U1 6 U2 48 PU JOHN WILEY & SONS LTD PI W SUSSEX PA BAFFINS LANE CHICHESTER, W SUSSEX, ENGLAND PO19 1UD SN 0197-9337 J9 EARTH SURF PROCESSES JI Earth Surf. Process. Landf. PD FEB PY 1995 VL 20 IS 1 BP 7 EP 20 DI 10.1002/esp.3290200103 PG 14 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA QD272 UT WOS:A1995QD27200002 ER PT J AU NORMAN, MD KEIL, K GRIFFIN, WL RYAN, CG AF NORMAN, MD KEIL, K GRIFFIN, WL RYAN, CG TI FRAGMENTS OF ANCIENT LUNAR CRUST - PETROLOGY AND GEOCHEMISTRY OF FERROAN NORITIC ANORTHOSITES FROM THE DESCARTES REGION OF THE MOON SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID ENSTATITE CHONDRITES; KOMATIITE COMPONENT; PROTON MICROPROBE; POLYMICT SAMPLES; BULK COMPOSITION; ROCKS; SYSTEMATICS; ELEMENTS; VOLATILE; ORIGIN AB Clasts of ferroan noritic anorthosite from Apollo 16 breccia 67016 have mineralogical and geochemical affinities with pristine ferroan anorthosites and therefore may represent primary igneous rocks from the lunar crust. The textures of these clasts document a complex history involving magmatic crystallization, brecciation, subsolidus recrystallization, and sulfide metasomatism. Nonetheless, the major, minor, and trace element compositions of their minerals, as determined by electron and proton microprobe, show that the clasts are essentially monomict and belong to the ferroan anorthositic suite of lunar highlands rocks. The low bulk Ni contents, low Ni/Co ratios, and ancient Sm-Nd isotopic age (greater than or equal to 4.5 Ga; Alibert et al., 1994) of the clasts are consistent with this interpretation. Strontium and gallium contents of plagioclase in the clasts show that their parental magma was depleted in Ga relative to Sr by a factor of about 30 relative to carbonaceous chondrites. This depletion of Ga, which is both moderately volatile and moderately siderophile, probably reflects volatile loss from the Moon rather than extraction of metal. The parental magma from which these clasts originally crystallized was enriched in Sr by about 4-6X relative to proposed bulk Moon compositions, which implies either that ferroan anorthosites crystallized late in the evolution of a lunar magma ocean, or that their parental magma was a basaltic partial melt. Bulk major and trace element compositions of these clasts are remarkably similar to that of the average upper crust of the Moon, which suggests that igneous ferroan noritic anorthosite such as that found in the North Ray Crater breccias and soils may be a significant primary component of the lunar crust. The ferroan noritic anorthosite clasts in 67016 are unusual among lunar samples for their abundance of troilite, and for the evidence of metasomatic introduction of volatile chalcophile elements such as Cu, Zn, Ni, Sb, and Se. Anhydrous C-O-S-Cl vapors are the most likely transport agent for these metals, which would be more consistent with an indigenous lunar origin for the volatiles rather than a cometary or meteoritic source. C1 UNIV HAWAII MANOA,SCH OCEAN & EARTH SCI & TECHNOL,HAWAII INST GEOPHYS & PLANETOL,HONOLULU,HI 96822. CSIRO,DIV EXPLORAT GEOSCI,N RYDE,NSW 2113,AUSTRALIA. UNIV HAWAII MANOA,SCH OCEAN & EARTH SCI & TECHNOL,HAWAII CTR VOLCANOL,HONOLULU,HI 96822. RP NORMAN, MD (reprint author), NASA,LYNDON B JOHNSON SPACE CTR,MAIL CODE SN2,HOUSTON,TX 77058, USA. RI Ryan, Chris/A-6032-2011; GAU, geochemist/H-1985-2016; Griffin, William/F-7713-2011; OI Ryan, Chris/0000-0003-2891-3912; Griffin, William L/0000-0002-0980-2566 NR 90 TC 18 Z9 18 U1 0 U2 3 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 FEB PY 1995 VL 59 IS 4 BP 831 EP 847 DI 10.1016/0016-7037(94)00363-Q PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA QH991 UT WOS:A1995QH99100016 ER PT J AU ULERY, AL GRAHAM, RC CHADWICK, OA WOOD, HB AF ULERY, AL GRAHAM, RC CHADWICK, OA WOOD, HB TI DECADE-SCALE CHANGES OF SOIL CARBON, NITROGEN AND EXCHANGEABLE CATIONS UNDER CHAPARRAL AND PINE SO GEODERMA LA English DT Article ID SAN-GABRIEL MOUNTAINS; SOUTHERN-CALIFORNIA; FIRE; PEDOGENESIS; DEPOSITION; NUTRIENTS; ECOSYSTEM AB Four large lysimeters on the San Dimas Experimental Forest, each filled with similar parent material and planted with monocultures of native species in 1946, provide a unique opportunity to quantify short-term effects of plant species on soil properties. The four species under which soils were investigated are scrub oak (Quercus dumosa Nutt.), chamise (Adenostoma fasciculatum Hook. and Am.), ceanothus (Ceanothus crassifolia Ton.), and Coulter pine (Pinus coulteri B. Don). A mass-balance approach was used to measure changes in C, N, exchangeable base cations, and exchangeable acidity to a depth of 1 m in the mineral soils over a 41-year period, The C content increased in all of the soils, but the greatest change was in the soil under oak (3.7 kg m(-3)), more than doubling the original amount. Since the source of C in these soils is the photosynthetic fixation of atmospheric CO2, the mass of C accumulated reflects the magnitude of the CO2 sink provided by chaparral soils in their initial stages of formation. The calculated rate of soil C accumulation is as much as 0.09 kg m(-3) yr(-1). The increase in N was highest in the soil under ceanothus (0.12 kg m(-3)), the only N-2-fixing species in this study. Exchangeable Ca increased by 25.7 mol m(-3) in the soil under oak, while the maximum increase in exchangeable Mg was 5.5 mol m(-3) also under oak. Exchangeable Na was leached from all of the soils (a maximum of 2.4 mol m(-3) lost from under chamise and ceanothus) and K was slightly depleted. C1 UNIV CALIF RIVERSIDE,DEPT SOIL & ENVIRONM SCI,RIVERSIDE,CA 92521. CALTECH,JET PROP LAB,PASADENA,CA 91109. US FOREST SERV,PACIFIC SW RES STN,RIVERSIDE,CA 92507. RP ULERY, AL (reprint author), USDA ARS,US SALIN LAB,4500 GLENWOOD DR,RIVERSIDE,CA 92501, USA. NR 36 TC 51 Z9 54 U1 1 U2 15 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0016-7061 J9 GEODERMA JI Geoderma PD FEB PY 1995 VL 65 IS 1-2 BP 121 EP 134 DI 10.1016/0016-7061(94)00034-8 PG 14 WC Soil Science SC Agriculture GA QL227 UT WOS:A1995QL22700007 ER PT J AU WEBB, FH BURSIK, M DIXON, T FARINA, F MARSHALL, G STEIN, RS AF WEBB, FH BURSIK, M DIXON, T FARINA, F MARSHALL, G STEIN, RS TI INFLATION OF LONG VALLEY CALDERA FROM 1 YEAR OF CONTINUOUS GPS OBSERVATIONS SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID EASTERN CALIFORNIA; CAMPI FLEGREI AB A permanent Global Positioning System receiver at Casa Diablo Hot Springs, Long Valley Caldera, California was installed in January, 1993, and has operated almost continuously since then. The data have been transmitted daily to the Jet Propulsion Laboratory for routine analysis with data from the Fiducial Laboratories for an international Natural sciences Network (FLINN) by the JPL FLINN analysis center. Results from these analyses have been used to interpret the on going deformation at Long Valley, with data excluded from periods when the antenna was covered under 2.5 meters of snow and from some periods when Anti Spoofing was enforced on the GPS signal. The remaining time series suggests that uplift of the resurgent dome of Long Valley Caldera during 1993 has been 2.5 +/- 1.1 cm/yr and horizontal motion has been 3.0 +/- 0.7 cm/yr at S53W in a no-net-rotation global reference frame, or 1.5 +/- 0.7 cm/yr at S14W relative to the Sierra Nevada block. These rates are consistent with uplift predicted from frequent horizontal strain measurements. Spectral analysis of the observations suggests that tidal forcing of the magma chamber is not a source of the variability in the 3 dimensional station location. These results suggest that remotely operated, continuously recording GPS receivers could prove to be a reliable tool for volcano monitoring throughout the world. C1 SUNY BUFFALO,DEPT GEOL,BUFFALO,NY 14260. UNIV MIAMI,ROSENSTIEL SCH MARINE & ATMOSPHER SCI,DIV MARINE GEOL & GEOPHYS,VIRGINIA KEY,FL 33149. US GEOL SURVEY,MENLO PK,CA 94025. RP WEBB, FH (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,MS 238-600,PASADENA,CA 91109, USA. NR 17 TC 19 Z9 19 U1 0 U2 2 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 FEB 1 PY 1995 VL 22 IS 3 BP 195 EP 198 DI 10.1029/94GL02968 PG 4 WC Geosciences, Multidisciplinary SC Geology GA QJ211 UT WOS:A1995QJ21100004 ER PT J AU TORRES, O BHARTIA, PK AF TORRES, O BHARTIA, PK TI EFFECT OF STRATOSPHERIC AEROSOL ON OZONE PROFILE FROM BUV MEASUREMENTS SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB Results of a simulation study on the effects of optically thick stratospheric sulfate aerosol layers on the backscattered ultraviolet radiation (buv) in the range 256-340 nm are presented. In general, the increased Mie scattering produced by the aerosols results in an enhancement of the buv radiation. The increase is approximately linear with optical depth and strongly depends on solar zenith angle and aerosol layer altitude in relation to the ozone maximum. The effect is greatest at those wavelengths whose contribution functions peak in the vicinity of the densest part of the aerosol layer. The aerosol induced perturbation of the buv field affects the ozone profile retrieval from space measurements by the SBUV experiment. In the tropical stratosphere, the retrieved ozone between 25 and 45 km is underestimated as a result of increased Mie scattering. On the other hand, an algorithm related effect causes the retrieved ozone below 25 lan to be overestimated by an amount similar to the stratospheric deficit. C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. RP TORRES, O (reprint author), HUGHES STX CORP,7701 GREENBELT RD,GREENBELT,MD 20770, USA. RI Torres, Omar/G-4929-2013; Bhartia, Pawan/A-4209-2016 OI Bhartia, Pawan/0000-0001-8307-9137 NR 8 TC 13 Z9 13 U1 0 U2 1 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 FEB 1 PY 1995 VL 22 IS 3 BP 235 EP 238 DI 10.1029/94GL02994 PG 4 WC Geosciences, Multidisciplinary SC Geology GA QJ211 UT WOS:A1995QJ21100014 ER PT J AU WANG, PH MCCORMICK, MP MINNIS, P KENT, GS YUE, GK SKEENS, KM AF WANG, PH MCCORMICK, MP MINNIS, P KENT, GS YUE, GK SKEENS, KM TI A METHOD FOR ESTIMATING VERTICAL-DISTRIBUTION OF THE SAGE-II OPAQUE CLOUD FREQUENCY SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article AB A method is developed to infer the vertical distribution of the occurrence frequency of clouds that are opaque to the Stratospheric Aerosol and Gas Experiment (SAGE) II instrument. An application of the method to the 1986 SAGE II observations is included in this paper. The 1986 SAGE II results are compared with the 1952-1981 cloud climatology of Warren et al. [1986, 1988]. C1 NASA,LANGLEY RES CTR,DIV ATMOSPHER SCI,HAMPTON,VA 23681. RP WANG, PH (reprint author), SCI & TECHNOL CORP,101 RES DR,HAMPTON,VA 23666, USA. RI Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 NR 17 TC 23 Z9 23 U1 0 U2 1 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 FEB 1 PY 1995 VL 22 IS 3 BP 243 EP 246 DI 10.1029/94GL02992 PG 4 WC Geosciences, Multidisciplinary SC Geology GA QJ211 UT WOS:A1995QJ21100016 ER PT J AU GOEMBEL, L HERRERO, FA AF GOEMBEL, L HERRERO, FA TI ANOMALOUS MERIDIONAL THERMOSPHERIC NEUTRAL WINDS IN THE AE-E NATE DATA - EFFECTS OF THE EQUATORIAL NIGHTTIME PRESSURE BULGE SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID TEMPERATURE AB The work described here makes it possible to identify anomalous wind behavior such as the nighttime meridional wind abatements that occur at F-region heights. A new analysis technique uses a simple empirical wind model to simulate measurements of ''normal'' winds (as measured by the Neutral Atmosphere and Temperature Experiment (NATE) that flew on the Atmosphere Explorer-E (AE-E)) to highlight anomalous wind measurements made by the satellite while in circular orbits at 270-290 km altitude. Our approach is based on the recognition that the ''in orbit'' wind variation must show the combined effects of the diurnal wind variation as seen from the ground with the latitude variation of the satellite orbit. For the data period 77250-78035 examined thus far, the wind abatement always occurred with a corresponding pressure or temperature maximum, and was detected on 12 out of the 36 nights with data. This study has revealed that the wind abatements occur only during or shortly after increases in solar EUV flux, as indicated by daily radio flux measurements. In the past, nighttime wind reversals at mid-latitudes have been associated with increased geomagnetic activity. This study indicates that intensified solar EUV heating may be responsible for anomalous thermospheric nighttime winds at mid-latitudes. C1 NASA,GODDARD SPACE FLIGHT CTR,EXTRATERR PHYS LAB,GREENBELT,MD 20771. RP GOEMBEL, L (reprint author), JOHNS HOPKINS UNIV,APPL PHYS LAB,JOHNS HOPKINS RD,LAUREL,MD 20723, USA. NR 12 TC 5 Z9 5 U1 0 U2 0 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 FEB 1 PY 1995 VL 22 IS 3 BP 271 EP 274 DI 10.1029/94GL03021 PG 4 WC Geosciences, Multidisciplinary SC Geology GA QJ211 UT WOS:A1995QJ21100023 ER PT J AU SCHNETZLER, CC KRUEGER, AJ BLUTH, GS SPROD, IE WALTER, LS AF SCHNETZLER, CC KRUEGER, AJ BLUTH, GS SPROD, IE WALTER, LS TI THE ATMOSPHERIC SO2 BUDGET FOR PINATUBO DERIVED FROM NOAA-11 SBUV/2 SPECTRAL DATA - COMMENT SO GEOPHYSICAL RESEARCH LETTERS LA English DT Letter ID ERUPTIONS; CLOUDS C1 MICHIGAN TECHNOL UNIV,DEPT GEOL,HOUGHTON,MI 49931. NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. NASA,GODDARD SPACE FLIGHT CTR,EARTH SCI DIRECTORATE,GREENBELT,MD 20771. HUGHES STX,LANHAM,MD 20706. RP SCHNETZLER, CC (reprint author), UNIV MARYLAND,DEPT GEOG,1113 LEFRAK HALL,COLLEGE PK,MD 20742, USA. NR 6 TC 4 Z9 4 U1 0 U2 0 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 FEB 1 PY 1995 VL 22 IS 3 BP 315 EP 316 DI 10.1029/94GL02406 PG 2 WC Geosciences, Multidisciplinary SC Geology GA QJ211 UT WOS:A1995QJ21100034 ER PT J AU MCPETERS, RD AF MCPETERS, RD TI THE ATMOSPHERIC SO2 BUDGET FOR PINATUBO DERIVED FROM NOAA-11 SBUV/2 SPECTRAL DATA - REPLY SO GEOPHYSICAL RESEARCH LETTERS LA English DT Letter ID ERUPTIONS RP MCPETERS, RD (reprint author), NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,CODE 916,GREENBELT,MD 20771, USA. RI McPeters, Richard/G-4955-2013 OI McPeters, Richard/0000-0002-8926-8462 NR 4 TC 2 Z9 2 U1 0 U2 1 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 FEB 1 PY 1995 VL 22 IS 3 BP 317 EP 319 DI 10.1029/94GL02444 PG 3 WC Geosciences, Multidisciplinary SC Geology GA QJ211 UT WOS:A1995QJ21100035 ER PT J AU TOON, B CUZZI, J SAGAN, C AF TOON, B CUZZI, J SAGAN, C TI POLLACK,JAMES,B. (1938-1994) - IN-MEMORIAM SO ICARUS LA English DT Item About an Individual C1 CORNELL UNIV,ITHACA,NY 14853. RP TOON, B (reprint author), NASA,AMES RES CTR,MOFFETT FIELD,CA 94035, USA. NR 1 TC 2 Z9 2 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 1995 VL 113 IS 2 BP 227 EP 231 DI 10.1006/icar.1995.1021 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QN154 UT WOS:A1995QN15400001 PM 11538591 ER PT J AU MOSES, JI RAGES, K POLLACK, JB AF MOSES, JI RAGES, K POLLACK, JB TI AN ANALYSIS OF NEPTUNE STRATOSPHERIC HAZE USING HIGH-PHASE-ANGLE VOYAGER IMAGES SO ICARUS LA English DT Article ID RADIO OCCULTATION MEASUREMENTS; UPPER-ATMOSPHERE; URANUS; PHOTOCHEMISTRY; HYDROCARBONS; METHANE; TEMPERATURE; SCATTERING; ABUNDANCE; AEROSOLS AB We have inverted high-phase-angle Voyager images of Neptune to determine the atmospheric extinction coefficient as a function of altitude and the scattering phase function at a reference altitude. Comparisons between theoretical models and observations help separate the contributions from molecular Rayleigh and aerosol scattering and help determine the variation of the aerosol size, concentration, and scattering properties with altitude. Further comparisons between models and data allow us to place constraints on the location and composition of the hazes, the concentration and downward Bur of certain condensible hydrocarbon gases, the eddy diffusion coefficient in the lower stratosphere, and the thermal profile in parts of Neptune's stratosphere. We find that a distinct stratospheric haze layer exists near 12(-1)(+1) mbar in Neptune's lower stratosphere, most probably due to condensed ethane, The derived stratospheric haze production rate of 1.0(-0.3)(+0.2) x 10(-15) g cm(-2) sec(-1) is substantially lower than photochemical model predictions. Evidence for hazes at higher altitudes also exists. Unlike the situation on Uranus, large particles (0.08-0.11 mu m) may be present at high altitudes on Neptune (e.g., near 0.5 mbar), well above the region in which we expect the major hydrocarbon species to condense. Near 28 mbar, the mean particle size is about 0.13(-0.02)(+0.02) mu m with a concentration of 5(-3)(+3) particles cm(-3). The cumulative haze extinction optical depth above 15 mbar in the clear filter is similar to 3 x 10(-3), and much of this extinction is due to scattering rather than absorption; thus, if our limb-scan sites are typical, the hazes cannot account for the stratospheric temperature inversion on Neptune and may not contribute significantly to atmospheric heating. We compare the imaging results with the results from other,observations, including those of the Voyager Photopolarimeter Subsystem, and discuss differences between Neptune and Uranus. (C) 1995 Academic Press, Inc. C1 SPACE PHYS RES INST,SUNNYVALE,CA 94087. NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. RP MOSES, JI (reprint author), LUNAR & PLANETARY INST,3600 BAY AREA BLVD,HOUSTON,TX 77058, USA. RI Moses, Julianne/I-2151-2013 OI Moses, Julianne/0000-0002-8837-0035 NR 60 TC 24 Z9 24 U1 1 U2 4 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 1995 VL 113 IS 2 BP 232 EP 266 DI 10.1006/icar.1995.1022 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QN154 UT WOS:A1995QN15400002 ER PT J AU BEZARD, B COUSTENIS, A MCKAY, CP AF BEZARD, B COUSTENIS, A MCKAY, CP TI TITANS STRATOSPHERIC TEMPERATURE ASYMMETRY - A RADIATIVE ORIGIN SO ICARUS LA English DT Article ID VOYAGER INFRARED OBSERVATIONS; RADIO-OCCULTATION; ATMOSPHERE; MODEL; PHOTOCHEMISTRY; AEROSOLS; ALBEDO AB During the 1981 Voyager encounter, Titan's stratosphere exhibited a large thermal asymmetry, with high northern latitudes being colder than comparable southern latitudes. Given the short radiative time constant, this asymmetry would not be expected at the season of the Voyager observations (spring equinox), if the infrared and solar opacity sources were distributed symmetrically. We have investigated the radiative budget of Titan's stratosphere, using two selections of Voyager IRIS spectra recorded at symmetric northern and southern latitudes. In the region 0.1-1 mbar, temperatures are 7 K colder at 50 degrees N than at 53 degrees S and the difference reaches similar to 13 K at 5 mbar. On the other hand, the northern region is strongly enriched in nitriles and hydrocarbons, and the haze optical depth derived from the continuum emission between 8 and 15 mu m is twice as Large as in the south. Cooling rate profiles have been computed at the two locations, using the gas and haze abundances derived from the IRIS measurements. We find that, despite lower temperatures, the cooling rate profiles in the pressure range 0.15-5 mbar are 20 to 40% larger in the north than in the south, because of the enhanced concentrations of infrared radiators. Because the northern hemisphere appears darker than the southern one in the Voyager images, enhanced solar heating is also expected to take place at SOON. Solar heating rate profiles have been calculated, with two different assumptions on the origin of the hemispheric asymmetry. In the most likely case where it results from a variation in the absorbance of the haze material, the heating rates are found to be 12-15% larger at the northern location than at the southern one, a smaller increase than that in the cooling rates. If the lower albedo in the north results from an increase in the particle number density, a 55 to 75% difference is found for the pressure range 0.15-5 mbar, thus larger than that calculated for the cooling rates. Considering the uncertainties in the haze model, dynamical heat transport may significantly contribute to the meridional temperature gradients observed in the stratosphere. On the other hand, the latitudinal variation in gas and haze composition may be sufficient to explain the entire temperature asymmetry observed, without invoking a lag in the thermal response of the atmosphere due to dynamical inertia. (C) 1995 Academic Press, Inc. C1 NASA,AMES RES CTR,DIV SPACE SCI,MOFFETT FIELD,CA 94035. RP BEZARD, B (reprint author), OBSERV PARIS,DEPT RECH SPATIALE,SECT MEUDON,F-92195 MEUDON,FRANCE. NR 24 TC 42 Z9 42 U1 0 U2 5 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 1995 VL 113 IS 2 BP 267 EP 276 DI 10.1006/icar.1995.1023 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QN154 UT WOS:A1995QN15400003 PM 11538592 ER PT J AU MAGALHAES, JA YOUNG, RE AF MAGALHAES, JA YOUNG, RE TI DOWNSLOPE WINDSTORMS IN THE LEE OF RIDGES ON MARS SO ICARUS LA English DT Article ID GENERAL-CIRCULATION MODEL; GLOBAL DUST STORMS; MOUNTAIN WAVES; ATMOSPHERIC DYNAMICS; WIND STREAKS; FLOW; SIMULATIONS; OBSTACLE; SIZE AB The semianalytical theory of downslope windstorms, originally developed to understand large increases in surface winds in the lee of major mountain chains on Earth, such as the famous windstorms in Boulder, Colorado, is applied to martian conditions. The focus of this work is to assess whether this theory can help us understand dark erosional wind streaks downstream of ridges on the martian surface, These streaks provide a well-documented example of dust raising on Mars, However, the formation of the streaks remains a mystery because atmospheric circulation models indicate surface friction velocities far lower than those required for the initiation of eolian activity. Downslope windstorms result from the interaction of topographically launched finite amplitude gravity waves with a level of zero wind, which vertically traps the waves, When this zero-wind level is at the proper height, large increases in downstream surface winds (up to a factor of 4) can be produced, During the martian night, downslope windstorms can occur in the lee of quite small ridges (heights greater than or equal to tens of meters) when a level of zero-wind is present in the lowest few kilometers of the atmosphere, Three independent models of the martian atmospheric circulation indeed show levels of zero wind in the form of wind reversals at the appropriate height and season and at the locations where the ridge-related dark streaks are concentrated. The strong upstream/downstream difference in surface winds produced by the downslope windstorm mechanism when a suitable wind reversal is present, rather than a particularly strong upstream wind, is what controls the occurrence of the ridge-related dark streaks, Downslope windstorms also appear to be potentially useful in understanding the build-up of dust in the atmosphere preceding the martian global dust storms. (C) 1995 Academic Press, Inc. C1 NASA,AMES RES CTR,DIV SPACE SCI,MOFFETT FIELD,CA 94035. RP MAGALHAES, JA (reprint author), SAN JOSE STATE UNIV FDN,NASA,AMES RES CTR,MAIL STOP 245-3,MOFFETT FIELD,CA 94035, USA. NR 34 TC 12 Z9 13 U1 0 U2 1 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 1995 VL 113 IS 2 BP 277 EP 294 DI 10.1006/icar.1995.1024 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QN154 UT WOS:A1995QN15400004 ER PT J AU LIOU, JC ZOOK, HA AF LIOU, JC ZOOK, HA TI AN ASTEROIDAL DUST RING OF MICRON-SIZED PARTICLES TRAPPED IN THE 1/1 MEAN MOTION RESONANCE WITH JUPITER SO ICARUS LA English DT Article ID POYNTING-ROBERTSON DRAG; SOLAR-SYSTEM AB We have studied the orbital evolution of micrometer-sized asteroidal dust particles under the influence of planetary gravitational perturbations, radiation pressure, Poynting-Robertson (PR) drag, and solar wind drag. It is found that a significant fraction of the 2-mu m diameter particles, with beta = 0.26, are thrown into the 1:1 mean motion resonance zone with Jupiter when they are released from their parent bodies. These particles stay trapped in this resonance for thousands of years and eventually get out of the resonance due to close encounters with Jupiter. Because of ongoing collisions in the asteroid belt, there is a continuous supply of dust particles around this size from the asteroidal belt contributed to the 1:1 resonance region. Therefore, there must exist a dust ring of asteroidal particles around 2 mu m in diameter locked in the 1 : 1 resonance with Jupiter. We also discuss the structure of the ring, the dynamics of how particles are trapped, how they evolve, and how they get out Of the resonance. (C) 1995 Academic Press, Inc. RP LIOU, JC (reprint author), NASA,LYNDON B JOHNSON SPACE CTR,SN3,HOUSTON,TX 77058, USA. NR 31 TC 18 Z9 18 U1 0 U2 0 PU ACADEMIC PRESS INC JNL-COMP SUBSCRIPTIONS PI SAN DIEGO PA 525B STREET, SUITE 1900, SAN DIEGO, CA 92101-4495 SN 0019-1035 J9 ICARUS JI Icarus PD FEB PY 1995 VL 113 IS 2 BP 403 EP 414 DI 10.1006/icar.1995.1030 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QN154 UT WOS:A1995QN15400010 ER PT J AU HINEDI, S SIMON, M RAPHAELI, D AF HINEDI, S SIMON, M RAPHAELI, D TI THE PERFORMANCE OF NONCOHERENT ORTHOGONAL M-FSK IN THE PRESENCE OF TIMING AND FREQUENCY ERRORS SO IEEE TRANSACTIONS ON COMMUNICATIONS LA English DT Article AB Practical M-FSK systems experience a combination of time and frequency offsets (errors). This paper assesses the deleterious effect of these offsets, first individually and then combined, on the average bit error probability performance of the system. Exact expressions for these various error probability performances are derived and evaluated numerically for system parameters of interest. Also presented are upper bounds on average symbol error probability for the case of frequency error alone which are useful in assessing the absolute and relative performance of the system. Both continuous and discontinuous phase M-FSK cases are considered when timing error is present, the latter being much less robust to this type of offset. RP HINEDI, S (reprint author), CALTECH,JET PROP LAB,COMMUN RES SECT,DIGITAL SIGNAL PROC RES GRP,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 10 TC 16 Z9 16 U1 1 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017-2394 SN 0090-6778 J9 IEEE T COMMUN JI IEEE Trans. Commun. PD FEB-APR PY 1995 VL 43 IS 2-4 BP 922 EP 933 DI 10.1109/26.380125 PN 2 PG 12 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA QV155 UT WOS:A1995QV15500041 ER PT J AU NGUYEN, TM HINEDI, SM AF NGUYEN, TM HINEDI, SM TI SELECTION TECHNIQUE FOR SUBCARRIER FREQUENCIES AND MODULATION INDEXES SO IEEE TRANSACTIONS ON COMMUNICATIONS LA English DT Article AB This paper presents a simple technique for the design of a phase-modulated residual carrier communications link to mitigate mutual interferences among the channels for optimum system performance. The emphasis is on two data channels which are operated simultaneously with a ranging signal. The data channels employ PCM/PM and PCM/PSK/PM modulation schemes for high and low data rate channels, respectively. The technique proposed here selects the optimum (1) subcarrier frequency to reduce the interference between the two data channels, and (2) modulation indices to suppress the undesired signals in the data channels. Further, this technique also provides optimum balance of power between the two telemetry data channels and the ranging channel. Although this technique Is proposed to optimize the performance degradation for two data channels, generalizations can be made for more than two data channels. To make the generalizations easier, this paper presents an algorithm based on the proposed technique, along with numerical results demonstrating its applicability. RP NGUYEN, TM (reprint author), CALTECH,JET PROPULS LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 10 TC 1 Z9 1 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 0090-6778 J9 IEEE T COMMUN JI IEEE Trans. Commun. PD FEB-APR PY 1995 VL 43 IS 2-4 BP 1055 EP 1066 DI 10.1109/26.380137 PN 2 PG 12 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA QV155 UT WOS:A1995QV15500053 ER PT J AU SIMON, MK CHENG, UJ AYDIN, L POLYDOROS, A LEVITT, BK AF SIMON, MK CHENG, UJ AYDIN, L POLYDOROS, A LEVITT, BK TI HOP TIMING ESTIMATION FOR NONCOHERENT FREQUENCY-HOPPED M-FSK INTERCEPT RECEIVERS SO IEEE TRANSACTIONS ON COMMUNICATIONS LA English DT Article ID SIGNALS AB The optimum hop timing estimator, based on classical likelihood-ratio (LR) theory, is derived for noncoherent slow and fast frequency-hopped M-FSK intercept receivers. Such receivers have no a priori knowledge of the hopping code and thus the solution to this estimation problem differs considerably from the more commonly considered case of the friendly receiver. The implementation and performance of the LR hop timing structures are presented and compared with that of other previously documented suboptimum schemes. In particular, when compared to the multiple-hop autocorrelation (MHAC) approach and the ''ping-pong'' approach, the average-likelihood ratio (ALR) and maximum-likelihood ratio (MLR) optimum estimators offer an improvement in performance of several dB in input SNR. Robustness issues for the optimal estimator are examined and alternative configurations are proposed that offer enhanced insensitivity to unknown frequency offsets. C1 UNIV SO CALIF,LOS ANGELES,CA 90089. RP SIMON, MK (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 17 TC 13 Z9 13 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 0090-6778 J9 IEEE T COMMUN JI IEEE Trans. Commun. PD FEB-APR PY 1995 VL 43 IS 2-4 BP 1144 EP 1154 DI 10.1109/26.380146 PN 2 PG 11 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA QV155 UT WOS:A1995QV15500062 ER PT J AU MILEANT, A MILLION, S HINEDI, S CHENG, U AF MILEANT, A MILLION, S HINEDI, S CHENG, U TI THE PERFORMANCE OF THE ALL-DIGITAL DATA TRANSITION TRACKING LOOP USING NONLINEAR-ANALYSIS SO IEEE TRANSACTIONS ON COMMUNICATIONS LA English DT Article AB This paper describes the performance of the all-digital data transition tracking loop (DTTL) with coherent and noncoherent sampling using nonlinear theory. The effects of few samples per symbol and of non-commensurate sampling symbol rates are addressed and analyzed for perfectly square pulses as well as Altered pulses. Their impact on the probability density and variance of the phase error are quantified through computer simulations. It is shown that the performance of the all-digital DTTL approaches its analog counterpart when the sampling and symbol rates are noncommensurate (i.e., the number of samples per symbol is irrational). The phase error variance for an even number of samples per symbol is also shown to degrade compared to an odd number of samples per symbol. RP MILEANT, A (reprint author), CALTECH,JET PROP LAB,COMMUN RES SECT,DIGITAL SIGNAL PROC RES GRP,PASADENA,CA 91109, USA. NR 11 TC 7 Z9 7 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 0090-6778 J9 IEEE T COMMUN JI IEEE Trans. Commun. PD FEB-APR PY 1995 VL 43 IS 2-4 BP 1202 EP 1215 DI 10.1109/26.380153 PN 2 PG 14 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA QV155 UT WOS:A1995QV15500069 ER PT J AU CHENG, UJ SIMON, MK POLYDOROS, A LEVITT, BK AF CHENG, UJ SIMON, MK POLYDOROS, A LEVITT, BK TI STATISTICAL-MODELS FOR EVALUATING THE PERFORMANCE OF NONCOHERENT SLOW FREQUENCY-HOPPED M-FSK INTERCEPT RECEIVERS SO IEEE TRANSACTIONS ON COMMUNICATIONS LA English DT Article AB Exact and approximate statistical models (analytical and simulation), based on average- and maximun-likelihood ratio tests, are studied and compared for the purpose of establishing an accurate assessment of the performance of noncoherent SFH M-FSK intercept recievers, Both continuous and discontinuous phase M-FSK cases are considered with important dofferences between the two. C1 UNIV SO CALIF,LOS ANGELES,CA. RP CHENG, UJ (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 7 TC 3 Z9 3 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 0090-6778 J9 IEEE T COMMUN JI IEEE Trans. Commun. PD FEB-APR PY 1995 VL 43 IS 2-4 BP 1703 EP 1712 DI 10.1109/26.380221 PN 3 PG 10 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA QV157 UT WOS:A1995QV15700067 ER PT J AU IYER, RK TRIVEDI, KS GOLDBERG, J AF IYER, RK TRIVEDI, KS GOLDBERG, J TI INTRODUCTION TO THE SPECIAL ISSUE ON FAULT-TOLERANT COMPUTING SO IEEE TRANSACTIONS ON COMPUTERS LA English DT Editorial Material C1 NASA,CTR EXCELLENCE AEROSP COMP,BATAVIA,IL. RP IYER, RK (reprint author), UNIV ILLINOIS,COORDINATED SCI LAB,1101 W SPRINGFIELD AVE,URBANA,IL 61801, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 SN 0018-9340 J9 IEEE T COMPUT JI IEEE Trans. Comput. PD FEB PY 1995 VL 44 IS 2 BP 165 EP 167 PG 3 WC Computer Science, Hardware & Architecture; Engineering, Electrical & Electronic SC Computer Science; Engineering GA QH584 UT WOS:A1995QH58400001 ER PT J AU NGUYEN, TM MARTIN, WL YEH, HG AF NGUYEN, TM MARTIN, WL YEH, HG TI REQUIRED BANDWIDTH, UNWANTED EMISSION, AND DATA POWER EFFICIENCY FOR RESIDUAL AND SUPPRESSED CARRIER SYSTEMS - A COMPARATIVE-STUDY SO IEEE TRANSACTIONS ON ELECTROMAGNETIC COMPATIBILITY LA English DT Article AB This paper presents a new concept for required bandwidth along with a method for computing this bandwidth and the associated undesired emission for the classes of PCM/PSK/PM, PCM/PM and BPSK signals, The PCM/PSK/PM signals considered here employ either a square wave or sinewave subcarrier with NRZ data format, On the other hand, the PCM/PM and BPSK signals use either a Bi-phase or an NRZ data format, Furthermore, the maximum allowable required bandwidth in the presence of noise and the data power efficiency for these modulation schemes will also be investigated, The term ''data power efficiency'' as considered in this paper consists of two principal components, namely, the amount of power contained in the data channel, and the Symbol Signal-to-Noise Ratio (SSNR) degradation due to the presence of InterSymbol Interference (ISI) for a specified required bandwidth, This paper evaluates both of these components numerically for the modulation schemes considered and the results are then compared, Furthermore, the impact of baseband filtering on the required bandwidth is also investigated in this paper. C1 CALTECH,JET PROP LAB,NASA,PASADENA,CA 91109. NR 14 TC 0 Z9 0 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 0018-9375 J9 IEEE T ELECTROMAGN C JI IEEE Trans. Electromagn. Compat. PD FEB PY 1995 VL 37 IS 1 BP 34 EP 50 DI 10.1109/15.350238 PG 17 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA QH102 UT WOS:A1995QH10200004 ER PT J AU HOMEMDEMELLO, LS AF HOMEMDEMELLO, LS TI SEQUENCE PLANNING FOR ROBOTIC ASSEMBLY OF TETRAHEDRAL TRUSS STRUCTURES SO IEEE TRANSACTIONS ON SYSTEMS MAN AND CYBERNETICS LA English DT Article AB An artificial intelligence approach to planning the robotic assembly of large tetrahedral truss structures is presented. Based on the computational formalism known as production system, the approach exploits the simplicity and uniformity of the shapes of the parts and the regularity of their interconnection to drastically reduce the required geometric reasoning computation. The global database consists of a hexagonal grid representation of the truss structure. This representation captures the multiple hierarchies in tetrahedral truss structures and allows a substantial reduction of the search space without sacrificing completeness. It allows the choice of a hierarchy to be made only when needed, thus allowing a more informed decision. Testing the preconditions of the production rules is computationally inexpensive because the patterned way in which the struts are interconnected is incorporated into the topology of the hexagonal grid representation. A directed graph representation of assembly sequences allows the use of both graph search and backtracking control strategies. The extension of the approach to planning repair sequences is outlined. A prototype planner, named TASP, has been implemented and successfully generated assembly sequences for a structure made of 102 struts. RP HOMEMDEMELLO, LS (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 22 TC 4 Z9 5 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 0018-9472 J9 IEEE T SYST MAN CYB JI IEEE Trans. Syst. Man Cybern. PD FEB PY 1995 VL 25 IS 2 BP 304 EP 312 DI 10.1109/21.364834 PG 9 WC Computer Science, Cybernetics; Engineering, Electrical & Electronic SC Computer Science; Engineering GA QC407 UT WOS:A1995QC40700008 ER PT J AU ZAK, H DAS, H AF ZAK, H DAS, H TI TOWARDS A TRAINING METHODOLOGY FOR SKILLED TELEOPERATION SO IEEE TRANSACTIONS ON SYSTEMS MAN AND CYBERNETICS LA English DT Article ID PERFORMANCE; AUTOMATICITY; FEEDBACK AB A novel approach to the design of training methodologies or programs for operators in man-machine systems and its application to the training of skilled human teleoperators is described. This approach requires that training goals are separated into four distinct categories: the maximization of performance consistency or reliability for critical tasks, the maximization of positive transfer between learned and new tasks, the minimization of the effects of internal operator states (e.g. fatigue, stress, workload), and the minimization of the effects of situational uncertainty or anomaly on performance. Being different from one another in fundamental ways these categories or goals entail the development and application of different training techniques. The paper reports the development of training procedures for achieving the first goal, that of performance consistency, for skilled teleoperators. This part methodology was evaluated against the training practices commonly used in the field, and was found to enhance the learning, hence promote the acquisition of performance consistency, of a challenging and realistic satellite servicing task. RP ZAK, H (reprint author), CALTECH,JET PROP LAB,ADV SYST & ADV COMP TECHNOL SECT,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 47 TC 1 Z9 1 U1 1 U2 1 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017-2394 SN 0018-9472 J9 IEEE T SYST MAN CYB JI IEEE Trans. Syst. Man Cybern. PD FEB PY 1995 VL 25 IS 2 BP 313 EP 327 DI 10.1109/21.364833 PG 15 WC Computer Science, Cybernetics; Engineering, Electrical & Electronic SC Computer Science; Engineering GA QC407 UT WOS:A1995QC40700009 ER PT J AU KOOI, JW CHAN, MS BIN, M BUMBLE, B LEDUC, HG WALKER, CK PHILLIPS, TG AF KOOI, JW CHAN, MS BIN, M BUMBLE, B LEDUC, HG WALKER, CK PHILLIPS, TG TI THE DEVELOPMENT OF AN 850-GHZ WAVE-GUIDE RECEIVER USING TUNED SIS JUNCTIONS ON 1-MU-M SI3N4 MEMBRANES SO INTERNATIONAL JOURNAL OF INFRARED AND MILLIMETER WAVES LA English DT Article ID NOISE AB We report preliminary development work on a 850 GHz SIS heterodyne receiver employing a tuned niobium tunnel junction on a 1 mu m Si3N4 supporting membrane. Since the mixer is meant to be operated well above the superconducting gap frequency of niobium (2 Delta/h approximate to 690 GHz) special care has been taken to minimize transmission line loss. We have therefore used junctions with an integrated radial stub RF matching network to tune out the large shunt susceptance of the junction and minimize the niobium film absorption loss. Scale model measurements of the waveguide embedding impedance have been made to aid in the design of the choke structure and RF matching network. Detailed Fourier Transform Spectrometer measurements of tuned junctions on both SiO2 and silicon nitride membranes show response up to 1100 GHz and indicate that the absorption loss in the niobium film is in the order of 4-7 dB at 850 GHz, in fairly good agreement with the theoretical loss calculated from the Mattis-Bardeen theory. The junctions have a center frequency of 800 GHz which presents a 6% downshift from the designed value. C1 JET PROPULS LAB,CTR SPACE MICROELECTR TECHNOL,PASADENA,CA. UNIV ARIZONA,TUCSON,AZ. RP KOOI, JW (reprint author), CALTECH,DIV PHYS MATH & ASTRON,CALTECH SUBMILLIMETER OBSERV,PASADENA,CA 91125, USA. NR 18 TC 4 Z9 4 U1 0 U2 0 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0195-9271 J9 INT J INFRARED MILLI JI Int. J. Infrared Millimeter Waves PD FEB PY 1995 VL 16 IS 2 BP 349 EP 362 DI 10.1007/BF02096322 PG 14 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA QJ918 UT WOS:A1995QJ91800002 ER PT J AU TARN, TJ DE, PK BEJCZY, AK LI, Z AF TARN, TJ DE, PK BEJCZY, AK LI, Z TI VISUALIZATION OF DUAL-ARM ROBOT MOTION SPACE UNDER KINEMATIC CONSTRAINTS SO INTERNATIONAL JOURNAL OF ROBOTICS RESEARCH LA English DT Article ID WORKSPACE; MANIPULATORS AB This article presents a technique for determining and visualizing the geometric motion capabilities of dual-arm robotic systems when the arms work on an object in a closed kinematic chain configuration, taking account of robot arms' base placements, object dimensions, object holding and contact constraints, and space occupancy conflicts of the two arms links. The constrained and object orientation restricted motion space in general can be visualized as a complex 3D object with hidden unreachable holes or cavities of varying shapes. An automated visualization methodology is presented together with its graphical implementation, illustrated by an example. The methodology is an inverse computer vision technique in the sense that it creates rather than recognizes visual forms. C1 LOCKWOOD GREENE ENGINEERS INC,INFORUM,ATLANTA,GA 30303. WASHINGTON UNIV,SCH MED,MALLINCKRODT INST RADIOL,ST LOUIS,MO 63110. CALTECH,JET PROP LAB,PASADENA,CA 91109. RP TARN, TJ (reprint author), WASHINGTON UNIV,DEPT SYST SCI & ENGN,CAMPUS BOX 1040,ST LOUIS,MO 63130, USA. NR 18 TC 0 Z9 0 U1 0 U2 1 PU MIT PRESS PI CAMBRIDGE PA 55 HAYWARD ST JOURNALS DEPT, CAMBRIDGE, MA 02142 SN 0278-3649 J9 INT J ROBOT RES JI Int. J. Robot Res. PD FEB PY 1995 VL 14 IS 1 BP 9 EP 18 DI 10.1177/027836499501400102 PG 10 WC Robotics SC Robotics GA QH137 UT WOS:A1995QH13700002 ER PT J AU SCHMIDT, EO ARDUINI, RF WIELICKI, BA STONE, RS TSAY, SC AF SCHMIDT, EO ARDUINI, RF WIELICKI, BA STONE, RS TSAY, SC TI CONSIDERATIONS FOR MODELING THIN CIRRUS EFFECTS VIA BRIGHTNESS TEMPERATURE DIFFERENCES SO JOURNAL OF APPLIED METEOROLOGY LA English DT Article ID RADIATIVE-TRANSFER THEORY; OPTICAL-PROPERTIES; ICE CRYSTALS; CLOUD COVER; SCATTERING; PARAMETERIZATION; CLASSIFICATION; ATMOSPHERES; PARTICLES; FIELDS AB Brightness temperature difference (BTD) values are calculated for selected Geostationary Operational Environmental Satellite (GOES-6) channels (3.9, 12.7 mu m) and Advanced Very High Resolution Radiometer channels (3.7, 12.0 mu m). Daytime and nighttime discrimination of particle size information is possible given the infrared cloud extinction optical depth and the BTD value. BTD values are presented and compared for cirrus clouds composed of equivalent ice spheres (volume, surface area) versus randomly oriented hexagonal ice crystals. The effect of the hexagonal ice crystals is to increase the magnitude of the BTD values calculated relative to equivalent ice sphere (volume, surface area) BTDs. Equivalent spheres (volume or surface area) do not do a very good job of modeling hexagonal ice crystal effects on BTDs; however, the use of composite spheres improves the simulation and offers interesting prospects. Careful consideration of the number of Legendre polynomial coefficients used to fit the scattering phase functions is crucial to realistic modeling of cirrus BTDs. Surface and view-angle effects are incorporated to provide more realistic simulation. C1 LOCKHEED ENGN & SCI CO,HAMPTON,VA 23666. NASA,LANGLEY RES CTR,DIV ATMOSPHER SCI,HAMPTON,VA 23665. UNIV COLORADO,COOPERAT INST RES ENVIRONM SCI,BOULDER,CO 80309. UNIV MARYLAND,DEPT METEOROL,COLLEGE PK,MD 20742. NR 33 TC 12 Z9 12 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 SN 0894-8763 J9 J APPL METEOROL JI J. Appl. Meteorol. PD FEB PY 1995 VL 34 IS 2 BP 447 EP 459 DI 10.1175/1520-0450-34.2.447 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QQ916 UT WOS:A1995QQ91600011 ER PT J AU NEGRI, AJ NELKIN, EJ ADLER, RF HUFFMAN, GJ KUMMEROW, C AF NEGRI, AJ NELKIN, EJ ADLER, RF HUFFMAN, GJ KUMMEROW, C TI EVALUATION OF PASSIVE MICROWAVE PRECIPITATION ALGORITHMS IN WINTERTIME MIDLATITUDE SITUATIONS SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID SURROUNDING WATERS; RAINFALL; CLASSIFICATION; IMAGER; JAPAN; SNOW AB The second intercomparison project of the Global Precipitation Climatology Project examined the estimation of midlatitude, cool-season precipitation. As part of that effort, the authors report here on the results of two microwave techniques, the Goddard scattering algorithm and the physical retrieval algorithm of Kummerow. Results from the estimation of instantaneous rain rate for five overpasses of the Special Sensor Microwave/Imager (SSM/I) are presented in a case study mode to illustrate both the strong and weak points of each technique. These five cases represent a sampling of the various types of precipitating systems observed. Results for the complete set of 20 swaths chosen by the United Kingdom Meteorological Office are then categorized by scatterplots and statistics of instantaneous radar versus microwave-estimated rain rate, rain/no-rain contingency tables, and scatterplots of areal coverage of rainfall. Neither algorithm produced a good statistical correlation with the radar data, yet in general, both did well at determining rainy areas. Two reasons are suggested for the low correlation coefficients between both algorithms and the radar data. Time differences between the SSM/I overpass and the radar observations can occasionally account for some of the differences. The primary reason for the low correlations, however, appears to be the predominance of very light rain in the area of interest during the winter. Both algorithms are in good spatial agreement with the radar when the radar data are restricted to rates above 1 mm h-1. When all radar rain rates are included, the radar areal coverage increases by as much as a factor of 10 in some cases. Because the Kummerow algorithm does not handle such low rain rates over land very well, and because the Goddard scattering algorithm uses 1 mm h-1 as the minimum reliably detectable rain rate, regimes that contain large areas of very light rain present inherent difficulties for these retrieval methods. Therefore, the proliferation of low rain rates observed during the experiment is the main contributor to low correlation coefficients and high root-mean-square differences. Misidentification of cold surface (e.g., snow cover) as precipitation was also a problem in several instances. C1 SCI SYST & APPLICAT INC,LANHAM,MD. RP NEGRI, AJ (reprint author), NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,CODE 912,GREENBELT,MD 20771, USA. RI Huffman, George/F-4494-2014 OI Huffman, George/0000-0003-3858-8308 NR 15 TC 19 Z9 19 U1 1 U2 2 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 1995 VL 12 IS 1 BP 20 EP 32 DI 10.1175/1520-0426(1995)012<0020:EOPMPA>2.0.CO;2 PG 13 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA RD058 UT WOS:A1995RD05800003 ER PT J AU KUMMEROW, C GIGLIO, L AF KUMMEROW, C GIGLIO, L TI A METHOD FOR COMBINING PASSIVE MICROWAVE AND INFRARED RAINFALL OBSERVATIONS SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID LOW-ORBIT MICROWAVE; TROPICAL RAINFALL; CONVECTIVE RAINFALL; GEOSYNCHRONOUS IR; STOCHASTIC-MODEL; SATELLITE; CLOUD; RADAR; SPACE; AREAS AB Passive microwave observations of rainfall offer the ability to obtain very accurate instantaneous estimates of rainfall. Because passive microwave instruments are confined to polar-orbiting satellites, however, such estimates must interpolate across long time periods, during which no measurements are available. In this paper the authors discuss a technique that allows one to partially overcome the sampling limitations by using frequent infrared observations from geosynchronous platforms. To accomplish this, the technique compares all coincident microwave and infrared observations. From each coincident pair, the infrared temperature threshold is selected that corresponds to an area equal to the raining area observed in the microwave image. The mean conditional rainfall rate as determined from the microwave image is then assigned to pixels in the infrared image that are colder than the selected threshold. The calibration is also applied to a fixed threshold of 235 K for comparison with established infrared techniques. Once a calibration is determined, it is applied to all infrared images. Monthly accumulations for both methods are then obtained by summing rainfall from all available infrared images. Two examples are used to evaluate the performance of the technique. The first consists of a one-month period (February 1988) over Darwin, Australia, where good validation data are available from radar and rain gauges. For this case it was found that the technique approximately doubled the rain inferred by the microwave method alone and produced exceptional agreement with the validation data. The second example involved comparisons with atoll rain gauges in the western Pacific for June 1989. Results here are overshadowed by the fact that the hourly infrared estimates from established techniques, by themselves, produced very good correlations with the rain gauges. The calibration technique was not able to improve upon these results. C1 SCI SYST & APPLICAT INC,LANHAM,MD. RP KUMMEROW, C (reprint author), NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,CODE 912,GREENBELT,MD 20771, USA. NR 23 TC 34 Z9 36 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 1995 VL 12 IS 1 BP 33 EP 45 DI 10.1175/1520-0426(1995)012<0033:AMFCPM>2.0.CO;2 PG 13 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA RD058 UT WOS:A1995RD05800004 ER PT J AU JONSSON, HH WILSON, JC BROCK, CA KNOLLENBERG, RG NEWTON, R DYE, JE BAUMGARDNER, D BORRMANN, S FERRY, GV PUESCHEL, R WOODS, DC PITTS, MC AF JONSSON, HH WILSON, JC BROCK, CA KNOLLENBERG, RG NEWTON, R DYE, JE BAUMGARDNER, D BORRMANN, S FERRY, GV PUESCHEL, R WOODS, DC PITTS, MC TI PERFORMANCE OF A FOCUSED CAVITY AEROSOL SPECTROMETER FOR MEASUREMENTS IN THE STRATOSPHERE OF PARTICLE-SIZE IN THE 0.06-2.0-MU-M-DIAMETER RANGE SO JOURNAL OF ATMOSPHERIC AND OCEANIC TECHNOLOGY LA English DT Article ID SULFATE AEROSOL; MT-PINATUBO; TEMPERATURE; ERUPTION; COUNTER AB A focused cavity aerosol spectrometer abroad a NASA ER-2 high-altitude aircraft provided high-resolution measurements of the size of the stratospheric particles in the 0.06-2.0-mum-diameter range in flights following the eruption of Mount Pinatubo in 1991. Effects of anisokinetic sampling and evaporation in the sampling system were accounted for by means adapted and specifically developed for this instrument. Calibrations with monodisperse aerosol particles provided the instrument's response matrix, which upon inversion during data reduction yielded the particle size distributions. The resultant dataset is internally consistent and generally shows agreement to within a factor of 2 with comparable measurements simultaneously obtained by a condensation nuclei counter, a forward-scattering spectrometer probe, and aerosol particle impactors, as well as with nearby extinction profiles obtained by satellite measurements and with lidar measurements of backscatter. C1 UNIV MAINZ,W-6500 MAINZ,GERMANY. NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NASA,LANGLEY RES CTR,HAMPTON,VA 23665. PARTICLE MEASURING SYST INC,BOULDER,CO. SCI APPLICAT INT CORP,HAMPTON,VA. NATL CTR ATMOSPHER RES,BOULDER,CO 80307. RP JONSSON, HH (reprint author), UNIV DENVER,DEPT ENGN,2390 YORK ST,DENVER,CO 80208, USA. RI Borrmann, Stephan/E-3868-2010; Brock, Charles/G-3406-2011 OI Brock, Charles/0000-0002-4033-4668 NR 22 TC 69 Z9 69 U1 0 U2 7 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 SN 0739-0572 J9 J ATMOS OCEAN TECH JI J. Atmos. Ocean. Technol. PD FEB PY 1995 VL 12 IS 1 BP 115 EP 129 DI 10.1175/1520-0426(1995)012<0115:POAFCA>2.0.CO;2 PG 15 WC Engineering, Ocean; Meteorology & Atmospheric Sciences SC Engineering; Meteorology & Atmospheric Sciences GA RD058 UT WOS:A1995RD05800009 ER PT J AU ANDERSON, FC ZIEGLER, JM PANDY, MG WHALEN, RT AF ANDERSON, FC ZIEGLER, JM PANDY, MG WHALEN, RT TI APPLICATION OF HIGH-PERFORMANCE COMPUTING TO NUMERICAL-SIMULATION OF HUMAN MOVEMENT SO JOURNAL OF BIOMECHANICAL ENGINEERING-TRANSACTIONS OF THE ASME LA English DT Note AB We have examined the feasibility of using massively-parallel and vector-processing supercomputers to solve large-scale optimization problems for human movement. Specifically, we compared the computational expense of determining the optimal controls for the single support phase of gait using a conventional serial machine (SGI Iris 4025,), a MIMD parallel machine (Intel iPSC/860), and a parallel-vector-processing machine (Cray Y-MP 8/864). With the human body modeled as a 14 degree-of-freedom linkage actuated by 46 musculotendinous units, computation of the optimal controls for gait could take up to 3 months of CPU time on the Iris. Both the Cray and the Intel are able to reduce this lime to practical levels. The optimal solution for gait can be found with about 77 hours of Cpu on the Cray and with about 88 hours of CpU on the Intel. Although the overall speeds of the Cray and the Intel were found to be similar, the unique capabilities of each machine are better suited to different portions of the computational algorithm used. The Intel was best suited to computing the derivatives of the performance criterion and the constraints whereas the Cray was best suited fo parameter optimization of the controls. These results suggest that the ideal computer architecture for solving very large-scale optimal control problems is a hybrid system in which a vector-processing machine is integrated into the communication network of a MIMD parallel machine. C1 UNIV TEXAS,DEPT MECH ENGN,AUSTIN,TX 78712. UNIV TEXAS,BIOMED ENGN PROGRAM,AUSTIN,TX 78712. NASA,AMES RES CTR,DIV LIFE SCI,MOFFETT FIELD,CA 94035. RP ANDERSON, FC (reprint author), UNIV TEXAS,DEPT KINESIOL,AUSTIN,TX 78712, USA. OI Pandy, Marcus/0000-0001-9234-1782 NR 4 TC 20 Z9 20 U1 2 U2 5 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 SN 0148-0731 J9 J BIOMECH ENG-T ASME JI J. Biomech. Eng.-Trans. ASME PD FEB PY 1995 VL 117 IS 1 BP 155 EP 157 DI 10.1115/1.2792264 PG 3 WC Biophysics; Engineering, Biomedical SC Biophysics; Engineering GA QJ949 UT WOS:A1995QJ94900020 PM 7609481 ER PT J AU COLLINS, CL DYALL, KG SCHAEFER, HF AF COLLINS, CL DYALL, KG SCHAEFER, HF TI RELATIVISTIC AND CORRELATION-EFFECTS IN CUH, AGH, AND AUH - COMPARISON OF VARIOUS RELATIVISTIC METHODS SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID SPIN-ORBIT OPERATORS; TRANSITION-METAL HYDRIDES; EFFECTIVE CORE POTENTIALS; HARTREE-FOCK CALCULATIONS; GTO WAVE-FUNCTIONS; BASIS SET QUALITY; ALL-ELECTRON; MOLECULAR CALCULATIONS; CONFIGURATION-INTERACTION; DIPOLE-MOMENT C1 NASA,AMES RES CTR,INST THERMOSCI,MOFFETT FIELD,CA 94035. UNIV GEORGIA,DEPT PHYS & ASTRON,ATHENS,GA 30602. RP COLLINS, CL (reprint author), UNIV GEORGIA,CTR COMPUTAT QUANTUM CHEM,ATHENS,GA 30602, USA. NR 56 TC 70 Z9 70 U1 0 U2 7 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 FEB 1 PY 1995 VL 102 IS 5 BP 2024 EP 2031 DI 10.1063/1.468724 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA QD542 UT WOS:A1995QD54200017 ER PT J AU MEHTA, VM DELWORTH, T AF MEHTA, VM DELWORTH, T TI DECADAL VARIABILITY OF THE TROPICAL ATLANTIC-OCEAN SURFACE-TEMPERATURE IN SHIPBOARD MEASUREMENTS AND IN A GLOBAL OCEAN-ATMOSPHERE MODEL SO JOURNAL OF CLIMATE LA English DT Article ID SEASONAL RAINFALL; NORTHEAST BRAZIL; TIME-SERIES; CIRCULATION; OSCILLATIONS; PREDICTION; VORTICITY; ANOMALIES; DYNAMICS AB Numerous analyses of relatively short (25-30 years in length) time series of the observed surface temperature of the tropical Atlantic Ocean have indicated the possible existence of decadal timescale variability. It was decided to search for such variability in 100-yr time series of sea surface temperature (SST) measured aboard ships and available in the recently published Global Ocean Surface Temperature Atlas (GOSTA). Fourier and singular spectrum analyses of the GOSTA SST time series averaged over 11 subregions, each approximately 1 x 10(6) km(2) in area, show that pronounced quasi-oscillatory decadal (similar to 8-20 yr) and multidecadal (similar to 30-40 yr) timescale variability exists in the GOSTA dataset over the tropical Atlantic. Motivated by the above results, SST variability was investigated in a 200-yr integration of a global model of the coupled oceanic and atmospheric general circulations developed at the Geophysical Fluid Dynamics Laboratory (GFDL). The second 100 yr of SST in the coupled model's tropical Atlantic region were analyzed with a variety of techniques. Analyses of SST time series, averaged over approximately the same subregions as the GOSTA time series, showed that the GFDL SST anomalies also undergo pronounced quasi-oscillatory decadal and multidecadal variability but at somewhat shorter timescales than the GOSTA SST anomalies. Further analyses of the horizontal structures of the decadal timescale variability in the GFDL coupled model showed the existence of two types of variability in general agreement with results of the GOSTA SST time series analyses. One type, characterized by timescales between 8 and 11 yr, has high spatial coherence within each hemisphere but not between the two hemispheres of the tropical Atlantic. A second type, characterized by timescales between 12 and 20 yr, has high spatial coherence between the two hemispheres. The second type of variability is considerably a weaker than the first. As in the GOSTA time series, the multidecadal variability in the GFDL SST time series has approximately opposite phases between the tropical North and South Atlantic Oceans. Empirical orthogonal function analyses of the tropical Atlantic SST anomalies revealed a north-south bipolar pattern as the dominant pattern of decadal variability. It is suggested that the bipolar pattern can be interpreted as decadal variability of the interhemispheric gradient of SST anomalies. The decadal and multidecadal timescale variability of the tropical Atlantic SST, both in the actual and in the GFDL model, stands out significantly above the background ''red noise'' and is coherent within each of the time series, suggesting that specific sets of processes may be responsible for the choice of the decadal and multidecadal timescales. Finally, it must be emphasized that the GFDL coupled ocean-atmosphere model generates the decadal and multidecadal timescale variability without any externally applied force, solar or lunar, at those timescales. C1 PRINCETON UNIV,NOAA,GEOPHYS FLUID DYNAM LAB,PRINCETON,NJ 08542. RP MEHTA, VM (reprint author), NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,UNIV SPACE RES ASSOC,GREENBELT,MD 20771, USA. RI Delworth, Thomas/C-5191-2014 NR 31 TC 94 Z9 96 U1 0 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 SN 0894-8755 J9 J CLIMATE JI J. Clim. PD FEB PY 1995 VL 8 IS 2 BP 172 EP 190 DI 10.1175/1520-0442(1995)008<0172:DVOTTA>2.0.CO;2 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QQ915 UT WOS:A1995QQ91500003 ER PT J AU LYNN, BH RIND, D AVISSAR, R AF LYNN, BH RIND, D AVISSAR, R TI THE IMPORTANCE OF MESOSCALE CIRCULATIONS GENERATED BY SUBGRID-SCALE LANDSCAPE HETEROGENEITIES IN GENERAL-CIRCULATION MODELS SO JOURNAL OF CLIMATE LA English DT Article ID NUMERICAL-MODEL; CLIMATE MODELS; BOUNDARY-LAYER; VEGETATION; IMPACT; PRECIPITATION; SENSITIVITY; ATMOSPHERE; MOISTURE; AREAS AB A mesoscale atmospheric model was used to evaluate the impact of subgrid-scale landscape discontinuities on the vertical profiles of resolved temperature, moisture, and moist static energy in the planetary boundary layer (PBL) of GCMs. These profiles were produced with a 3D version of the model (using a horizontal grid resolution of 7.5 km and 13 vertical layers in the PBL) by averaging horizontally the various atmospheric variables over a 180 X 180 km(2) domain-about the size of the horizontal domain represented by a single grid element in a GCM. They were compared to corresponding vertical profiles produced with a 1D version of the model, which simulates the PBL, as in a GCM, over a single horizontal grid element. Differences obtained between the horizontally averaged atmospheric variables produced with the 3D simulations and the 1D simulations emphasize the impact of subgrid-scale landscape discontinuities on GCM-resolved variables. Various types of landscape discontinuities, characterized by horizontal contrasts of surface wetness and size of land patches, were simulated under various background-wind conditions. Differences of temperature, specific humidity, and moist static energy as large as 4 K, 6 g kg(-1), and 10 kJ kg(-1) were obtained in some cases. These differences were not affected significantly by moderate winds but were sensitive to the spatial distribution of surface wetness. These results emphasize the need to parameterize mesoscale processes induced by landscape discontinuities in GCMs. C1 RUTGERS STATE UNIV,DEPT METEOROL & PHYS OCEANOG,NEW BRUNSWICK,NJ 08903. NASA,GODDARD INST SPACE STUDIES,NEW YORK,NY 10025. NR 38 TC 60 Z9 62 U1 0 U2 1 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 SN 0894-8755 J9 J CLIMATE JI J. Clim. PD FEB PY 1995 VL 8 IS 2 BP 191 EP 205 DI 10.1175/1520-0442(1995)008<0191:TIOMCG>2.0.CO;2 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QQ915 UT WOS:A1995QQ91500004 ER PT J AU LI, ZQ WHITLOCK, CH CHARLOCK, TP AF LI, ZQ WHITLOCK, CH CHARLOCK, TP TI ASSESSMENT OF THE GLOBAL MONTHLY MEAN SURFACE INSOLATION ESTIMATED FROM SATELLITE MEASUREMENTS USING GLOBAL ENERGY-BALANCE ARCHIVE DATA SO JOURNAL OF CLIMATE LA English DT Article ID RADIATION BUDGET; SOLAR-RADIATION; WATER-VAPOR; VARIABILITY; IRRADIANCE; ABSORPTION; ATMOSPHERE; PROJECT; BAND AB Global datasets of surface radiation budget (SRB) have been obtained from satellite programs. These satellite-based estimates need validation with ground-truth observations. This study validates the estimates of monthly mean surface insolation contained in two satellite-based SRB datasets with the surface measurements made at worldwide radiation stations from the Global Energy Balance Archive (GEBA). One dataset was developed from the Earth Radiation Budget Experiment (ERBE) using the algorithm of Li et al. (ERBE/SRB), and the other from the International Satellite Cloud Climatology Project (ISCCP) using the algorithm of Pinker and Laszlo and that of Staylor (GEWEX/SRB). Since the ERBE/SRB data contain the surface net solar radiation only, the values of surface insolation were derived by making use of the surface albedo data contained in the GEWEX/SRB product. The resulting surface insolation has a bias error near zero and a root-mean-square error (RMSE) between 8 and 28 W m(-2). The RMSE is mainly associated with poor representation of surface observations within a grid cell. When the number of surface observations are sufficient, the random error is estimated to be about 5 W m(-2) with present satellite-based estimates. In addition to demonstrating the strength of the retrieving method, the small random error demonstrates how well the ERBE derives the monthly mean fluxes at the top of the atmosphere (TOA). A larger scatter is found for the comparison of transmissivity than for that of insolation. Month to month comparison of insolation reveals a weak seasonal trend in bias error with an amplitude of about 3 W m(-2). As for the insolation data from the GEWEX/SRB, larger bias errors of 5-10 W m(-2) are evident with stronger seasonal trends and almost identical RMSEs. C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23665. RP LI, ZQ (reprint author), CANADA CTR REMOTE SENSING,588 BOOTH ST,OTTAWA,ON K1A 0Y7,CANADA. RI Li, Zhanqing/F-4424-2010 OI Li, Zhanqing/0000-0001-6737-382X NR 35 TC 55 Z9 55 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 SN 0894-8755 J9 J CLIMATE JI J. Clim. PD FEB PY 1995 VL 8 IS 2 BP 315 EP 328 DI 10.1175/1520-0442(1995)008<0315:AOTGMM>2.0.CO;2 PG 14 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QQ915 UT WOS:A1995QQ91500012 ER PT J AU PALOSZ, W LEHOCZKY, SL SZOFRAN, FR AF PALOSZ, W LEHOCZKY, SL SZOFRAN, FR TI THERMOCHEMICAL MODEL OF PHYSICAL VAPOR TRANSPORT OF CADMIUM-ZINC TELLURIDE SO JOURNAL OF CRYSTAL GROWTH LA English DT Article ID SINGLE-CRYSTALS; CLOSED AMPOULES; GROWTH; SUBLIMATION; CDTE AB A theoretical model for the diffusive mass transport of the ternary compound cadmium-zinc telluride by physical vapor transport (PVT) is presented. Considerable differences between the composition of the source and deposited material, and a steep decrease in the mass flu with an increase in ZnTe content in Cd(1-x)ZnxTe crystals have been found for X < 0.1. The difference in composition between the crystal and the source decreases with a decrease in undercooling Delta T and/or with an increase in the excess of metal constituents (Cd + Zn) in the vapor phase. RP PALOSZ, W (reprint author), NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB,HUNTSVILLE,AL 35812, USA. NR 27 TC 14 Z9 14 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 J9 J CRYST GROWTH JI J. Cryst. Growth PD FEB PY 1995 VL 148 IS 1-2 BP 49 EP 55 DI 10.1016/0022-0248(94)00833-7 PG 7 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA QJ642 UT WOS:A1995QJ64200009 ER PT J AU PALOSZ, W SZOFRAN, FR LEHOCZKY, SL AF PALOSZ, W SZOFRAN, FR LEHOCZKY, SL TI EXPERIMENTAL STUDIES ON MASS-TRANSPORT OF CADMIUM-ZINC TELLURIDE BY PHYSICAL VAPOR TRANSPORT SO JOURNAL OF CRYSTAL GROWTH LA English DT Article ID CLOSED AMPOULES AB Experimental studies on mass transport of ternary compound, Cd1-xZnxTe by physical vapor transport (PVT) for source compositions up to X=0.21 are presented. The effect of thermochemical (temperatures, vapor composition) and other factors (preparation of the source, crystal growth rate, temperature gradient) on composition and composition profiles of the grown crystals were investigated. A steep decrease in the mass flux with an increase in X(crystal) for X < 0.1, and a difference in composition between the source and the deposited material have been observed. The composition profiles of the crystals were found to depend on the density and pretreatment of the source, and on the temperature gradient in the source zone. The homogeneity of the crystals improves at low undercoolings and/or when an appropriate excess of metal constituents is present in the vapor phase. The experimental results are in good agreement with our thermochemical model of this system. RP PALOSZ, W (reprint author), NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB,HUNTSVILLE,AL 35812, USA. NR 6 TC 12 Z9 12 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 J9 J CRYST GROWTH JI J. Cryst. Growth PD FEB PY 1995 VL 148 IS 1-2 BP 56 EP 62 DI 10.1016/0022-0248(94)00834-5 PG 7 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA QJ642 UT WOS:A1995QJ64200010 ER PT J AU CHEN, KT GEORGE, MA ZHANG, Y BURGER, A SU, CH SHA, YG GILLIES, DC LEHOCZKY, SL AF CHEN, KT GEORGE, MA ZHANG, Y BURGER, A SU, CH SHA, YG GILLIES, DC LEHOCZKY, SL TI SELENIUM PRECIPITATION IN ZNSE CRYSTALS GROWN BY PHYSICAL VAPOR TRANSPORT SO JOURNAL OF CRYSTAL GROWTH LA English DT Article ID MOLECULAR-BEAM EPITAXY; ATOMIC-FORCE MICROSCOPY AB The morphology of freshly cleaved ZnSe surfaces was investigated by atomic force microscopy and the results were correlated with differential scanning calorimetry (DSC) data. Selenium precipitates in undoped ZnSe crystals grown by the physical vapor transport method were determined. The Se inclusions have a size of about 20 nm. A transition temperature at 221 degrees C in the DSC measurement is interpreted as the eutectic temperature of Se-saturated ZnSe. The total amount of the ZnSe/Se-rich second phase was 0.8 wt%, and some segregation effect along low angle grain boundaries was evident. C1 FISK UNIV,CTR PHOTON MAT & DEVICES,DEPT PHYS,NASHVILLE,TN 37208. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB,HUNTSVILLE,AL 35812. NR 18 TC 4 Z9 5 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 J9 J CRYST GROWTH JI J. Cryst. Growth PD FEB PY 1995 VL 147 IS 3-4 BP 292 EP 296 DI 10.1016/0022-0248(94)00733-0 PG 5 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA QG489 UT WOS:A1995QG48900007 ER PT J AU RYER, CH OLLA, BL AF RYER, CH OLLA, BL TI THE INFLUENCE OF FOOD DISTRIBUTION UPON THE DEVELOPMENT OF AGGRESSIVE AND COMPETITIVE BEHAVIOR IN JUVENILE CHUM SALMON, ONCORHYNCHUS-KETA SO JOURNAL OF FISH BIOLOGY LA English DT Article DE CHUM SALMON; NATURE; NURTURE; FOOD DISTRIBUTION; AGGRESSION; FISH BEHAVIOR; DOMINANCE; GROWTH DEPENSATION ID SALVELINUS-ALPINUS L; AGONISTIC BEHAVIOR; ATLANTIC SALMON; COHO SALMON; ARCTIC CHARR; SALAR L; POPULATIONS; HATCHERY; GROWTH; WILD AB Groups of juvenile chum salmon were reared on food that was either dispersed throughout. or localized in one area of, the rearing tank. Groups receiving localized food displayed more aggression than those receiving dispersed food. This led to differences in growth, with fish reared on localized food having greater individual growth variability, i.e. growth depensation. However, after several months of rearing in these different feeding/social environments, fish reared on dispersed food were just as aggressive when first exposed to localized food as were fish reared on localized food. Furthermore. in competitive contests between fish of the two rearing histories, those reared on dispersed food were just as likely to become dominant as those reared on localized food. These results suggest that the behavioural development of aggressiveness is not amenable to alteration by manipulation of food distribution. RP RYER, CH (reprint author), OREGON STATE UNIV,HATFIELD MARINE SCI CTR,NATL MARINE FISHERIES SERV,ALASKA FISHERIES SCI CTR,NEWPORT,OR 97365, USA. NR 32 TC 54 Z9 54 U1 1 U2 4 PU ACADEMIC PRESS (LONDON) LTD PI LONDON PA 24-28 OVAL RD, LONDON, ENGLAND NW1 7DX SN 0022-1112 J9 J FISH BIOL JI J. Fish Biol. PD FEB PY 1995 VL 46 IS 2 BP 264 EP 272 DI 10.1111/j.1095-8649.1995.tb05967.x PG 9 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA QM968 UT WOS:A1995QM96800007 ER PT J AU ESCOUBET, CP SMITH, MF FUNG, SF HOFFMAN, RA BOSQUED, JM AF ESCOUBET, CP SMITH, MF FUNG, SF HOFFMAN, RA BOSQUED, JM TI ELECTRON STRUCTURES IN THE CUSP CLEFT REGION OBSERVED BY DE-2 SATELLITE SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID FLUX-TRANSFER EVENTS; AURORAL PARTICLE-ACCELERATION; INTERPLANETARY MAGNETIC-FIELD; DEPENDENT PLASMA-FLOW; SOLAR-WIND; DAYSIDE MAGNETOPAUSE; BIRKELAND CURRENTS; BOUNDARY-LAYER; POLAR CUSP; IONOSPHERIC SIGNATURES AB Narrow enhancements of electron precipitation, with energy and flux well above typical values, have been observed with DE 2 in the cusp/cleft region. The electron flux in the energy range 0.2-1 keV was 2 orders of magnitude higher in these structures than in the magnetosheath and were seen in approximately 80% of DE 2 cusp crossings at ionospheric altitudes. Typically, there was more than one electron structure in each cusp crossing. The position of these structures showed a systematic variation: for poleward ion dispersion (energy decreases with increasing latitude), electron structures were seen more often on the equatorial boundary of the cusp, while for equatorward ion dispersion (energy decreases with decreasing latitude), electron structures were more often seen on the poleward boundary. This suggests that the electron structures are associated with newly reconnected field lines. The electron spectra suggest that field-aligned acceleration processes could produce the electron structures, first near the boundary of the cusp/cleft during the reconnection of field lines and then in the cusp/cleft during the motion of reconnected flux tubes through the polar ionosphere. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. CTR ETUD SPATIALE RAYONNEMENTS,CNRS,UPS,F-31029 TOULOUSE,FRANCE. RI Fung, Shing/F-5647-2012 NR 72 TC 3 Z9 3 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 FEB 1 PY 1995 VL 100 IS A2 BP 1597 EP 1610 DI 10.1029/94JA02307 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QH751 UT WOS:A1995QH75100002 ER PT J AU LEE, RB GIBSON, MA WILSON, RS THOMAS, S AF LEE, RB GIBSON, MA WILSON, RS THOMAS, S TI LONG-TERM TOTAL SOLAR IRRADIANCE VARIABILITY DURING SUNSPOT CYCLE-22 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SURFACE-TEMPERATURE; RADIATION BUDGET; LUMINOSITY; CLIMATE; LENGTH; FLUX AB Total solar irradiance measurements from the 1984-1993 Earth Radiation Budget Satellite (ERBS) active cavity radiometer and 1978-1993 Nimbus 7 transfer cavity radiometer spacecraft experiments are analyzed to detect the presences of 11-, 22-, and 80-year irradiance variability components, The analyses confirmed the existence of a significant 11-year irradiance variability component, associated with solar magnetic activity and the sunspot cycle. The analyses also suggest the presence of a 22- or 80-year variability component. The earlier Nimbus 7 and Solar Maximum Mission (SMM) spacecraft irradiance measurements decreased approximately 1.2 and 1.3 Wm(-2), respectively, between 1980 and 1986. The Nimbus 7 values increased 1.2 Wm(-2) between 1986 and 1989. The ERBS irradiance measurements increased 1.3 W-m-2 during 1986-1989, and then decreased 0.4 Wm(-2) (at an annual rate of 0.14 Wm(-2)yr(-1)) during 1990-1993. Considering the correlations between ERBS, Nimbus 7, and SMM irradiance trends and solar magnetic activity, the total solar irradiance should decrease to minimum levels by 1997 as solar activity decreases to minimum levels, and then increase to maximum levels by the year 2000 as solar activity rises. The ERBS measurements yielded 1365.4 +/- 0.7 Wm(-2) as the mean irradiance value with measurement accuracies and precisions of 0.2% and 0.02%, respectively. The ERBS mean irradiance value is within 0.2% of the 1367.4, 1365.9, and 1366.9 Wm(-2) mean values for the SMM, Upper Atmosphere Research Satellite (UARS), and Space Shuttle Atmospheric Laboratory for Applications and Science (ATLAS 1) Solar Constant (SOLCON) active cavity radiometer spacecraft experiments, respectively. The Nimbus 7 measurements yielded 1372.1 Wm(-2) as the mean value with a measurement accuracy of 0.5%. Empirical irradiance model fits, based upon 10.7-cm solar radio flux (F10) and photometric sunspot index (PSI), were used to assess the quality of the ERBS, Nimbus 7, SMM, and the UARS irradiance data sets and to identify irradiance variability trends which may be caused by drifts or shifts in the spacecraft sensor responses. Comparisons among the fits and measured irradiances indicate that the Nimbus 7 radiometer response shifted by a total of 0.8 Wm(-2) between September 1989 and April 1990 and that the ERBS and UARS radiometers each drifted approximately 0.5 Wm(-2) during the first 5 months in orbit. C1 SCI APPLICAT INT CORP,HAMPTON,VA 23666. RP LEE, RB (reprint author), NASA,LANGLEY RES CTR,DIV ATMOSPHER SCI,HAMPTON,VA 23681, USA. NR 42 TC 95 Z9 95 U1 1 U2 4 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 FEB 1 PY 1995 VL 100 IS A2 BP 1667 EP 1675 DI 10.1029/94JA02897 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QH751 UT WOS:A1995QH75100008 ER PT J AU KATZ, I LILLEY, JR GREB, A MCCOY, JE GALOFARO, J FERGUSON, DC AF KATZ, I LILLEY, JR GREB, A MCCOY, JE GALOFARO, J FERGUSON, DC TI PLASMA TURBULENCE ENHANCED CURRENT COLLECTION - RESULTS FROM THE PLASMA MOTOR GENERATOR ELECTRODYNAMIC TETHER FLIGHT SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CATHODE AB The plasma motor generator (PMG) experiment, launched June 26, 1993, was a tethered system of two identical plasma contactors connected via a 500-m conducting tether. The experiment was designed to demonstrate the ability of plasma contactors to provide a low-impedance connection between a spacecraft and the ionosphere for both the electron emission and collection. The flight data indicate that plasma contactors enhance electron collection and emission by both neutralizing the electron space charge and scattering electrons across the geomagnetic field lines. Up to a 0.3 A steady current flowed along the tether in a circuit completed through the ionosphere. An analytical model for plasma contactor interaction with a background plasma which incorporates electron scattering by plasma waves is compared with the flight data. Good agreement between the model and the data is achieved for an effective scattering frequency equal to one twentieth of the local plasma contactor plasma frequency. C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44185. NASA,LYNDON B JOHNSON SPACE CTR,HOUSTON,TX 77058. RP KATZ, I (reprint author), MAXWELL LABS INC,DIV S CUBED,POB 1620,LA JOLLA,CA 92038, USA. NR 7 TC 12 Z9 12 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 FEB 1 PY 1995 VL 100 IS A2 BP 1687 EP 1690 DI 10.1029/94JA03142 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QH751 UT WOS:A1995QH75100010 ER PT J AU SZABO, A LEPPING, RP AF SZABO, A LEPPING, RP TI NEPTUNE INBOUND BOW SHOCK SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID SOLAR-WIND FLOW; PERPENDICULAR SHOCKS; PLASMA OBSERVATIONS; ION DISTRIBUTIONS; RESOLVED LAYER; GYRATING IONS; HIGH-BETA; VOYAGER-2; COLLISIONLESS; ELECTRONS AB Voyager 2 crossed the inbound or upstream Neptunian bow shock at 1430 spacecraft event time on August 24 in 1989 (Belcher et al., 1989). The plasma and magnetic field measurements allow us to study the solar wind interaction with the outermost gas giant. To fully utilize all of the spacecraft observations, an improved nonlinear least squares, ''Rankine-Hugoniot'' magnetohydrodynamic shock-fitting technique has been developed (Szabo, 1994). This technique,is applied to the Nptunian data set. We find that the upstream bow shock normal points nearly exactly toward the Sun consistent with any reasonable large-scale model of the bow shock for a near subsolar crossing. The shock was moving outward with a speed of 14 +/- 12 km/s. The shock can be characterized as a low beta, high Mach number, strong quasi-perpendicular shock. Finally, the shock microstructure features are resolved and found to scale well with theoretical expectations. C1 MIT,DEPT PHYS,CAMBRIDGE,MA 02139. MIT,CTR SPACE RES,CAMBRIDGE,MA 02139. RP SZABO, A (reprint author), NASA,GODDARD SPACE FLIGHT CTR,EXTRATERR PHYS LAB,GREENBELT,MD 20771, USA. NR 33 TC 13 Z9 13 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 FEB 1 PY 1995 VL 100 IS A2 BP 1723 EP 1730 DI 10.1029/94JA02491 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QH751 UT WOS:A1995QH75100013 ER PT J AU CANE, HV RICHARDSON, IG AF CANE, HV RICHARDSON, IG TI COSMIC-RAY DECREASES AND SOLAR-WIND DISTURBANCES DURING LATE OCTOBER-1989 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MAGNETIC CLOUDS; INTERPLANETARY SHOCKS; VOYAGER; IMP-8 AB We describe the interplanetary phenomena (energetic particles, solar wind plasma, and magnetic field) seen at IMP 8 and at ICE, located 65 degrees west of IMP 8, during the period October 19-31, 1989, when neutron monitors observed three ground level events originating in one active region when it was in the longitude range E09 degrees to W57 degrees. At least four shocks, associated with energetic particle enhancements, which can be attributed to a sequence of coronal mass ejections from the same active region, were seen at both spacecraft. An additional shock was observed only at ICE late in this period when the active region was behind the west limb. Considering all the data (which unfortunately suffer from large gaps), it appears that the ejecta associated with the shocks were detected only when the spacecraft and solar source longitude were separated by less than 50 degrees. The shocks extended over a greater range of longitudes. The cosmic ray record at Earth is consistent with this picture such that only the first two shock-associated cosmic ray decreases had the signature expected for intercepting ejecta material. This same time period was also examined by Bavassano et al. (1994). However, we do not agree with their conclusion that ''magnetic clouds'' extending at least 75 degrees from the source longitude were present. C1 UNIV TASMANIA,DEPT PHYS,HOBART,TAS 7001,AUSTRALIA. UNIV MARYLAND,DEPT ASTRON,COLLEGE PK,MD 20742. RP CANE, HV (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. OI Richardson, Ian/0000-0002-3855-3634 NR 27 TC 34 Z9 34 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 FEB 1 PY 1995 VL 100 IS A2 BP 1755 EP 1762 DI 10.1029/94JA03073 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QH751 UT WOS:A1995QH75100017 ER PT J AU KUMAR, S WHITE, SM AF KUMAR, S WHITE, SM TI DEPENDENT SCATTERING PROPERTIES OF WOVEN FIBROUS INSULATIONS FOR NORMAL INCIDENCE SO JOURNAL OF HEAT TRANSFER-TRANSACTIONS OF THE ASME LA English DT Article DE RADIATION; RADIATION INTERACTIONS ID RADIATIVE PROPERTIES; EXTINCTION; ABSORPTION; PARTICLES; SOOT; WAVE AB The scattering properties of woven fibrous materials are examined in this paper and a simple model is presented to account for the interactions between the scattered radiation from different individual fibers. The case of a normally incident plane electromagnetic wave is considered. Fiber sizes in the Rayleigh regime are considered for developing closed-form solutions. Previous studies in the literature that have addressed the scattering properties of fibrous materials have mostly ignored the effect of constructive or destructive addition of scattered waves from individual fibers, the exception being the case of parallel fibers. The difference in the effects of interference on scattering properties of parallel fibers and of woven fabrics arises from the additional interaction of radiation scattered from mutually perpendicular fibers in the latter case, which further complicates the analysis. C1 NASA,AMES RES CTR,THERMAL PROTECT MAT BRANCH,MOFFETT FIELD,CA 94035. RP KUMAR, S (reprint author), POLYTECH INST NEW YORK,DEPT MECH ENGN,333 JAY ST,BROOKLYN,NY 11201, USA. RI Kumar, Sunil/H-1082-2012 NR 14 TC 9 Z9 9 U1 0 U2 0 PU ASME-AMER SOC MECHANICAL ENG PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 SN 0022-1481 J9 J HEAT TRANS-T ASME JI J. Heat Transf.-Trans. ASME PD FEB PY 1995 VL 117 IS 1 BP 160 EP 166 DI 10.1115/1.2822297 PG 7 WC Thermodynamics; Engineering, Mechanical SC Thermodynamics; Engineering GA QK777 UT WOS:A1995QK77700020 ER PT J AU ROYBAL, RE MIGLIONICO, CJ STEIN, C MURR, LE LINCOLN, KA AF ROYBAL, RE MIGLIONICO, CJ STEIN, C MURR, LE LINCOLN, KA TI CHARACTERIZATION OF VAPOR PLUME SPECIES AND DEPOSITION RESIDUES RESULTING FROM PULSED-LASER ABLATION OF A GRAPHITE-EPOXY COMPOSITE SO JOURNAL OF MATERIALS SCIENCE LA English DT Article AB A modified time-of-flight mass spectrometer fitted with a special collection stage for carbon-coated transmission electron microscope specimen grids is used to monitor laser-pulse ablation products from graphite/epoxy composite targets. Scanning electron microscopy observations show ablation damage to consist of matrix pyrolysis, fibre fracture and spallation of fragments which include elemental hydrogen, carbon epoxide and acetylene groups. Transmission electron microscope examination of specimen grids showed a variety of crystals and polycrystalline hexagonal graphites having a wide range of shapes including spheres and faceted polyhedra and platelets, textured flake structures, and microrosettes. These observations lend some credibility to a model for laser-shock and pyrolysis effects which create molecular plume fragments and deposition fragments of hexagonal graphite. C1 UNIV TEXAS,DEPT MET & MAT ENGN,EL PASO,TX 79968. NASA,AMES RES CTR,ELORET INST,MOFFETT FIELD,CA 94035. RP ROYBAL, RE (reprint author), VTSI,PHILLIPS LAB,SPACE ENVIRONM INTERACT BRANCH,KIRTLAND AFB,NM 87117, USA. OI Murr, Lawrence/0000-0001-5942-8376 NR 14 TC 2 Z9 2 U1 0 U2 6 PU CHAPMAN HALL LTD PI LONDON PA 2-6 BOUNDARY ROW, LONDON, ENGLAND SE1 8HN SN 0022-2461 J9 J MATER SCI JI J. Mater. Sci. PD FEB 1 PY 1995 VL 30 IS 3 BP 800 EP 808 DI 10.1007/BF00356345 PG 9 WC Materials Science, Multidisciplinary SC Materials Science GA QG988 UT WOS:A1995QG98800035 ER PT J AU DHERE, NG WATERHOUSE, DL SUNDARAM, KB MELENDEZ, O PARIKH, NR PATNAIK, B AF DHERE, NG WATERHOUSE, DL SUNDARAM, KB MELENDEZ, O PARIKH, NR PATNAIK, B TI STUDIES ON CHEMICAL BATH DEPOSITED CADMIUM-SULFIDE FILMS BY BUFFER SOLUTION TECHNIQUE SO JOURNAL OF MATERIALS SCIENCE-MATERIALS IN ELECTRONICS LA English DT Article ID CDS THIN-FILMS; SOLAR-CELLS AB Cadmium sulphide films were grown by a chemical bath technique using cadmium acetate and cadmium chloride as the Cd ion source and thiourea as the sulphur source. The solution growth process was carried out with and without buffer solutions containing ammonium acetate and ammonium chloride onto glass substrates. Various properties of the films such as surface morphology, crystallinity, composition, optical properties and dark resistivities were compared for both the above techniques. C1 UNIV CENT FLORIDA,DEPT ELECT & COMP ENGN,ORLANDO,FL 32816. NASA,J F KENNEDY SPACE CTR,KENNEDY SPACE CTR,FL 32889. UNIV N CAROLINA,DEPT PHYS & ASTRON,CHAPEL HILL,NC 27599. RP DHERE, NG (reprint author), FLORIDA SOLAR ENERGY CTR,CAPE CANAVERAL,FL 32920, USA. NR 20 TC 21 Z9 24 U1 1 U2 7 PU CHAPMAN HALL LTD PI LONDON PA 2-6 BOUNDARY ROW, LONDON, ENGLAND SE1 8HN SN 0957-4522 J9 J MATER SCI-MATER EL JI J. Mater. Sci.-Mater. Electron. PD FEB PY 1995 VL 6 IS 1 BP 52 EP 59 PG 8 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Engineering; Materials Science; Physics GA RD077 UT WOS:A1995RD07700010 ER PT J AU GOTSIS, PK GUPTILL, JD AF GOTSIS, PK GUPTILL, JD TI FREE-VIBRATION OF FIBER-COMPOSITE THIN SHELLS IN A HOT ENVIRONMENT SO JOURNAL OF REINFORCED PLASTICS AND COMPOSITES LA English DT Article DE LAMINATED CYLINDERS; FIBER COMPOSITES; ANGLE-PLY LAMINATES; COMPOSITE STRUCTURES; COMPUTATIONAL SIMULATION; RESIDUAL STRESSES; HIGH TEMPERATURE; MOISTURE; STRUCTURAL ANALYSIS; FINITE ELEMENT ANALYSIS; FREE VIBRATION; NATURAL FREQUENCIES; MODE SHAPE AB Results are presented of parametric studies to assess the effects of various parameters on the free vibration behavior (natural frequencies) of [+/-theta](2) angle-ply fiber composite thin shells in a hot environment. These results were obtained by using a three-dimensional finite element structural analysis computer code. The fiber composite shell is assumed to be cylindrical and made from T300 graphite fibers embedded in an intermediate-modulus high-strength matrix (IMHS). The residual stresses induced into the laminated structure during the curing are taken into account. The following parameters are investigated: the length and the thickness of the shell, the fiber orientations, the fiber volume fraction, the temperature profile through the thickness of the laminate and the different ply thicknesses. Results obtained indicate that: the fiber orientations and the length of the laminated shell had significant effect on the natural frequencies. The fiber volume fraction, the laminate thickness and the temperature profile through the shell thickness had a weak effect on the natural frequencies. Finally, the laminates with different ply thicknesses had insignificant influence on the behavior of the vibrated laminated shell. RP GOTSIS, PK (reprint author), NASA,LEWIS RES CTR,CLEVELAND,OH 44135, USA. NR 12 TC 2 Z9 2 U1 0 U2 0 PU TECHNOMIC PUBL CO INC PI LANCASTER PA 851 NEW HOLLAND AVE, BOX 3535, LANCASTER, PA 17604 SN 0731-6844 J9 J REINF PLAST COMP JI J. Reinf. Plast. Compos. PD FEB PY 1995 VL 14 IS 2 BP 143 EP 163 PG 21 WC Materials Science, Composites; Polymer Science SC Materials Science; Polymer Science GA QM812 UT WOS:A1995QM81200004 ER PT J AU SHEN, SH LAU, KM AF SHEN, SH LAU, KM TI BIENNIAL OSCILLATION ASSOCIATED WITH THE EAST-ASIAN SUMMER MONSOON AND TROPICAL SEA-SURFACE TEMPERATURES SO JOURNAL OF THE METEOROLOGICAL SOCIETY OF JAPAN LA English DT Article ID NINO SOUTHERN OSCILLATION; EL-NINO; NORTHERN SUMMER; PACIFIC; ANOMALIES; CHINA; TIME AB In this paper, the interannual variability of the East Asian summer monsoon (EASM) rainfall and the tropical sea surface temperature (SST) have been studied. It is found that the EASM rainfall possesses a strong biennial signal, which is particularly pronounced over the southeast China. For the SST, the biennial oscillation is the second most significant quasi-periodic signal over the entire tropical Indian and Pacific Oceans. Results indicate that the biennial variations in the SST and EASM rainfall are closely linked. The SST pattern which is best correlated with EASM rainfall appears in the form of a double see-saw with quasi-stationary centers of action over the Indian Ocean, the Asian monsoon region and the eastern Pacific. The most pronounced SST signals are found in the equatorial eastern Pacific and Indian Ocean about two seasons preceding and following the EASM rainfall. Evidence is presented suggesting that the biennial variability of the EASM rainfall is phase-locked to a global scale biennial oscillation involving the interplay of the Asian monsoon, the Hadley and Walker circulations, and basin wide fluctuations in SST. In particular, the eastward propagation of zonal wind anomalies from the Indian Ocean to the western Pacific, which regulates the moisture fluxes from the western Pacific to the East Asian region, appears to be a key component of the biennial fluctuation associated with EASM rainfall. Results suggest that the relationship between the Asian monsoon and tropical SST is more robust in the biennial than the ENSO time scale, hence raising the possibility that the biennial oscillation may be more fundamentally related to monsoon-ocean-atmosphere interaction than ENSO itself. C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. RP SHEN, SH (reprint author), UNIV MARYLAND,DEPT METEOROL,COLLEGE PK,MD 20742, USA. RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 NR 26 TC 145 Z9 169 U1 0 U2 5 PU METEOROLOGICAL SOC JPN PI TOKYO PA C/O JPN METEOROL AGENCY 1-3-4 OTE-MACHI, CHIYODA-KU, TOKYO JAPAN SN 0026-1165 J9 J METEOROL SOC JPN JI J. Meteorol. Soc. Jpn. PD FEB PY 1995 VL 73 IS 1 BP 105 EP 124 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QN847 UT WOS:A1995QN84700009 ER PT J AU FEIBELMAN, WA AF FEIBELMAN, WA TI P-CYGNI AND ITS CLUSTER SO JOURNAL OF THE ROYAL ASTRONOMICAL SOCIETY OF CANADA LA English DT Editorial Material RP FEIBELMAN, WA (reprint author), NASA,GODDARD SPACE FLIGHT CTR,CODE 684 1,GREENBELT,MD 20771, USA. NR 0 TC 2 Z9 2 U1 0 U2 0 PU ROYAL ASTRON SOC CANADA PI TORONTO PA 136 DUPONT ST, TORONTO ON M5R 1V2, CANADA SN 0035-872X J9 J ROY ASTRON SOC CAN JI J. R. Astron. Soc. Can. PD FEB PY 1995 VL 89 IS 1 BP 3 EP 5 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QZ079 UT WOS:A1995QZ07900001 ER PT J AU TOWNSEND, RE POOLEY, SG AF TOWNSEND, RE POOLEY, SG TI FRACTIONAL LICENSES - AN ALTERNATIVE TO LICENSE BUY-BACKS SO LAND ECONOMICS LA English DT Article ID FISHERIES C1 NATL MARINE FISHERIES SERV,SW FISHERIES SCI CTR,HONOLULU LAB,HONOLULU,HI. RP TOWNSEND, RE (reprint author), UNIV MAINE,DEPT ECON,ORONO,ME 04473, USA. NR 9 TC 1 Z9 2 U1 0 U2 0 PU UNIV WISCONSIN PI MADISON PA SOCIAL SCIENCE BLDG, MADISON, WI 53706 SN 0023-7639 J9 LAND ECON JI Land Econ. PD FEB PY 1995 VL 71 IS 1 BP 141 EP 143 DI 10.2307/3146765 PG 3 WC Economics; Environmental Studies SC Business & Economics; Environmental Sciences & Ecology GA QE484 UT WOS:A1995QE48400012 ER PT J AU GREENLEAF, JE JACKSON, CGR LAWLESS, D AF GREENLEAF, JE JACKSON, CGR LAWLESS, D TI CD4+ CD8+ T-LYMPHOCYTE RATIO - EFFECTS OF REHYDRATION BEFORE EXERCISE IN DEHYDRATED MEN SO MEDICINE AND SCIENCE IN SPORTS AND EXERCISE LA English DT Article DE DRINKS; DRINKING; IMMUNE FUNCTION; PLASMA VOLUME; PLASMA OSMOLALITY ID PHYSICAL EXERCISE; SUBPOPULATIONS; STRESS; RESPONSES AB Effects of fluid ingestion on CD4+/CD8+ T-lymphocyte cell ratios were measured in four dehydrated men (ages 30-46 yr) before and after 70 min of supine submaximal (71% VO2max) lower extremity cycle exercise. Just before exercise, Evans blue dye was injected for measurement of plasma volume. The subjects then drank one of six fluid formulations (12 ml.kg(-1)) in 3-4 min. All six mean post-hydration (pre-exercise) CD4+/CD8+ ratios (Becton-Dickinson Fluorescence Activated Cell Sorter and FACScan Consort-30 software program [San Jose, CA]) were below the normal range of 1.2-1.5; mean (+/- SE) and range were 0.77 +/- 0.12 and 0.39-1.15, respectively. The post-exercise ratios increased: mean = 1.36 +/- 0.15 (P < 0.05) and range = 0.98-1.98. Regression of mean CD4+/CD8+ ratios on mean plasma osmolality resulted in pre- and post-exercise correlation coefficients of -0.76 (P < 0.10) and -0.92 (P < 0.01), respectively. The decreased pre-exercise ratios (after drinking) were probably not caused by the Evans blue dye but appeared to be associated more with the stress (osmotic) of dehydration. The increased post-exercise ratios to normal levels accompanied the rehydration and were not due to the varied electrolyte and osmotic concentrations of the ingested fluids or to the varied vascular volume shifts during exercise. Thus, the level of subject hydration and plasma osmolality may be factors involved in the mechanism of immune system modulation induced by exercise. C1 UNIV NO COLORADO,GREELEY,CO 80639. ROCKEFELLER UNIV,CELLULAR PHYSIOL & IMMUNOL LAB,NEW YORK,NY 10021. RP GREENLEAF, JE (reprint author), NASA,AMES RES CTR,HUMAN ENVIRONM PHYSIOL LAB 23911,GRAVITAT PHYSIOL BRANCH 23911,MOFFETT FIELD,CA 94035, USA. NR 23 TC 9 Z9 9 U1 1 U2 3 PU WILLIAMS & WILKINS PI BALTIMORE PA 351 WEST CAMDEN ST, BALTIMORE, MD 21201-2436 SN 0195-9131 J9 MED SCI SPORT EXER JI Med. Sci. Sports Exerc. PD FEB PY 1995 VL 27 IS 2 BP 194 EP 199 PG 6 WC Sport Sciences SC Sport Sciences GA QF640 UT WOS:A1995QF64000008 PM 7723642 ER PT J AU RAJ, SV FARMER, SC AF RAJ, SV FARMER, SC TI CHARACTERISTICS OF A NEW CREEP REGIME IN POLYCRYSTALLINE NIAL SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID PLASTIC-FLOW PROPERTIES; GRAIN-SIZE; TEMPERATURE; DEFORMATION; MECHANISMS; DEPENDENCE; BEHAVIOR; 1000-K; 1300-K; COAL AB Constant-load creep tests were conducted on fine-grained (similar to 23 mu m) Ni-50.6 (at, pet) Al in the temperature range of 1000 to 1400 K. Power-law creep with a stress exponent, n approximate to 6.5, and an activation energy, Q(c) approximate to 290 kJ mol(-1), was observed above 25 MPa, while a new mechanism with n approximate to 2 and Q(c) approximate to 100 kJ mol(-1) dominates when sigma < 25 MPa, where sigma is the applied stress. A comparison of the creep behavior of fine- and coarse-grained NiAl established that the mechanism in the n approximate to 2 region was dependent on grain size, and the magnitude of the grain-size exponent was estimated to be about 2. Transmission electron microscopy (TEM) observations of the deformed specimens revealed a mixture of dislocation tangles, dipoles, loops, and sub-boundary networks in the power-law creep regime. The deformation microstructures were inhomogeneous in the n approximate to 2 creep regime, and many grains did not reveal any dislocation activity. However, bands of dislocation loops were observed in a few grains, where these loops appeared to have been emitted from the grain boundaries. The observed creep characteristics of the low-stress region suggest the dominance of an accommodated grain-boundary sliding (GBS) mechanism, although the experimental creep rates were lower than those predicted by theoretical models by over seven orders of magnitude. The low value of Q(c) in this region, which is approximately one-third that for lattice self-diffusion, is attributed to the possible existence of interconnected vacancy flow channels, or ''nanotubes,'' at the grain boundaries. RP RAJ, SV (reprint author), NASA,LEWIS RES CTR,CLEVELAND,OH 44135, USA. NR 44 TC 20 Z9 20 U1 1 U2 3 PU MINERALS METALS MATERIALS SOC PI WARRENDALE PA 420 COMMONWEALTH DR, WARRENDALE, PA 15086 SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD FEB PY 1995 VL 26 IS 2 BP 343 EP 356 DI 10.1007/BF02664671 PG 14 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA QC367 UT WOS:A1995QC36700010 ER PT J AU SMIALEK, JL TUBBS, BK AF SMIALEK, JL TUBBS, BK TI EFFECT OF SULFUR REMOVAL ON SCALE ADHESION TO PWA-1480 SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID ADHERENCE; ELEMENTS; ALLOYS AB A commercial superalloy, PWA 1480, was annealed in hydrogen at 1000 degrees C to 1300 degrees C in order to remove a 10 ppmw sulfur impurity. This treatment was very successful above 1200 degrees C, resulting in residual sulfur contents below 0.1 ppmw. The degree of scale adhesion in subsequent 1100 degrees C cyclic oxidation tests was inversely related to residual sulfur content. Control of adhesion by desulfurization in the absence of reactive elements supports an adhesion mechanism based on oxide-metal bonding weakened by sulfur segregation. Attempts at sulfur purging and improving adhesion by repeated oxidation/polishing were not successful, in contrast to previous studies on NiCrAl. C1 CASE WESTERN RESERVE UNIV,CLEVELAND,OH. RP SMIALEK, JL (reprint author), NASA,LEWIS RES CTR,CLEVELAND,OH 44135, USA. NR 21 TC 43 Z9 43 U1 0 U2 3 PU MINERALS METALS MATERIALS SOC PI WARRENDALE PA 420 COMMONWEALTH DR, WARRENDALE, PA 15086 SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD FEB PY 1995 VL 26 IS 2 BP 427 EP 435 DI 10.1007/BF02664679 PG 9 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA QC367 UT WOS:A1995QC36700018 ER PT J AU TEWARI, SN ASTHANA, R TIWARI, R BOWMAN, RR SMITH, J AF TEWARI, SN ASTHANA, R TIWARI, R BOWMAN, RR SMITH, J TI INFLUENCE OF INTERFACIAL REACTIONS ON THE FIBER-MATRIX INTERFACIAL SHEAR-STRENGTH IN SAPPHIRE FIBER-REINFORCED NIAL(YB) COMPOSITES SO METALLURGICAL AND MATERIALS TRANSACTIONS A-PHYSICAL METALLURGY AND MATERIALS SCIENCE LA English DT Article ID ALLOYS AB The influence of microstructure of the fiber-matrix interface on the interfacial shear strength, measured using a fiber-pushout technique, has been examined in a sapphire-fiber-reinforced NiAl(Yb) matrix composite under the following conditions: (1) as-fabricated powder metallurgy (PM) composites, (2) PM composites after solid-state heat treatment (HT), and (3) PM composites after directional solidification (DS). The fiber-pushout stress-displacement behavior consisted of an initial ''pseudoelastic'' region, wherein the stress increased linearly with displacement, followed by an ''inelastic'' region, where the slope of the stress-displacement plot decreased until a maximum stress was reached, and the subsequent gradual stress decreased to a ''frictional'' stress. Energy-dispersive spectroscopy (EDS) and X-ray analyses showed that the interfacial region in the PM NiAl(Yb) composites was comprised of Yb2O3, O-rich NiAl and some spinel oxide (Yb3Al5O12), whereas the interfacial region in the HT and DS composites was comprised mainly of Yb3Al5O12. A reaction mechanism has been proposed to explain the presence of interfacial species observed in the sapphire-NiAl(Yb) composite. The extent of inter facial chemical reactions and severity of fiber surface degradation increased progressively in this order: PM < HT < DS. Chemical interactions between the fiber and the NiAl(Yb) matrix resulted in chemical bonding and higher interfacial shear strength compared to sapphire-NiAl composites without Yb. Unlike the sapphire-NiAl system, the frictional shear stress in the sapphire-NiAl(Yb) composites was strongly dependent on the processing conditions. C1 NASA,LEWIS RES CTR,DIV MAT,CLEVELAND,OH 44135. NASA,LEWIS RES CTR,INTERMETALL BRANCH,CLEVELAND,OH 44135. RP TEWARI, SN (reprint author), CLEVELAND STATE UNIV,DEPT CHEM ENGN,CLEVELAND,OH 44115, USA. NR 18 TC 16 Z9 16 U1 0 U2 2 PU MINERALS METALS MATERIALS SOC PI WARRENDALE PA 420 COMMONWEALTH DR, WARRENDALE, PA 15086 SN 1073-5623 J9 METALL MATER TRANS A JI Metall. Mater. Trans. A-Phys. Metall. Mater. Sci. PD FEB PY 1995 VL 26 IS 2 BP 477 EP 491 DI 10.1007/BF02664684 PG 15 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA QC367 UT WOS:A1995QC36700023 ER PT J AU WANG, CY AHUJA, S BECKERMANN, C DEGROH, HC AF WANG, CY AHUJA, S BECKERMANN, C DEGROH, HC TI MULTIPARTICLE INTERFACIAL DRAG IN EQUIAXED SOLIDIFICATION SO METALLURGICAL AND MATERIALS TRANSACTIONS B-PROCESS METALLURGY AND MATERIALS PROCESSING SCIENCE LA English DT Article ID TRANSPORT PHENOMENA; POROUS PARTICLES; FLOW; MODEL; LIQUID; SEDIMENTATION; COLUMNAR; SYSTEMS; RATES AB A physical model is proposed for the solid/liquid interfacial drag in both globular and dendritic equiaxed solidification. By accounting for the presence of multiple particles and the nonsphericity and porosity of the individual equiaxed crystals, a drag correlation is developed, which is valid over the full range of solid volume fractions. It is shown that neither the solid liquid interfacial area concentration nor the grain size alone is adequate to characterize the interfacial drag for equiaxed dendritic crystals in both the free particle and packed bed regimes; thus, the present model is based on a multiple length scale approach. The model predictions are compared to previous analytical and numerical results as well as to experimental data available in the literature, and favorable agreement is achieved. C1 ENGN MECH RES CORP, TROY, MI 48098 USA. NASA, LEWIS RES CTR, CLEVELAND, OH 44135 USA. RP WANG, CY (reprint author), UNIV IOWA, DEPT ENGN MECH, IOWA CITY, IA 52242 USA. RI Wang, Chao-Yang/C-4122-2009; Beckermann, Christoph/F-7158-2010 OI Beckermann, Christoph/0000-0002-9976-0995 NR 29 TC 73 Z9 77 U1 1 U2 10 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1073-5615 J9 METALL MATER TRANS B JI Metall. Mater. Trans. B-Proc. Metall. Mater. Proc. Sci. PD FEB PY 1995 VL 26 IS 1 BP 111 EP 119 DI 10.1007/BF02648984 PG 9 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA QD551 UT WOS:A1995QD55100013 ER PT J AU TRINH, EH DEPEW, J AF TRINH, EH DEPEW, J TI SOLID-SURFACE WETTING AND THE DEPLOYMENT OF DROPS IN MICROGRAVITY SO MICROGRAVITY SCIENCE AND TECHNOLOGY LA English DT Article AB The complete or partial deployment of liquid samples in low gravity is primarily influenced by the interfacial properties of the specific liquid and solid materials used because the overwhelming bins of the Earth gravitational acceleration is removed. This study addresses the engineering aspects of injecting and deploying drops of prescribed volume into an acoustic positioning chamber in microgravity. The specific problems of interest are the design, testing, and implementation of injector tips to be used in a simultaneously retracting dual-injector system in the Drop Physics Module microgravity experiment facility. Prior to release, the liquid to be deployed must be retained within a restricted area at the very end of the injectors under dynamic stimuli from the continuous injection flow as well as from the stepped motion of the injectors. The final released drop must have a well determined volume and negligible residual linear or angular momentum. The outcome of Earth-based short-duration low gravity experiments had been the selection of two types of injector tips which were flown as back-up parts. They were successfully utilized during the USML-1 Spacelab mission as the primary tips. The combination of a larger contact surface, liquid pinning with a sharp edge, and selective coating of strategic tip surfaces with a non-wetting compound has allowed a significant increase in the success rate of deployment of simple and compound drops of aqueous solutions of glycerol and silicone oil. The diameter of the samples studied in the Drop Physics Module range between 0.3 and 2.7 cm. The tests conducted on-orbit with a manually operated small device have allowed the calibration of the volume deployed for a few drop sizes. The design for improved tips to be used during the next USML flight is based on these results. RP TRINH, EH (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 4 TC 1 Z9 1 U1 0 U2 0 PU CARL HANSER VERLAG PI MUNICH PA KOLBERGERSTRASSE 22, POSTFACH 860420, W-8163 MUNICH, GERMANY SN 0938-0108 J9 MICROGRAVITY SCI TEC JI Microgravity Sci. Technol. PD FEB PY 1995 VL 7 IS 4 BP 299 EP 306 PG 8 WC Engineering, Aerospace; Thermodynamics; Mechanics SC Engineering; Thermodynamics; Mechanics GA QH175 UT WOS:A1995QH17500007 ER PT J AU SONNENFELD, G KOEBEL, DA DAVIS, S AF SONNENFELD, G KOEBEL, DA DAVIS, S TI EFFECTS OF HYPERGRAVITY ON IMMUNOLOGICAL FUNCTION SO MICROGRAVITY SCIENCE AND TECHNOLOGY LA English DT Article ID EXPERIMENT PROGRAM INTERFERON; SPACE-FLIGHT; SPACEFLIGHT; SHUTTLE; RATS AB The purpose of this study was to compare the effects of hypergravity exposure (2 g) with those of exposure to space flight in the Cosmos 2044 flight. To do so, rats were centrifuged continuously for 14 days. Two different experiments were carried out on tissue obtained from the centrifuged rats. In the first experiment, rat bone marrow cells were examined for their response to recombinant murine colony stimulating factor-granulocyte/monocyte (GM-CSF). In the second experiment, rat spleen and bone marrow cells were stained in with a variety of antibodies directed against cell surface antigenic markets. These cells were preserved and analyzed on a flow cytometer. The results of the studies indicated that bone marrow cells from centrifuged rats showed no significant change in response to GM-CSF as compared to bone marrow cells from control rats. Spleen cells from flown rats showed some statistically significant changes in leukocytes subset distribution, but no differences that appeared to be of biological significance. These results indicate that hypergravity did not greatly affect the same immunological parameters affected by space flight in the Cosmos 2044 mission. C1 UNIV LOUISVILLE,SCH MED,DEPT MICROBIOL & IMMUNOL,LOUISVILLE,KY 40292. UNIV LOUISVILLE,SCH DENT,LOUISVILLE,KY 40292. NASA,AMES RES CTR,DIV LIFE SCI,MOFFETT FIELD,CA 94035. RP SONNENFELD, G (reprint author), CAROLINAS MED CTR,DEPT GEN SURG,POB 32861,CHARLOTTE,NC 28232, USA. NR 21 TC 4 Z9 4 U1 0 U2 1 PU CARL HANSER VERLAG PI MUNICH PA KOLBERGERSTRASSE 22, POSTFACH 860420, W-8163 MUNICH, GERMANY SN 0938-0108 J9 MICROGRAVITY SCI TEC JI Microgravity Sci. Technol. PD FEB PY 1995 VL 7 IS 4 BP 323 EP 326 PG 4 WC Engineering, Aerospace; Thermodynamics; Mechanics SC Engineering; Thermodynamics; Mechanics GA QH175 UT WOS:A1995QH17500010 PM 11538782 ER PT J AU NOEVER, DA NIKORA, VI AF NOEVER, DA NIKORA, VI TI RAREFIED SOLIDS SO MICROGRAVITY SCIENCE AND TECHNOLOGY LA English DT Note AB One important limit to creating low density materials is the objects' own weight. As a solid or colloidal matrix becomes more rarefied, gravity acts destructively to compress its supporting skeleton. We describe experimental results and propose a model which matches the low gravity behavior of rarefied or fractal solids. On parabolic airplane flights, we sought to demonstrate a key component of producing higher surface area fractals. Flight paths were selected to give a range of gravity levels: 0.01 g/g(0) (low), 0.16 g/g(0) (Lunar), 0.33 g/g(0) (Martian), 1 g/g(0), (Earth) and 1.8 g/g(0) (high) (where g(0) = 980 cm s(-2)). Results using the model material of hydrophobic silica indicated that stable agglomeration of such tenuous objects can increase markedly in reduced gravity. Optical characterization revealed that fractal dimension changed directly with varying gravity. As measured by fractal dimension, effective surface area and roughness increased by 40 % in low gravity. This finding supports the conclusion that relieving internal weight stresses on delicate aggregates can enhance their overall size (by two orders of magnitude) and internal surface area. We conclude that gravitational restructuring limits the overall size and void content of low-density solids. These sparse colloidal regimes may present new and technologically attractive physics, ranging from improved insulators, liquid-like surface tension in a ''solid'' matrix, and characteristically low conductivities for sound and (8 to 14 mu m wavelength) infrared radiation. C1 MOLDAVIAN ACAD SCI,INST GEOL & GEOPHYS,KISHINEV,MOLDOVA. RP NOEVER, DA (reprint author), NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,MAIL CODE ES-76,HUNTSVILLE,AL 35812, USA. NR 31 TC 0 Z9 0 U1 0 U2 0 PU CARL HANSER VERLAG PI MUNICH PA KOLBERGERSTRASSE 22, POSTFACH 860420, W-8163 MUNICH, GERMANY SN 0938-0108 J9 MICROGRAVITY SCI TEC JI Microgravity Sci. Technol. PD FEB PY 1995 VL 7 IS 4 BP 343 EP 347 PG 5 WC Engineering, Aerospace; Thermodynamics; Mechanics SC Engineering; Thermodynamics; Mechanics GA QH175 UT WOS:A1995QH17500014 ER PT J AU SCOVILLE, N BAJGAR, C ROLFE, J FLEURIAL, JP VANDERSANDE, J AF SCOVILLE, N BAJGAR, C ROLFE, J FLEURIAL, JP VANDERSANDE, J TI THERMAL-CONDUCTIVITY REDUCTION IN SIGE ALLOYS BY THE ADDITION OF NANOPHASE PARTICLES SO NANOSTRUCTURED MATERIALS LA English DT Article; Proceedings Paper CT Special MRS Symposium on Molecularly Designed Ultrafine Nanostructured Materials CY APR, 1994 CL SAN FRANCISCO, CA AB Transport models have predicted that the thermal conductivity of SiGe alloys could be appreciably reduced by incorporating discrete 40 Angstrom particles within the SiGe grains. These particles would scatter the thermal phonons which transport most of the heal in these alloys. Such a thermal conductivity reduction would lead to substantial improvements in the figure-of-merit and efficiency of thermoelectric materials used in power generation applications. This paper reports on the results of adding 40 Angstrom particles to SiGe by using a spark erosion process. Thermal conductivity reductions consistent with the transport models have been achieved; however, the improvement in figure-of-merit has not been as large as predicted. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. RP SCOVILLE, N (reprint author), THERMOTREX CORP,74 WEST ST,WALTHAM,MA 02254, USA. NR 6 TC 31 Z9 36 U1 0 U2 20 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0965-9773 J9 NANOSTRUCT MATER JI Nanostruct. Mater. PD FEB PY 1995 VL 5 IS 2 BP 207 EP 223 DI 10.1016/0965-9773(95)00018-6 PG 17 WC Materials Science, Multidisciplinary SC Materials Science GA QW482 UT WOS:A1995QW48200010 ER PT J AU CANE, HV AF CANE, HV TI THE STRUCTURE AND EVOLUTION OF INTERPLANETARY SHOCKS AND THE RELEVANCE FOR PARTICLE-ACCELERATION SO NUCLEAR PHYSICS B LA English DT Article; Proceedings Paper CT 14th European Cosmic Ray Symposium (14th ECRS) - Cosmic Rays 94: Solar, Heliospheric, Astrophysical and High-Energy Aspects CY AUG 28-SEP 03, 1994 CL BALATONFURED, HUNGARY SP HUNGARIAN ACAD SCI, KFKI RES INST PARTICLE & NUCL PHYS, SPACE PHYS DEPT, INT UNION PURE & APPL PHYS, COSM RAY COMM ID CORONAL MASS EJECTIONS; SOLAR FILAMENT ERUPTIONS; ENERGETIC PARTICLES; EVENTS; WIND; SPACECRAFT AB It is now widely accepted that interplanetary shocks initiated by coronal mass ejections play a dominant role in the generation of the vast majority of large solar energetic particle events. However, our understanding of the details of the acceleration process is far from complete. It is important to better understand the large-scale properties of shocks and how these properties change with distance from the Sun. In this paper I summarize shock and particle observations and. indicate where the problems lie. C1 UNIV TASMANIA,DEPT PHYS,HOBART,TAS 7001,AUSTRALIA. RP CANE, HV (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. NR 39 TC 22 Z9 22 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 FEB PY 1995 SU 39A BP 35 EP 44 DI 10.1016/0920-5632(95)00005-T PG 10 WC Physics, Particles & Fields SC Physics GA QN132 UT WOS:A1995QN13200005 ER PT J AU SCHAEFFER, JC MURPHY, WH SMIALEK, JL AF SCHAEFFER, JC MURPHY, WH SMIALEK, JL TI THE EFFECT OF SURFACE CONDITION AND SULFUR ON THE ENVIRONMENTAL RESISTANCE OF AIRFOILS SO OXIDATION OF METALS LA English DT Article DE TURBINE AIRFOILS; GLOW DISCHARGE MASS SPECTROSCOPY (GDMS); CYCLIC OXIDATION; YTTRIUM; TYPE-I HOT CORROSION; SULFUR; DESULFURIZATION; H-2 ANNEALING, CAST SURFACE ID ADHERENCE; ALLOYS; ADDITIONS; MECHANISM; ELEMENTS AB The environmental protection of aircraft engine high-pressure turbine blades is dependent upon the formation of a thin, slow-growing, external alumina scale. The adherence of alumina (Al2O3) scales to superalloys or coatings has been shown to be improved by adding an oxygen-active element (Y) or by desulfurization. Studies will be presented that show that cast surfaces are contaminated with sulfur and are more susceptible to high-velocity oxidation than machined surfaces regardless of an oxygen-active-element addition. In addition, the positive effect of oxygen-active elements and desulfurization on the performance of a single-crystal and directionally solidified Ni-base super-alloy in a 1149 degrees C cyclic oxidation test and a 927 degrees C/5 ppm sea-salt Type-I hot-corrosion test will be discussed. C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. RP SCHAEFFER, JC (reprint author), GE AIRCRAFT ENGINES,ENGN MAT TECHNOL LAB,CINCINNATI,OH, USA. NR 20 TC 14 Z9 14 U1 1 U2 1 PU PLENUM PUBL CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0030-770X J9 OXID MET JI Oxid. Met. PD FEB PY 1995 VL 43 IS 1-2 BP 1 EP 23 DI 10.1007/BF01046745 PG 23 WC Metallurgy & Metallurgical Engineering SC Metallurgy & Metallurgical Engineering GA QH287 UT WOS:A1995QH28700001 ER PT J AU BREHM, EW GOETTGE, RT MCCALEB, FW AF BREHM, EW GOETTGE, RT MCCALEB, FW TI START ES - AN EXPERT-SYSTEM TOOL FOR SYSTEM PERFORMANCE AND RELIABILITY-ANALYSIS SO PERFORMANCE EVALUATION LA English DT Article DE EXPERT SYSTEM; KNOWLEDGE-BASED SYSTEM; PERFORMANCE MODELING; RELIABILITY MODELING AB This paper describes START/ES, an expert system based tool for performance and reliability analysis of complex computer systems. START/ES provides an iconic system design capture interface, which allows direct manipulation of system design attributes and facilitates the exploration of a wide range of design alternatives. System design descriptions are automatically translated into mathematical models, which evaluate candidate designs in terms of both performance and reliability. Evaluation results can be analyzed by the automated reasoning component of the tool, which uses a rule-based approach to diagnose performance and reliability problems, and to recommend design changes for achieving system designs which are compliant with all requirements. Finally, the rule base is extensible and can be modified using START/ES's rule builder interface. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP BREHM, EW (reprint author), ADV SYST TECHNOL INC,12200 E BRIARWOOD AVE,SUITE 260,ENGLEWOOD,CO 80112, USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0166-5316 J9 PERFORM EVALUATION JI Perform. Eval. PD FEB PY 1995 VL 22 IS 1 BP 43 EP 58 DI 10.1016/0166-5316(93)E0037-6 PG 16 WC Computer Science, Hardware & Architecture; Computer Science, Theory & Methods SC Computer Science GA QJ375 UT WOS:A1995QJ37500004 ER PT J AU HARDING, LW ITSWEIRE, EC ESAIAS, WE AF HARDING, LW ITSWEIRE, EC ESAIAS, WE TI ALGORITHM DEVELOPMENT FOR RECOVERING CHLOROPHYLL CONCENTRATIONS IN THE CHESAPEAKE BAY USING AIRCRAFT REMOTE-SENSING, 1989-91 SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article ID PHYTOPLANKTON; ESTUARIES; PATTERNS; DELAWARE AB A study using aircraft remote sensing of chlorophyll concentrations was conducted in the Chesapeake Bay from 1989 to 1991. The goal was to improve spatial and temporal resolution of the distribution of phytoplankton in this highly dynamic and variable estuary. The focus of the study was on improving our ability to estimate chlorophyll a [Chl a] from aircraft by developing local algorithms for individual years, and by exploring the use of seasonally and spatially specific algorithms. Our findings suggest that an overall, multi-year algorithm can be used predictively to estimate the distribution of Chl a i.e., the location, duration, and spatial extent of phytoplankton blooms - in near real time-. Refinements that improve the recovery of Chl a include the separation of spring data from the data for other seasons, and the use of separate local algorithms for regions of low and high turbidity. These developments improve the accuracy with which we recover Chl a in the Chesapeake Bay using aircraft remote sensing and have implications for the detection of changes in algal biomass that are expected to accompany nutrient reductions between now and the turn of the century. Our results suggest that the shipboard sampling of the Monitoring Program may underestimate the biomass of phytoplankton blooms and, hence, the amount of particulate carbon produced in the Bay. This finding has ramifications for detecting changes in phyloplankton abundance that are expected to accompany nutrient reductions, and for processes such as hypoxia (i.e., low oxygen concentrations) that are driven by organic material derived from the spring phytoplankton bloom in the mesohaline region of the Chesapeake Bay. C1 UNIV MARYLAND,HORN POINT ENVIRONM LABS,CAMBRIDGE,MD 21613. NATL SCI FDN,DIV OCEAN SCI,WASHINGTON,DC 20550. JOHNS HOPKINS UNIV,DEPT GEOG & ENVIRONM ENGN,BALTIMORE,MD 21218. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP HARDING, LW (reprint author), UNIV MARYLAND,SEA GRANT COLL,COLLEGE PK,MD 20742, USA. NR 17 TC 24 Z9 26 U1 1 U2 3 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD FEB PY 1995 VL 61 IS 2 BP 177 EP 185 PG 9 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA TB089 UT WOS:A1995TB08900007 ER PT J AU OMIDVAR, K MCALLISTER, AM AF OMIDVAR, K MCALLISTER, AM TI EVALUATION OF HIGH-LEVEL BOUND-BOUND AND BOUND-CONTINUUM HYDROGENIC OSCILLATOR-STRENGTHS BY ASYMPTOTIC-EXPANSION SO PHYSICAL REVIEW A LA English DT Article RP OMIDVAR, K (reprint author), NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771, USA. NR 10 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 FEB PY 1995 VL 51 IS 2 BP 1063 EP 1066 DI 10.1103/PhysRevA.51.1063 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA QH071 UT WOS:A1995QH07100031 ER PT J AU DERRICKSON, JH EBY, PB MOON, KH PARNELL, TA KING, DT GREGORY, JC TAKAHASHI, Y OGATA, T AF DERRICKSON, JH EBY, PB MOON, KH PARNELL, TA KING, DT GREGORY, JC TAKAHASHI, Y OGATA, T TI DIRECT PRODUCTION OF ELECTRON-POSITRON PAIRS BY 200-GEV/NUCLEON OXYGEN AND SULFUR IONS IN NUCLEAR-EMULSION SO PHYSICAL REVIEW A LA English DT Article ID RELATIVISTIC HEAVY-IONS; CROSS-SECTION; COLLISIONS C1 UNIV TENNESSEE,DEPT PHYS & ASTRON,KNOXVILLE,TN 37996. UNIV ALABAMA,COLL SCI,HUNTSVILLE,AL 35899. UNIV TOKYO,INST COSM RAY RES,TANASHI 188,TOKYO,JAPAN. RP DERRICKSON, JH (reprint author), NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB,HUNTSVILLE,AL 35812, USA. NR 46 TC 8 Z9 8 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 FEB PY 1995 VL 51 IS 2 BP 1253 EP 1259 DI 10.1103/PhysRevA.51.1253 PG 7 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA QH071 UT WOS:A1995QH07100052 ER PT J AU TRIPATHY, BC BROWN, CS AF TRIPATHY, BC BROWN, CS TI ROOT-SHOOT INTERACTION IN THE GREENING OF WHEAT SEEDLINGS CROWN UNDER RED-LIGHT SO PLANT PHYSIOLOGY LA English DT Article ID BLUE-LIGHT; CHLOROPHYLL BIOSYNTHESIS; CHLOROPLAST DEVELOPMENT; INDUCED PHOSPHORYLATION; PROTOPORPHYRIN-IX; MG-PROTOPORPHYRIN; QUALITY; PLANTS; PROTOCHLOROPHYLLIDE; TRANSDUCTION AB Wheat seedlings grown with roots exposed to constant red light (300-500 mu mol m(-2) s(-1)) did not accumulate chlorophyll in the leaves. In contrast, seedlings grown with their roots shielded from light accumulated chlorophylls. Chlorophyll biosynthesis could be induced in red-light-grown chlorophyll-deficient yellow plants by either reducing the red-light intensity at the root surface to 100 mu mol m(-2) s(-1) or supplementing with 6% blue light. The inhibition of chlorophyll biosynthesis was due to impairment of the Mg-chelatase enzyme working at the origin of the Mg-tetrapyrrole pathway. The root-perceived photomorphogenic inhibition of shoot greening demonstrates root-shoot interaction in the greening process. C1 DYNAMAC CORP,KENNEDY SPACE CTR,FL 32899. RP TRIPATHY, BC (reprint author), NASA,MAIL CODE MD RES,KENNEDY SPACE CTR,FL 32899, USA. NR 22 TC 58 Z9 71 U1 0 U2 3 PU AMER SOC PLANT PHYSIOLOGISTS PI ROCKVILLE PA 15501 MONONA DRIVE, ROCKVILLE, MD 20855 SN 0032-0889 J9 PLANT PHYSIOL JI Plant Physiol. PD FEB PY 1995 VL 107 IS 2 BP 407 EP 411 PG 5 WC Plant Sciences SC Plant Sciences GA QH872 UT WOS:A1995QH87200011 PM 11536685 ER PT J AU HECHT, H AF HECHT, H TI RETINAL, ATTENTIONAL, AND CAUSAL ASPECTS OF ILLUSORY-MOTION DIRECTIONALITY SO PSYCHOLOGICAL RESEARCH-PSYCHOLOGISCHE FORSCHUNG LA English DT Article ID PERCEPTION; SENSITIVITY; ALLOCATION; SENSATION; STIMULUS; CORTEX AB Extended objects presented instantaneously appeared to propagate or grow into their final shape. A strong bias was found toward perceiving straight lines to grow away from the observer's point of fixation. It attention and fixation were not directed to the same point of the visual field, both influenced illustory motion directionality, and if another small object was present on the screen at a location that was neither fixated nor attended to, the object that was instantaneously presented seemed to grow away from this point. Thus, three factors are involved in illustory-motion directionality: biases toward perceiving objects spreading away from the fixation point, away from an attended area, and away from preexisting objects. The experiments indicate that a satisfactory explanation of the illusion has to include bottom-up and top-down processes. They also challenge existing theories of motion detection. RP HECHT, H (reprint author), NASA,AMES RES CTR,MS 262-3,MOFFETT FIELD,CA 94035, USA. NR 26 TC 7 Z9 7 U1 0 U2 0 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0340-0727 J9 PSYCHOL RES-PSYCH FO JI Psychol. Res.-Psychol. Forsch. PD FEB PY 1995 VL 57 IS 2 BP 70 EP 79 PG 10 WC Psychology, Experimental SC Psychology GA QJ063 UT WOS:A1995QJ06300002 PM 7708899 ER PT J AU WALBORN, NR LENNON, DJ HASER, SM KUDRITZKI, RP VOELS, SA AF WALBORN, NR LENNON, DJ HASER, SM KUDRITZKI, RP VOELS, SA TI THE PHYSICS OF MASSIVE OB STARS IN DIFFERENT PARENT GALAXIES .1. ULTRAVIOLET AND OPTICAL SPECTRAL MORPHOLOGY IN THE MAGELLANIC CLOUDS SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID RADIATION DRIVEN WINDS; HOT LUMINOUS STARS; STELLAR WINDS; QUANTITATIVE SPECTROSCOPY; B-SUPERGIANTS; SMC; CLASSIFICATION; NGC-346; SK-159; REGION AB HST/FOS and ESO 3.6-m/CASPEC observations have been made of 18 stars ranging in spectral type from O3 through B0.5 Ia, half of them in each of the Large and Small Magellanic Clouds, in order to investigate massive stellar winds and evolution as a function of metallicity. The spectroscopic data are initially presented and described here in an atlas format. The relative weakness of the stellar-wind features in the SMC early OV spectra, due to their metal deficiency, is remarkable. Because of their unsaturated profiles, discrete absorption components can be detected in many of them, which is generally not possible in LMC and Galactic counterparts at such early types, or even in SMC giants and supergiants. On the other hand, an O3 III spectrum in the SMC has a weak C IV but strong N V wind profile, possibly indicating the presence of processed material. Wind terminal velocities are also given and intercompared between similar spectral types in the two galaxies. In general, the terminal velocities of the SMC stars are smaller, in qualitative agreement with the predictions of radiation-driven wind theory. Further analyses in progress will provide atmospheric and wind parameters for these stars, which will be relevant to evolutionary models and the interpretation of composite starburst spectra. C1 UNIV MUNICH,INST ASTRON & ASTROPHYS,D-81679 MUNICH,GERMANY. NASA,GODDARD SPACE FLIGHT CTR,ASTROPHYS DATA FACIL,GREENBELT,MD 20771. RP WALBORN, NR (reprint author), SPACE TELESCOPE SCI INST,3700 SAN MARTIN DR,BALTIMORE,MD 21218, USA. NR 49 TC 109 Z9 109 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 FEB PY 1995 VL 107 IS 708 BP 104 EP 119 DI 10.1086/133524 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QJ054 UT WOS:A1995QJ05400002 ER PT J AU HOLTZMAN, J HESTER, JJ CASERTANO, S TRAUGER, JT WATSON, AM BALLESTER, GE BURROWS, CJ CLARKE, JT CRISP, D EVANS, RW GALLAGHER, JS GRIFFITHS, RE HOESSEL, JG MATTHEWS, LD MOULD, JR SCOWEN, PA STAPELFELDT, KR WESTPHAL, JA AF HOLTZMAN, J HESTER, JJ CASERTANO, S TRAUGER, JT WATSON, AM BALLESTER, GE BURROWS, CJ CLARKE, JT CRISP, D EVANS, RW GALLAGHER, JS GRIFFITHS, RE HOESSEL, JG MATTHEWS, LD MOULD, JR SCOWEN, PA STAPELFELDT, KR WESTPHAL, JA TI THE PERFORMANCE AND CALIBRATION OF WFPC2 ON THE HUBBLE-SPACE-TELESCOPE SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID GROUND-BASED OBSERVATIONS; FIELD PLANETARY CAMERA; PHOTOMETRIC CALIBRATION AB The WFPC2 was installed in the Hubble Space Telescope (HST) in 1993 December, Since then, the instrument has been providing high-quality images. A significant amount of calibration data has been collected to aid in the understanding of the on-orbit performance of the instrument. Generally, the behavior of the camera is similar to its performance during the system-level thermal vacuum test at JPL in 1993 May. Surprises were a significant charge-transfer-efficiency (CTE) problem and a significant growth rate in hot pixels at the original operating temperature of the CCDs (-76 degrees C), The operating temperature of the WFPC2 CCDs was changed to -88 degrees C on 1994 April 23, and significant improvements in CTE and hot pixels are seen at this temperature. In this paper we describe the on-orbit performance of the WFPC2. We discuss the optical and thermal history, the instrument throughput and stability, the PSE the effects of undersampling on photometry, the properties of cosmic rays observed on-orbit, and the geometric distortion in the camera. We present the best techniques for the reduction of WFPC2 data, and describe the construction of calibration products including superbiases, superdarks, and flat fields. C1 ARIZONA STATE UNIV,DEPT PHYS & ASTRON,TEMPE,AZ 85287. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. CALTECH,JET PROP LAB,PASADENA,CA 91109. UNIV MICHIGAN,DEPT ATMOSPHER OCEAN & SPACE SCI,ANN ARBOR,MI 48109. UNIV WISCONSIN,DEPT ASTRON,MADISON,WI 53706. JOHNS HOPKINS UNIV,DEPT ASTRON,BALTIMORE,MD 21218. SUNY STONY BROOK,ASTRON PROGRAM,STONY BROOK,NY 11794. AUSTRALIAN NATL UNIV,MT STROMLO & SIDING SPRING OBSERV,WESTON,ACT 2611,AUSTRALIA. CALTECH,DIV GEOL & PLANETARY SCI,PASADENA,CA 91125. RP HOLTZMAN, J (reprint author), LOWELL OBSERV,1400 W MARS HILL RD,FLAGSTAFF,AZ 86001, USA. RI Stapelfeldt, Karl/D-2721-2012; Clarke, John/C-8644-2013 NR 8 TC 430 Z9 433 U1 1 U2 7 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 FEB PY 1995 VL 107 IS 708 BP 156 EP 178 DI 10.1086/133533 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QJ054 UT WOS:A1995QJ05400011 ER PT J AU CHOUDHURY, BJ DORMAN, TJ HSU, AY AF CHOUDHURY, BJ DORMAN, TJ HSU, AY TI MODELED AND OBSERVED RELATIONS BETWEEN THE AVHRR SPLIT WINDOW TEMPERATURE DIFFERENCE AND ATMOSPHERIC PRECIPITABLE WATER OVER LAND SURFACES SO REMOTE SENSING OF ENVIRONMENT LA English DT Article ID HIGH-RESOLUTION RADIOMETER; SATELLITE; VAPOR; EMISSIVITY; CHANNELS AB Atmospheric correction to near-infrared reflectances for land surface studies requires information about precipitable water. A relation between the split window temperature difference (Delta T) and atmosphere precipitable water (W) over land surfaces is developed from the radiative transfer equation considering spectral variation of the emissivity. This relation is found to be essentially linear with slope and intercept being dependent on the emissivity. The observed Delta T (from NOAA-9 AVHRR data for 10.1-11.5 mu m and 11.2-12.6 mu m channels) and W (from radiosonde data) for 1 year (1988) at 24 globally distributed locations of various surface types (hot and temperate deserts, savannas, temperature deciduous forest, rainforest, boreal forest, etc.) were analyzed to assess the relation between Delta T and W and compared with the theoretical results. These globally distributed data were segregated into specified ranges of visible reflectance (from the AVHRR corresponding to Delta T data) so as to minimize emissivity variations in determining the slope and the intercept of the Delta T-W relationship and in estimating emissivity. Both the theory and the observations demonstrate the feasibility of estimating W from Delta T over vegetated surfaces, although a priori knowledge of emissivity will be needed for a wider application. C1 SCI SYST & APPLICAT INC,LANHAM,MD. RP CHOUDHURY, BJ (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HYDROL SCI BRANCH,CODE 974,GREENBELT,MD 20771, USA. NR 29 TC 24 Z9 25 U1 0 U2 2 PU ELSEVIER SCIENCE PUBL CO INC PI NEW YORK PA 655 AVENUE OF THE AMERICAS, NEW YORK, NY 10010 SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD FEB PY 1995 VL 51 IS 2 BP 281 EP 290 DI 10.1016/0034-4257(94)00087-4 PG 10 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA QM842 UT WOS:A1995QM84200005 ER PT J AU HANAN, NP PRINCE, SD HOLBEN, BN AF HANAN, NP PRINCE, SD HOLBEN, BN TI ATMOSPHERIC CORRECTION OF AVHRR DATA FOR BIOPHYSICAL REMOTE-SENSING OF THE SAHEL SO REMOTE SENSING OF ENVIRONMENT LA English DT Article ID AEROSOL OPTICAL-THICKNESS; NEAR-IR BANDS; SOLAR-RADIATION; CORN CANOPIES; WATER-VAPOR; REFLECTANCE; MODEL; VARIABILITY; SCATTERING; REGION AB The importance of atmospheric correction of reflectances measured with the Advanced Very High Resolution Radiometer (AVHRR) for biophysical studies using the normalized difference vegetation index (NDVI) is examined for a study area in the Sahel for which measurements of aerosol and water vapor were available. During the rainy season atmospheric aerosols were relatively more variable than water vapor. Atmospheric corrections were applied to Channel 1 (red) and Channel 2 (near-infrared) for the effects of molecular absorption and Rayleigh scatter, aerosol scatter and absorption, and water vapor absorption. The results were expressed as the difference between corrected and uncorrected reflectances (Delta rho). In Channel 1 the magnitude and variability of Delta rho was mostly caused by aerosols. In Channel 2 the magnitude of Delta rho was caused by water vapor, but most of the variability was caused by aerosols. Most of the degradation in the NDVI signal (Delta nu iota) was caused by water vapor but the variability in Delta nu iota was caused by both water vapor and aerosol. Atmospheric corrections using seasonal averages of atmospheric water vapor and aerosol optical depths resulted in corrections that were similar to the full corrections using daily values. In the Sahel it may therefore be acceptable to use average values for the atmospheric variables to correct satellite data when sunphotometer data are not available, although the effects of interannual variability in mean atmospheric conditions are not known. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP HANAN, NP (reprint author), UNIV MARYLAND,DEPT GEOGRAPHY,GLOBAL REMOTE SENSING STUDIES LAB,COLLEGE PK,MD 20742, USA. OI Hanan, Niall/0000-0002-9130-5306 NR 42 TC 13 Z9 13 U1 0 U2 1 PU ELSEVIER SCIENCE PUBL CO INC PI NEW YORK PA 655 AVENUE OF THE AMERICAS, NEW YORK, NY 10010 SN 0034-4257 J9 REMOTE SENS ENVIRON JI Remote Sens. Environ. PD FEB PY 1995 VL 51 IS 2 BP 306 EP 316 DI 10.1016/0034-4257(94)00099-9 PG 11 WC Environmental Sciences; Remote Sensing; Imaging Science & Photographic Technology SC Environmental Sciences & Ecology; Remote Sensing; Imaging Science & Photographic Technology GA QM842 UT WOS:A1995QM84200007 ER PT J AU COSTA, ME BLAIR, DG BUCKINGHAM, MJ SINCLAIR, MW FERRIS, RH JAUNCEY, DL REYNOLDS, JE TZIOUMIS, AK PRESTON, RA AF COSTA, ME BLAIR, DG BUCKINGHAM, MJ SINCLAIR, MW FERRIS, RH JAUNCEY, DL REYNOLDS, JE TZIOUMIS, AK PRESTON, RA TI APPLICATION OF COMMERCIAL ANTENNAS TO VERY LONG-BASE-LINE INTERFEROMETRY RADIO ASTRONOMY SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article C1 AUSTRALIA TELESCOPE NATL FACIL,EPPING,NSW 2121,AUSTRALIA. CALTECH,JET PROP LAB,PASADENA,CA 91109. RP COSTA, ME (reprint author), UNIV WESTERN AUSTRALIA,DEPT PHYS,NEDLANDS,WA 6009,AUSTRALIA. NR 7 TC 2 Z9 2 U1 0 U2 0 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD FEB PY 1995 VL 66 IS 2 BP 995 EP 999 DI 10.1063/1.1145634 PN 1 PG 5 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA QK980 UT WOS:A1995QK98000007 ER PT J AU DUBICK, MA DAVIS, JM MYERS, T WADE, CE KRAMER, GC AF DUBICK, MA DAVIS, JM MYERS, T WADE, CE KRAMER, GC TI DOSE-RESPONSE EFFECTS OF HYPERTONIC SALINE AND DEXTRAN ON CARDIOVASCULAR-RESPONSES AND PLASMA-VOLUME EXPANSION IN SHEEP SO SHOCK LA English DT Article ID 7.5-PERCENT NACL/6-PERCENT DEXTRAN-70; SEVERE HEMORRHAGIC-SHOCK; 6-PERCENT DEXTRAN-70; PLATELET-AGGREGATION; CONSCIOUS SWINE; BLOOD-FLOW; RESUSCITATION; NACL; DOGS; COAGULATION AB Despite the established efficacy of 7.5% NaCl/6% dextran-70 in the treatment of hypovolemia, the optimal formulation of a hyperosmotic/hyperoncotic small volume resuscitation solution has yet to be defined. The present study investigates the cardiovascular effects of hypertonic saline ranging from 3.75%-25% NaCl (HS) and dextran-70 (D-70) ranging from 3 to 24%. HS and D-70 were studied alone or in specific combinations at a dose of 4 mL/kg, in euvolemic sheep. Blood samples were collected before, during and up to 60 min after infusion of the test solutions. Dose-dependent effects of HS were immediate increases in cardiac output (GO) of 30-85%, falling to 10-35% over baseline after 60 min. HS concentrations over 3.75% significantly reduced systemic vascular resistance, but HS had no significant effect on mean arterial pressure (MAP). Plasma volume (PV) expansion with HS was an immediate, but transient increase of 12-35%. Infusion of D-70 induced sustained 10-20% increases in CO and 10-30% increases in PV, peaking 10 min post-infusion, D-70 also resulted in small (5-12 mmHg) increases in MAP. Cardiovascular effects of D-70 correlated with a dose-dependent increase in plasma dextran concentrations. All HS solutions significantly increased plasma Na, which peaked at greater than or equal to 200 mEq/L in the 25% group, The effects of D-70 and HS combined were additive on PV expansion and CO. These data indicate that concentrations of HS and D-70 which are higher than those currently used have a greater capability for expanding PV, but use of HS >7.5% may be limited by resulting hypernatremia. C1 LETTERMAN ARMY INST RES,DIV MIL TRAUMA RES,SAN FRANCISCO,CA 94129. UNIV CALIF DAVIS,DEPT NUTR,DAVIS,CA 95616. UNIV CALIF DAVIS,DEPT SURG,DAVIS,CA 95616. UNIV TEXAS,MED BRANCH,DEPT ANESTHESIOL,GALVESTON,TX 77550. UNIV TEXAS,MED BRANCH,DEPT PHYSIOL,GALVESTON,TX 77550. NASA,AMES RES CTR,DIV LIFE SCI,MOFFETT FIELD,CA 94035. NR 34 TC 23 Z9 25 U1 0 U2 0 PU BIOMEDICAL PRESS PI AUGUSTA PA 1021 15TH ST, BIOTECH PARK STE 9, AUGUSTA, GA 30901 SN 1073-2322 J9 SHOCK JI Shock PD FEB PY 1995 VL 3 IS 2 BP 137 EP 144 DI 10.1097/00024382-199502000-00009 PG 8 WC Critical Care Medicine; Hematology; Surgery; Peripheral Vascular Disease SC General & Internal Medicine; Hematology; Surgery; Cardiovascular System & Cardiology GA QG636 UT WOS:A1995QG63600009 PM 7538433 ER PT J AU ACUNA, MH OGILVIE, KW BAKER, DN CURTIS, SA FAIRFIELD, DH MISH, WH AF ACUNA, MH OGILVIE, KW BAKER, DN CURTIS, SA FAIRFIELD, DH MISH, WH TI THE GLOBAL GEOSPACE SCIENCE PROGRAM AND ITS INVESTIGATIONS SO SPACE SCIENCE REVIEWS LA English DT Review AB The detailed study of the solar-terrestrial energy chain will be greatly enhanced with the launch and simultaneous operation of several spacecraft during the current decade. These programs are being coordinates in the United States under the umbrella of the International Solar Terrestrial Physics Program (ISTP) and include fundamental contributions from Japan (GEOTAIL Program) and Europe (SOHO and CLUSTER Programs). The principal United States contribution to this effort is the Global Geospace Science Program (GGS) described in this overview paper. Two spacecraft, WIND and POLAR, carrying an advanced complement of field, particle and imaging instruments, will conduct investigations of several key regions of 'geospace'. This paper provides a general overview of the science objectives of the missions, the spacecraft orbits and the ground elements that have been developed to process and analyze the instrument observations. RP ACUNA, MH (reprint author), NASA,GODDARD SPACE FLIGHT CTR,EXTRATERR PHYS LAB,GREENBELT,MD 20771, USA. NR 14 TC 156 Z9 156 U1 0 U2 2 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 5 EP 21 DI 10.1007/BF00751323 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100002 ER PT J AU WHIPPLE, E LANCASTER, H AF WHIPPLE, E LANCASTER, H TI INTERNATIONAL COORDINATION OF SOLAR-TERRESTRIAL SCIENCE SO SPACE SCIENCE REVIEWS LA English DT Review AB A broad, international, cooperative effort is under way to study and develop quantitative understanding of the fundamental electrodynamic processes in the solar-terrestrial environment. Japan, Europe, Russia, the United States, and other countries are providing spacecraft to be placed in key regions with the aim of utilizing coordinated, multipoint spaceflight measurements, groundbased observations, and theory to study the global energy budget of geospace. The U.S. contribution began in the late 1970's as the OPEN program (Origin of Plasmas in Earth's Neighborhood) and was reconstituted in the 1980's as the Global Geospace Science (GGS) program. The international effort, known in the U.S. as the International Solar Terrestrial Physics program (ISTP), began with the launch of the Japanese GEOTAIL in 1992, and will continue with the U.S. spacecraft WIND and POLAR in 1994-1995, and the European four-spacecraft Cluster fleet and its Solar and Heliospheric Observatory (SOHO) in 1995. Russia will launch its Interball set of four spacecraft in 1995. The Inter-Agency Consultative Group (IACG) is promoting the coordination of the spacecraft observations by means of scientific campaigns aimed at addressing scientific questions that can only be answered by observations from the multiple spacecraft. The Solar Terrestrial Energy Program (STEP) is coordinating the involvement of the broad scientific community and especially the correlative ground observations. C1 NASA HEADQUARTERS,WASHINGTON,DC 20546. SCI APPLICAT INT CORP,WASHINGTON,DC 20024. NR 14 TC 2 Z9 2 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 41 EP 54 DI 10.1007/BF00751325 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100004 ER PT J AU OGILVIE, KW CHORNAY, DJ FRITZENREITER, RJ HUNSAKER, F KELLER, J LOBELL, J MILLER, G SCUDDER, JD SITTLER, EC TORBERT, RB BODET, D NEEDELL, G LAZARUS, AJ STEINBERG, JT TAPPAN, JH AF OGILVIE, KW CHORNAY, DJ FRITZENREITER, RJ HUNSAKER, F KELLER, J LOBELL, J MILLER, G SCUDDER, JD SITTLER, EC TORBERT, RB BODET, D NEEDELL, G LAZARUS, AJ STEINBERG, JT TAPPAN, JH TI SWE, A COMPREHENSIVE PLASMA INSTRUMENT FOR THE WIND SPACECRAFT SO SPACE SCIENCE REVIEWS LA English DT Review ID GLOBAL PROCESSES; ELECTRONS AB The Solar Wind Experiment (SWE) on the WIND spacecraft is a comprehensive, integrated set of sensors which is designed to investigate outstanding problems in solar wind physics. It consists of two Faraday cup (FC) sensors; a vector electron and ion spectrometer (VEIS); a strahl sensor, which is especially configured to study the electron 'strahl' close to the magnetic field direction; and an on-board calibration system. The energy/charge range of the Faraday cups is 150 V to 8 kV, and that of the VEIS is 7 V to 24.8 kV. The time resolution depends on the operational mode used, but can be of the order of a few seconds for 3-D measurements. 'Key parameters' which broadly characterize the solar wind positive ion velocity distribution function will be made available rapidly from the GGS Central Data Handling Facility. C1 UNIV NEW HAMPSHIRE,INST STUDY EARTH OCEANS & SPACE,DEPT PHYS,DURHAM,NH 03284. UNIV NEW HAMPSHIRE,INST STUDY EARTH OCEANS & SPACE,CTR SPACE SCI,DURHAM,NH 03284. MIT,CTR SPACE RES,CAMBRIDGE,MA 02139. BOSTON UNIV,MICROELECTR RES LAB,BOSTON,MA 02215. RP OGILVIE, KW (reprint author), NASA,GODDARD SPACE FLIGHT CTR,INTERPLANTARY PHYS BRANCH,GREENBELT,MD 20771, USA. RI Scudder, Jack/D-8417-2013; Keller, John/I-5097-2013 OI Scudder, Jack/0000-0001-7975-5630; NR 10 TC 637 Z9 638 U1 4 U2 14 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 55 EP 77 DI 10.1007/BF00751326 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100005 ER PT J AU GLOECKLER, G BALSIGER, H BURGI, A BOCHSLER, P FISK, LA GALVIN, AB GEISS, J GLIEM, F HAMILTON, DC HOLZER, TE HOVESTADT, D IPAVICH, FM KIRSCH, E LUNDGREN, RA OGILVIE, KW SHELDON, RB WILKEN, B AF GLOECKLER, G BALSIGER, H BURGI, A BOCHSLER, P FISK, LA GALVIN, AB GEISS, J GLIEM, F HAMILTON, DC HOLZER, TE HOVESTADT, D IPAVICH, FM KIRSCH, E LUNDGREN, RA OGILVIE, KW SHELDON, RB WILKEN, B TI THE SOLAR-WIND AND SUPRATHERMAL ION COMPOSITION INVESTIGATION ON THE WIND SPACECRAFT SO SPACE SCIENCE REVIEWS LA English DT Review ID EARTHS BOW SHOCK; HEAVY-IONS; GIACOBINI-ZINNER; CHARGE STATES; ABUNDANCES; MAGNETOSPHERE; HELIOSPHERE; ENERGIES; UPSTREAM; NUCLEON AB The Solar Wind and Suprathermal Ion Composition Experiment (SMS) on WIND is designed to determine uniquely the elemental, isotopic, and ionic-charge composition of the solar wind, the temperatures and mean speeds of all major solar-wind ions, from H through Fe, at solar wind speeds ranging from 175 kms(-1) (protons) to 1280 kms(-1) (Fe+8), and the composition, charge states as well as the 3-dimensional distribution functions of suprathermal ions, including interstellar pick-up He+, of energies up to 230 keV/e. The experiment consists of three instruments with a common Data Processing Unit. Each of the three instruments uses electrostatic analysis followed by a time-of-flight and, as required, an energy measurement. The observations made by SMS will make valuable contributions to the ISTP objectives by providing information regarding the composition and energy distribution of matter entering the magnetosphere. In addition SMS results will have an impact on many areas of solar and heliospheric physics, in particular providing important and unique information on: (i) conditions and processes in the region of the corona where the solar wind is accelerated; (ii) the location of the source regions of the solar wind in the corona; (iii) coronal heating processes; (iv) the extent and causes of variations in the composition of the solar atmosphere; (v) plasma processes in the solar wind; (vi) the acceleration of particles in the solar wind; and (vii) the physics of the pick-up process of interstellar He as well as lunar particles in the solar wind, and the isotopic composition of interstellar helium. C1 UNIV BERN,INST PHYS,BERN,SWITZERLAND. UNIV MICHIGAN,DEPT ATMOSPHER OCEAN & SPACE SCI,ANN ARBOR,MI 48109. TECH UNIV CAROLO WILHELMINA BRAUNSCHWEIG,INST DATENVERARBEITUNGSANLAGEN,W-3300 BRAUNSCHWEIG,GERMANY. NATL CTR ATMOSPHER RES,HIGH ALTITUDE OBSERV,BOULDER,CO 80307. MAX PLANCK INST AERON,KATLENBURG DUHM,GERMANY. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP GLOECKLER, G (reprint author), UNIV MARYLAND,DEPT PHYS,COLLEGE PK,MD 20742, USA. RI Galvin, Antoinette/A-6114-2013; OI Hamilton, Douglas/0000-0001-6103-8019 NR 43 TC 59 Z9 60 U1 0 U2 3 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 79 EP 124 DI 10.1007/BF00751327 PG 46 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100006 ER PT J AU VONROSENVINGE, TT BARBIER, LM KARSCH, J LIBERMAN, R MADDEN, MP NOLAN, T REAMES, DV RYAN, L SINGH, S TREXEL, H WINKERT, G MASON, GM HAMILTON, DC WALPOLE, P AF VONROSENVINGE, TT BARBIER, LM KARSCH, J LIBERMAN, R MADDEN, MP NOLAN, T REAMES, DV RYAN, L SINGH, S TREXEL, H WINKERT, G MASON, GM HAMILTON, DC WALPOLE, P TI THE ENERGETIC PARTICLES - ACCELERATION, COMPOSITION, AND TRANSPORT (EPACT) INVESTIGATION ON THE WIND SPACECRAFT SO SPACE SCIENCE REVIEWS LA English DT Review ID FLARES AB The Energetic Particles: Acceleration, Composition, and Transport (EPACT) investigation is designed to make comprehensive observations of solar, interplanetary, and galactic particles over wide ranges of charge, mass, energy, and intensity using a combination of and different particle telescopes. This paper summarizes the scientific goals of EPACT and provides a detailed description of the instrument design and capabilities. Electrons are measured from 0.2 to 10 MeV, primarily providing time markers for injections of solar particles. Hydrogen is measured from 1.4 to 120 MeV, and Helium is measured from 0.04 to 500 MeV nucl(-1). The collection powers and energy ranges for heavier nuclei up to iron are ideal for observations of quiet-time populations such as particles accelerated by interplanetary shocks and the anomalous cosmic rays (thought to be accelerated at the boundary of the heliosphere). The large collection power available is also ideal for observations of He-3, He-4, and heavier nuclei in impulsive He-3-rich solar events. There is even the possibility of observing ultra heavy nuclei (Z > 30) in large solar events for the first time. Finally, there is a telescope designed to measure isotopes from He (3.4-55 MeV nucl(-1)) to Fe (12-230 MeV nucl(-1)), which is intended for solar particles, the anomalous cosmic rays and galactic cosmic rays. The overall capabilities of EPACT provide scientifically interesting measurements over all phases of the solar cycle. There will also be important opportunities for combined studies with other spacecraft, such as SAMPEX, Ulysses, and Voyagers 1 and 2. C1 UNIV MARYLAND,DEPT PHYS,COLLEGE PK,MD 20742. RP VONROSENVINGE, TT (reprint author), NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771, USA. OI Hamilton, Douglas/0000-0001-6103-8019 NR 12 TC 112 Z9 112 U1 0 U2 4 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 155 EP 206 PG 52 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100008 ER PT J AU LEPPING, RP ACUNA, MH BURLAGA, LF FARRELL, WM SLAVIN, JA SCHATTEN, KH MARIANI, F NESS, NF NEUBAUER, FM WHANG, YC BYRNES, JB KENNON, RS PANETTA, PV SCHEIFELE, J WORLEY, EM AF LEPPING, RP ACUNA, MH BURLAGA, LF FARRELL, WM SLAVIN, JA SCHATTEN, KH MARIANI, F NESS, NF NEUBAUER, FM WHANG, YC BYRNES, JB KENNON, RS PANETTA, PV SCHEIFELE, J WORLEY, EM TI THE WIND MAGNETIC-FIELD INVESTIGATION SO SPACE SCIENCE REVIEWS LA English DT Review ID CORONAL MASS EJECTIONS; IMP-8 OBSERVATIONS; PLASMA SHEET; STORMS; MAGNETOSPHERE; PASSAGE; SHOCK; CLOUD; EARTH; NORTHERN AB The magnetic field experiment on WIND will provide data for studies of a broad range of scales of structures and fluctuation characteristics of the interplanetary magnetic field throughout the mission, and, where appropriate, relate them to the statics and dynamics of the magnetosphere. The basic instrument of the Magnetic Field Investigation (MFI) is a boom-mounted dual triaxial fluxgate magnetometer and associated electronics. The dual configuration provides redundancy and also permits accurate removal of the dipolar portion of the spacecraft magnetic field. The instrument provides (1) near real-time data at nominally one vector per 92 s as key parameter data for broad dissemination, (2) rapid data at 10.9 vectors s(-1) for standard analysis, and (3) occasionally, snapshot (SS) memory data and Fast Fourier Transform data (FFT), both based on 44 vectors s(-1). These measurements will be precise (0.025%), accurate, ultra-sensitive (0.008 nT/step quantization), and where the sensor noise level is < 0.006 nT r.m.s. for 0-10 Hz. The digital processing unit utilizes a 12-bit microprocessor controlled analogue-to-digital converter. The instrument features a very wide dynamic range of measurement capability, from +/-4 nT up to +/-65536 nT per axis in eight discrete ranges. (The upper range permits complete testing in the Earth's field.) In the FTT mode power spectral density elements are transmitted to the ground as fast as once every 23 s (high rate), and 2.7 min of SS memory time series data, triggered automatically by pre-set command, requires typically about 5.1 hours for transmission. Standard data products are expected to be the following vector field averages: 0.0227-s (detail data from SS), 0.092 s ('detail' in standard mode), 3 s, 1 min, and 1 hour, in both GSE and GSM coordinates, as well as the FFT spectral elements. As has been our team's tradition, high instrument reliability is obtained by the use of fully redundant systems and extremely conservative designs. We plan studies of the solar wind: (1) as a collisionless plasma laboratory, at all time scales, macro, meso and micro, but concentrating on the kinetic scale, the highest time resolution of the instrument (=0.022 s), (2) as a consequence of solar energy and mass output, (3) as an external source of plasma that can couple mass, momentum, and energy to the Earth's magnetosphere, and (4) as it is modified as a consequence of its imbedded field interacting with the moon. Since the GEOTAIL Inboard Magnetometer (GIM), which is similar to the MFI instrument, was developed by members of our team, we provide a brief discussion of GIM related science objectives, along with MFI related science goals. C1 NATL SCI FDN,DIV ATMOSPHER SCI,WASHINGTON,DC 20550. UNIV DELAWARE,BARTOL RES INST,NEWARK,DE 19716. UNIV ROMA TOR VERGATA,DIPARTIMENTO FIS,I-00173 ROME,ITALY. UNIV COLOGNE,INST GEOPHYS & METEOROL,W-5000 COLOGNE 41,GERMANY. CATHOLIC UNIV AMER,DEPT MECH ENGN,WASHINGTON,DC 20064. RP LEPPING, RP (reprint author), NASA,GODDARD SPACE FLIGHT CTR,EXTRATERR PHYS LAB,GREENBELT,MD 20771, USA. RI Slavin, James/H-3170-2012; Farrell, William/I-4865-2013 OI Slavin, James/0000-0002-9206-724X; NR 50 TC 771 Z9 777 U1 6 U2 52 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 207 EP 229 DI 10.1007/BF00751330 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100009 ER PT J AU BOUGERET, JL KAISER, ML KELLOGG, PJ MANNING, R GOETZ, K MONSON, SJ MONGE, N FRIEL, L MEETRE, CA PERCHE, C SITRUK, L HOANG, S AF BOUGERET, JL KAISER, ML KELLOGG, PJ MANNING, R GOETZ, K MONSON, SJ MONGE, N FRIEL, L MEETRE, CA PERCHE, C SITRUK, L HOANG, S TI WAVES - THE RADIO AND PLASMA-WAVE INVESTIGATION ON THE WIND SPACECRAFT SO SPACE SCIENCE REVIEWS LA English DT Review ID TERRESTRIAL KILOMETRIC RADIATION; ACTIVE REGIONS; FREQUENCY; FORESHOCK; EMISSIONS; EARTH AB The WAVES investigation on the WIND spacecraft will provide comprehensive measurements of the radio and plasma wave phenomena which occur in Geospace. Analyses of these measurements, in coordination with the other onboard plasma, energetic particles, and field measurements will help us understand the kinetic processes that are important in the solar wind and in key boundary regions of the Geospace. These processes are then to be interpreted in conjunction with results from the other ISTP spacecraft in order to discern the measurements and parameters for mass, momentum, and energy flow throughout geospace. This investigation will also contribute to observations of radio waves emitted in regions where the solar wind is accelerated. The WAVES investigation comprises several innovations in this kind of instrumentation: among which the first use, to our knowledge, of neural networks in real-time on board a scientific spacecraft to analyze data and command observation modes, and the first use of a wavelet transform-like analysis in real time to perform a spectral analysis of a broad band signal. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NASA,GODDARD SPACE FLIGHT CTR,LANHAM,MD. HUGHES STX,LANHAM,MD. STIL,MAYNOOTH,KILDARE,IRELAND. UNIV MINNESOTA,SCH PHYS & ASTRON,MINNEAPOLIS,MN 55455. RP BOUGERET, JL (reprint author), OBSERV PARIS,DESPA,CNRS,URA 264,F-92195 MEUDON,FRANCE. NR 16 TC 523 Z9 529 U1 2 U2 11 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 231 EP 263 DI 10.1007/BF00751331 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100010 ER PT J AU APTEKAR, RL FREDERIKS, DD GOLENETSKII, SV ILYNSKII, VN MAZETS, EP PANOV, VN SOKOLOVA, ZJ TEREKHOV, MM SHESHIN, LO CLINE, TL STILWELL, DE AF APTEKAR, RL FREDERIKS, DD GOLENETSKII, SV ILYNSKII, VN MAZETS, EP PANOV, VN SOKOLOVA, ZJ TEREKHOV, MM SHESHIN, LO CLINE, TL STILWELL, DE TI KONUS-W GAMMA-RAY BURST EXPERIMENT FOR THE GGS WIND SPACECRAFT SO SPACE SCIENCE REVIEWS LA English DT Review AB The Konus-W experiment to be flown on board the GGS-Wind spacecraft is designed to observe gamma-ray bursts and solar flares with moderate spectral and high time resolution. Two large scintillators are used to provide omnidirectional sensitivity. The primary scientific objectives are the study of the continuum energy spectra and spectral features of these events in the energy range of 10 keV to 10 MeV, as well as their time histories in soft, medium, and hard energy bands, with a time resolution to 2 ms. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP APTEKAR, RL (reprint author), AF IOFFE PHYS TECH INST,POLITEKHNICHESKAYA 26,ST PETERSBURG 194021,RUSSIA. RI Golenetskii, Sergey/B-3818-2015; Frederiks, Dmitry/C-7612-2014; Aptekar, Raphail/B-3456-2015 OI Frederiks, Dmitry/0000-0002-1153-6340; NR 5 TC 105 Z9 105 U1 0 U2 1 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 265 EP 272 DI 10.1007/BF00751332 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100011 ER PT J AU OWENS, A BAKER, R CLINE, TL GEHRELS, N JERMAKIAN, J NOLAN, T RAMATY, R SEIFERT, H SHEPHARD, DA SMITH, G STILWELL, DE TEEGARDEN, BJ CORK, CP LANDIS, DA LUKE, PN MADDEN, NW MALONE, D PEHL, RH YAVER, H HURLEY, K MATHIAS, S POST, AH AF OWENS, A BAKER, R CLINE, TL GEHRELS, N JERMAKIAN, J NOLAN, T RAMATY, R SEIFERT, H SHEPHARD, DA SMITH, G STILWELL, DE TEEGARDEN, BJ CORK, CP LANDIS, DA LUKE, PN MADDEN, NW MALONE, D PEHL, RH YAVER, H HURLEY, K MATHIAS, S POST, AH TI HIGH-RESOLUTION GE SPECTROMETER FOR GAMMA-RAY BURST ASTRONOMY SO SPACE SCIENCE REVIEWS LA English DT Review ID ABSORPTION; FEATURES AB The Transient Gamma-Ray Spectrometer (TGRS) to be flown aboard the WIND spacecraft is primarily designed to perform high resolution spectroscopy of transient gamma-ray events, such as cosmic gamma-ray bursts and solar flares over the energy range 25 keV to 8.2 MeV with an expected spectroscopic resolution of similar to 3 keV at 1 MeV. The detector itself consists of a 215 cm(3) high purity n-type Ge crystal kept at cryogenic temperatures by a passive radiative cooler. The geometric field of view defined by the cooler is similar to 1.8 pi steradian. To avoid continuous triggers by soft solar events, a thin BeCu Sun-shield around the sides of the cooler has been provided. A passive Mo/Pb occulter, which modulates signals from within +/-5 degrees of the ecliptic plane at the spacecraft spin frequency, is used to identify and study solar flares, as well as emission from the galactic plane and center. Thus, in addition to transient event measurements, the instrument will allow the search for possible diffuse background lines and monitor the 511 keV positron annihilation radiation from the galactic center. In order to handle the typically large burst count rates, which can be in excess of 100 kHz, burst data are stored directly in an onboard 2.75 Mbit burst memory with an absolute timing accuracy of +/-1.5 ms after ground processing. The memory is capable of storing the entire spectral data set of all but the largest bursts. WIND is scheduled to be launched on a Delta II launch vehicle from Cape Canaveral on November 1, 1994. After injection into a phasing orbit, the spacecraft will execute a double lunar swing-by before being moved into a controlled 'halo' orbit about the L1 Lagrangian point (similar to 250 R(e) towards the Sun). This will provide a 5 light-second light travel time with which to triangulate gamma-ray burst sources with Earth-orbiting systems, such as those on-board the Gamma-Ray Observatory (GRO). The response of instrument to transient gamma-ray events such as GRB's and solar flares will be presented as well as the expected response to steady state point sources and galactic center line emission. C1 NASA, GODDARD SPACE FLIGHT CTR, HIGH ENERGY ASTROPHYS LAB, GREENBELT, MD 20771 USA. LAWRENCE BERKELEY LAB, BERKELEY, CA 94702 USA. UNIV CALIF BERKELEY, SPACE SCI LAB, BERKELEY, CA 94720 USA. ARTHUR D LITTLE INC, CAMBRIDGE, MA 02140 USA. RI Gehrels, Neil/D-2971-2012 NR 29 TC 24 Z9 24 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 273 EP 296 DI 10.1007/BF00751333 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100012 ER PT J AU TORR, MR TORR, DG ZUKIC, M JOHNSON, RB AJELLO, J BANKS, P CLARK, K COLE, K KEFFER, C PARKS, G TSURUTANI, B SPANN, J AF TORR, MR TORR, DG ZUKIC, M JOHNSON, RB AJELLO, J BANKS, P CLARK, K COLE, K KEFFER, C PARKS, G TSURUTANI, B SPANN, J TI A FAR-ULTRAVIOLET IMAGER FOR THE INTERNATIONAL SOLAR-TERRESTRIAL PHYSICS MISSION SO SPACE SCIENCE REVIEWS LA English DT Review ID THIN-FILMS; DEPENDENCE; EMISSIONS; SATELLITE; FILTERS; AURORA; SPACE AB The aurorae are the result of collisions with the atmosphere of energetic particles that have their origin in the solar wind, and reach the atmosphere after having undergone varying degrees of acceleration and redistribution within the Earth's magnetosphere. The global scale phenomenon represented by the aurorae therefore contains considerable information concerning the solar-terrestrial connection. For example, by correctly measuring specific auroral emissions, and with the aid of comprehensive models of the region, we can infer the total energy flux entering the atmosphere and the average energy of the particles causing these emissions. Furthermore, from these auroral emissions we can determine the ionospheric conductances that are part of the closing of the magnetospheric currents through the ionosphere, and from these we can in turn obtain the electric potentials and convective patterns that are an essential element to our understanding of the global magnetosphere-ionosphere-thermosphere-mesosphere. Simultaneously acquired images of the auroral oval and polar cap not only yield the temporal and spatial morphology from which we can infer activity indices, but in conjunction with simultaneous measurements made on spacecraft at other locations within the magnetosphere, allow us to map the various parts of the oval back to their source regions in the magnetosphere. This paper describes the Ultraviolet Imager for the Global Geospace Sciences portion of the International Solar-Terrestrial Physics program. The instrument operates in the far ultraviolet (FUV) and is capable of imaging the auroral oval regardless of whether it is sunlit or in darkness. The instrument has an 8 degrees circular field of view and is located on a despun platform which permits simultaneous imaging of the entire oval for at least 9 hours of every 18 hour orbit. The three mirror, unobscured aperture, optical system (f/2.9) provides excellent imaging over this full field of view, yielding a per pixel angular resolution of 0.6 milliradians. Its FUV filters have been designed to allow accurate spectral separation of the features of interest, thus allowing quantitative interpretation of the images to provide the parameters mentioned above. The system has been designed to provide ten orders of magnitude blocking against longer wavelength (primarily visible) scattered sunlight, thus allowing the first imaging of key, spectrally resolved, FUV diagnostic features in the fully sunlit midday aurorae. The intensified-CCD detector has a nominal frame rate of 37 s, and the fast optical system has a noise equivalent signal within one frame of similar to 10 R. The instantaneous dynamic range is > 1000 and can be positioned within an overall gain range of 10(4), allowing measurement of both the very weak polar cap emissions and the very bright aurora. The optical surfaces have been designed to be sufficiently smooth to permit this dynamic range to be utilized without the scattering of light from bright features into the weaker features. Finally, the data product can only be as good as the degree to which the instrument performance is characterized and calibrated. In the VUV, calibration of an an imager intended for quantitative studies is a task requiring some pioneering methods, but it is now possible to calibrate such an instrument over its focal plane to an accuracy of +/-10%. In summary, very recent advances in optical, filter and detector technology have been exploited to produce an auroral imager to meet the ISTP objectives. C1 UNIV ALABAMA, OPT AERON LAB, HUNTSVILLE, AL 35899 USA. OPT ETC INC, HUNTSVILLE, AL 35801 USA. JET PROP LAB, PASADENA, CA USA. UNIV MICHIGAN, ANN ARBOR, MI 48109 USA. UNIV WASHINGTON, SEATTLE, WA USA. LA TROBE UNIV, LATROBE, AUSTRALIA. NASA, GEORGE C MARSHALL SPACE FLIGHT CTR, SPACE SCI LAB, HUNTSVILLE, AL 35812 USA. RP NASA, GEORGE C MARSHALL SPACE FLIGHT CTR, PAYLOAD PROJECTS OFF, HUNTSVILLE, AL 35812 USA. NR 39 TC 307 Z9 308 U1 2 U2 11 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 329 EP 383 DI 10.1007/BF00751335 PG 55 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100014 ER PT J AU MOORE, TE CHAPPELL, CR CHANDLER, MO FIELDS, SA POLLOCK, CJ REASONER, DL YOUNG, DT BURCH, JL EAKER, N WAITE, JH MCCOMAS, DJ NORDHOLDT, JE THOMSEN, MF BERTHELIER, JJ ROBSON, R AF MOORE, TE CHAPPELL, CR CHANDLER, MO FIELDS, SA POLLOCK, CJ REASONER, DL YOUNG, DT BURCH, JL EAKER, N WAITE, JH MCCOMAS, DJ NORDHOLDT, JE THOMSEN, MF BERTHELIER, JJ ROBSON, R TI THE THERMAL ION DYNAMICS EXPERIMENT AND PLASMA SOURCE INSTRUMENT SO SPACE SCIENCE REVIEWS LA English DT Review AB The Thermal Ion Dynamics Experiment (TIDE) and the Plasma Source Instrument (PSI) have been developed in response to the requirements of the ISTP Program for three-dimensional (3D) plasma composition measurements capable of tracking the circulation of low-energy (0-500 eV) plasma through the polar magnetosphere. This plasma is composed of penetrating magnetosheath and escaping ionospheric components. It is in part lost to the downstream solar wind and in part recirculated within the magnetosphere, participating in the formation of the diamagnetic hot plasma sheet and ring current plasma populations. Significant obstacles which have previously made this task impossible include the low density and energy of the outflowing ionospheric plasma plume and the positive spacecraft floating potentials which exclude the lowest-energy plasma from detection on ordinary spacecraft. Based on a unique combination of focusing electrostatic ion optics and time of flight detection and mass analysis, TIDE provides the sensitivity (seven apertures of similar to 1 cm(2) effective area each) and angular resolution (6 degrees x 18 degrees) required for this purpose. PSI produces a low energy plasma locally at the POLAR spacecraft that provides the ion current required to balance the photoelectron current, along with a low temperature electron population, regulating the spacecraft potential slightly positive relative to the space plasma. TIDE/PSI will: (a) measure the density and flow fields of the solar and terrestrial plasmas within the high polar cap and magnetospheric lobes; (b) quantify the extent to which ionospheric and solar ions are recirculated within the distant magnetotail neutral sheet or lost to the distant tail and solar wind; (c) investigate the mass-dependent degree energization of these plasmas by measuring their thermodynamic properties; (d) investigate the relative roles of ionosphere and solar wind as sources of plasma to the plasma sheet and ring current. C1 SW RES INST,SAN ANTONIO,TX 78284. LOS ALAMOS NATL LAB,LOS ALAMOS,NM 87545. CTR RECH PHYS ENVIRONN,F-94107 ST MAUR FOSSES,FRANCE. HUGHES AIRCRAFT CO,RES LABS,MALIBU,CA 90265. RP MOORE, TE (reprint author), NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812, USA. RI Moore, Thomas/D-4675-2012 OI Moore, Thomas/0000-0002-3150-1137 NR 14 TC 76 Z9 76 U1 1 U2 6 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 409 EP 458 DI 10.1007/BF00751337 PG 50 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100016 ER PT J AU SCUDDER, J HUNSACKER, F MILLER, G LOBELL, J ZAWISTOWSKI, T OGILVIE, K KELLER, J CHORNAY, D HERRERO, F FITZENREITER, R FAIRFIELD, D NEEDELL, J BODET, D GOOGINS, J KLETZING, C TORBERT, R VANDIVER, J BENTLEY, R FILLIUS, W MCILWAIN, C WHIPPLE, E KORTH, A AF SCUDDER, J HUNSACKER, F MILLER, G LOBELL, J ZAWISTOWSKI, T OGILVIE, K KELLER, J CHORNAY, D HERRERO, F FITZENREITER, R FAIRFIELD, D NEEDELL, J BODET, D GOOGINS, J KLETZING, C TORBERT, R VANDIVER, J BENTLEY, R FILLIUS, W MCILWAIN, C WHIPPLE, E KORTH, A TI HYDRA-A3-DIMENSIONAL ELECTRON AND ION HOT PLASMA INSTRUMENT FOR THE POLAR SPACECRAFT OF THE GGS MISSION SO SPACE SCIENCE REVIEWS LA English DT Review ID SPECTRAL CHARACTERISTICS; GEOMAGNETIC CONDITIONS; SHEET ION; POPULATIONS AB HYDRA is an experimental hot plasma investigation for the POLAR spacecraft of the GGS program. A consortium of institutions has designed a suite of particle analyzers that sample the velocity space of electron and ions between similar or equal to 2 keV/q - 35 keV/q in three dimensions, with a routine time resolution of 0.5 s. Routine coverage of velocity space will be accomplished with an angular homogeneity assumption of similar or equal to 16 degrees, appropriate for subsonic plasmas, but with special similar or equal to 1.5 degrees resolution for electrons with energies between 100 eV and 10 keV along and opposed to the local magnetic field. This instrument produces 4.9 kilobits s(-1) to the telemetry, consumes on average 14 W and requires 18.7 kg for deployment including its internal shielding. The scientific objectives for the polar magnetosphere fall into four broad categories: (1) those to define the ambient kinetic regimes of ions and electrons; (2) those to elucidate the magnetohydrodynamic responses in these regimes; (3) those to assess the particle populations with high time resolution; and (4) those to determine the global topology of the magnetic field. In the first group are issues of identifying the origins of particles at high magnetic latitudes, their energization, the altitude dependence of the forces, including parallel electric fields they have traversed. In the second group are the physics of the fluid flows, regimes of current, and plasma depletion zones during quiescent and disturbed magnetic conditions. In the third group is the exploration of the processes that accompany the rapid time variations known to occur in the auroral zone, cusp and entry layers as they affect the flow of mass, momentum and energy in the auroral region. In the fourth class of objectives are studies in conjunction with the SWE measurements of the Strahl in the solar wind that exploit the small gyroradius of thermal electrons to detect those magnetic field lines that penetrate the auroral region that are directly 'open' to interplanetary space where, for example, the Polar Rain is observed. C1 NASA,GODDARD SPACE FLIGHT CTR,EXTRATERR PHYS LAB,GREENBELT,MD 20771. UNIV NEW HAMPSHIRE,DURHAM,NH 03824. UNIV CALIF SAN DIEGO,LA JOLLA,CA 92093. VANDIVER ASSOCIATES,HUNTSVILLE,AL. MPAE,KATLENBERG LINDAU,GERMANY. RP SCUDDER, J (reprint author), UNIV IOWA,IOWA CITY,IA 52242, USA. RI Keller, John/I-5097-2013; OI Kletzing, Craig/0000-0002-4136-3348 NR 17 TC 136 Z9 136 U1 0 U2 3 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 459 EP 495 DI 10.1007/BF00751338 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100017 ER PT J AU BLAKE, JB FENNELL, JF FRIESEN, LM JOHNSON, BM KOLASINSKI, WA MABRY, DJ OSBORN, JV PENZIN, SH SCHNAUSS, ER SPENCE, HE BAKER, DN BELIAN, R FRITZ, TA FORD, W LAUBSCHER, B STIGLICH, R BARAZE, RA HILSENRATH, MF IMHOF, WL KILNER, JR MOBILIA, J VOSS, DH KORTH, A GULL, M FISHER, K GRANDE, M HALL, D AF BLAKE, JB FENNELL, JF FRIESEN, LM JOHNSON, BM KOLASINSKI, WA MABRY, DJ OSBORN, JV PENZIN, SH SCHNAUSS, ER SPENCE, HE BAKER, DN BELIAN, R FRITZ, TA FORD, W LAUBSCHER, B STIGLICH, R BARAZE, RA HILSENRATH, MF IMHOF, WL KILNER, JR MOBILIA, J VOSS, DH KORTH, A GULL, M FISHER, K GRANDE, M HALL, D TI CEPPAD - COMPREHENSIVE ENERGETIC PARTICLE AND PITCH-ANGLE DISTRIBUTION EXPERIMENT ON POLAR SO SPACE SCIENCE REVIEWS LA English DT Review AB The CEPPAD Experiment consists of four sensors for investigating energetic particle phenomena on the POLAR mission. These sensors provide 3-D proton and electron angular distributions in the energy range of 20 keV to 1 MeV, energetic proton and electron measurements extending to energies greater than 10 MeV, high angular and time resolution measurements in the loss-cone, and data on energetic neutral particles. All sensors operate in conjunction with special on-board data processing units which control sensor data acquisition modes while performing in-flight data processing, data compression, and telemetry formatting. Presented here is a CEPPAD system overview together with descriptions of the individual sensors, the in-flight data processing, and examples of sensor calibration data. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. LOS ALAMOS NATL LAB,LOS ALAMOS,NM 87545. LOCKHEED PALO ALTO RES LABS,PALO ALTO,CA 94304. MAX PLANCK INST AERON,KATLENBURG DUHM,GERMANY. RUTHERFORD APPLETON LAB,DIDCOT,OXON,ENGLAND. RP BLAKE, JB (reprint author), AEROSP CORP,POB 92957,LOS ANGELES,CA 90009, USA. RI Spence, Harlan/A-1942-2011; Grande, Manuel/C-2242-2013; OI Grande, Manuel/0000-0002-2233-2618; Spence, Harlan/0000-0002-2526-2205 NR 0 TC 131 Z9 131 U1 3 U2 7 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 531 EP 562 DI 10.1007/BF00751340 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100019 ER PT J AU HARVEY, P MOZER, FS PANKOW, D WYGANT, J MAYNARD, NC SINGER, H SULLIVAN, W ANDERSON, PB PFAFF, R AGGSON, T PEDERSEN, A FALTHAMMAR, CG TANSKANNEN, P AF HARVEY, P MOZER, FS PANKOW, D WYGANT, J MAYNARD, NC SINGER, H SULLIVAN, W ANDERSON, PB PFAFF, R AGGSON, T PEDERSEN, A FALTHAMMAR, CG TANSKANNEN, P TI THE ELECTRIC-FIELD INSTRUMENT ON THE POLAR SATELLITE SO SPACE SCIENCE REVIEWS LA English DT Review AB The Polar satellite carries a system of four wire booms in the spacecraft spin plane and two rigid booms along the spin axis. Each of the booms has a spherical sensor at its tip along with nearby guard and stub surfaces whose potentials relative to that of their sphere are controlled by associated electronics. The potential differences between opposite sphere pairs are measured to yield the three components of the DC to >1 MHz electric field. Spheres can also be operated in a mode in which their collected current is measured to give information on the plasma density and its fluctuations. The scientific studies to be performed by this experiment as well as the mechanical and electrical properties of the detector system are described. C1 GPSG,GEOPHYS DIRECTORATE,PHILLIPS LAB,HANSCOM AFB,BEDFORD,MA. BOSTON UNIV,CTR SPACE PHYS,BOSTON,MA 02215. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. EUROPEAN SPACE TECHNOL CTR,2200 AG NOORDWIJK,NETHERLANDS. ROYAL INST TECHNOL,S-10044 STOCKHOLM,SWEDEN. UNIV OULU,OULU,FINLAND. UNIV CALIF BERKELEY,DEPT PHYS,BERKELEY,CA 94720. RP HARVEY, P (reprint author), UNIV CALIF BERKELEY,SPACE SCI LAB,BERKELEY,CA 94720, USA. RI Pfaff, Robert/F-5703-2012 OI Pfaff, Robert/0000-0002-4881-9715 NR 0 TC 131 Z9 135 U1 2 U2 4 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 583 EP 596 DI 10.1007/BF00751342 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100021 ER PT J AU MISH, WH GREEN, JL REPH, MG PEREDO, M AF MISH, WH GREEN, JL REPH, MG PEREDO, M TI ISTP SCIENCE DATA SYSTEMS AND PRODUCTS SO SPACE SCIENCE REVIEWS LA English DT Review ID MAGNETOSPHERIC MAGNETIC-FIELD; QUANTITATIVE MODELS; BIRKELAND CURRENTS; SHEET AB The International Solar-Terrestrial Physics (ISTP) program will provide simultaneous coordinated scientific measurements from most of the major areas of geospace including specific locations on the Earth's surface. This paper describes the comprehensive ISTP ground science data handling system which has been developed to promote optimal mission planning and efficient data processing, analysis and distribution. The essential components of this ground system are the ISTP Central Data Handling Facility (CDHF), the Information Processing Division's Data Distribution Facility (DDF), the ISTP/Global Geospace Science (GGS) Science Planning and Operations Facility (SPOF) and the NASA Data Archive and Distribution Service (NDADS). The ISTP CDHF is the one place in the program where measurements from this wide variety of geospace and ground-based instrumentation and theoretical studies are brought together. Subsequently, these data will be distributed, along with ancillary data, in a unified fashion to the ISTP Principal Investigator (PI) and Go-Investigator (CoI) teams for analysis on their local systems. The CDHF ingests the telemetry streams, orbit, attitude, and command history from the GEOTAIL, WIND, POLAR, SOHO, and LMP-8 Spacecraft; computes summary data sets, called Key Parameters (KPs), for each scientific instrument; ingests pre-computed KPs from other spacecraft and ground based investigations; provides a computational platform for parameterized modeling; and provides a number of 'data services' for the ISTP community of investigators. The DDF organizes the KPs, decommutated telemetry, and associated ancillary data into products for distribution to the ISTP community on CD-ROMs. The SPOF is the component of the GGS program responsible for the development and coordination of ISTP science planning operations. The SPOF operates under the direction of the ISTP Project Scientist and is responsible for the development and coordination of the science plan for ISTP spacecraft. Instrument command requests for the WIND and POLAR investigations are submitted by the PIs to the SPOF where they are checked for science conflicts, forwarded to the GSFC Command Management System/Payload Operations Control Center (CMS/POCC) for engineering conflict validation, and finally incorporated into the conflict-free science operations plan. Conflict resolution is accomplished through iteration between the PIs, SPOF and CMS and in consultation with the Project Scientist when necessary. The long term archival of ISTP KP and level-zero data will be undertaken by NASA's National Space Science Data Center using the NASA Data Archive and Distribution Service (NDADS). This on-line archive facility will provide rapid access to archived KPs and event data and includes security features to restrict access to the data during the time they are proprietary. C1 NASA,GODDARD SPACE FLIGHT CTR,HUGHES STX CORP,GREENBELT,MD 20771. RP MISH, WH (reprint author), NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771, USA. NR 30 TC 14 Z9 14 U1 0 U2 2 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0038-6308 J9 SPACE SCI REV JI Space Sci. Rev. PD FEB PY 1995 VL 71 IS 1-4 BP 815 EP 877 DI 10.1007/BF00751352 PG 63 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QU891 UT WOS:A1995QU89100031 ER PT J AU RAIKAR, GN GREGORY, JC PARTLOW, WD HERZIG, H CHOYKE, WJ AF RAIKAR, GN GREGORY, JC PARTLOW, WD HERZIG, H CHOYKE, WJ TI SURFACE CHARACTERIZATION OF SIC MIRRORS EXPOSED TO FAST ATOMIC OXYGEN SO SURFACE AND INTERFACE ANALYSIS LA English DT Article; Proceedings Paper CT Surface Analysis 94 CY JUN 15-17, 1994 CL BURLINGTON, MA SP AMER VACUUM SOC, APPL SURFACE SCI DIV, AMER VACUUM SOC, NEW ENGLAND CHAPTER, AMER SOC TESTING & MAT ID OXIDATION; SILICON; SPECTROSCOPY; FILMS AB Two chemical vapor deposited silicon carbide (SiC) mirrors were exposed to the 5 eV fast atomic oxygen environment in low Earth orbit on NASA's Long Duration Exposure Facility (LDEF) which remained in space for nearly 6 years. The samples were characterized using the techniques of x-ray photoelectron spectroscopy (XPS), ellipsometry, and reflectance measurements. The normal-incidence optical reflectance of the atomic-oxygen-expose portion of one sample degraded considerably over the 60-160 nm span. The XPS results showed the presence of SiO2-like species, the thickness varying from 1 to 8 nm depending upon the location of the samples on the space-craft. The XPS results are in good agreement with those from ellipsometry measurements. C1 WESTINGHOUSE ELECT CORP,CTR SCI & TECHNOL,PITTSBURGH,PA 15235. NASA,GODDARD SPACE FLIGHT CTR,DIV SPACE TECHNOL,OPT BRANCH,GREENBELT,MD 20771. UNIV PITTSBURGH,DEPT PHYS & ASTRON,PITTSBURGH,PA 15260. RP RAIKAR, GN (reprint author), UNIV ALABAMA,DEPT CHEM,SURFACE SCI LABS,HUNTSVILLE,AL 35899, USA. NR 19 TC 9 Z9 9 U1 0 U2 0 PU JOHN WILEY & SONS LTD PI W SUSSEX PA BAFFINS LANE CHICHESTER, W SUSSEX, ENGLAND PO19 1UD SN 0142-2421 J9 SURF INTERFACE ANAL JI Surf. Interface Anal. PD FEB PY 1995 VL 23 IS 2 BP 77 EP 82 DI 10.1002/sia.740230206 PG 6 WC Chemistry, Physical SC Chemistry GA QM242 UT WOS:A1995QM24200004 ER PT J AU DUCK, PW LASSEIGNE, DG HUSSAINI, MY AF DUCK, PW LASSEIGNE, DG HUSSAINI, MY TI ON THE INTERACTION BETWEEN THE SHOCK-WAVE ATTACHED TO A WEDGE AND FREESTREAM DISTURBANCES SO THEORETICAL AND COMPUTATIONAL FLUID DYNAMICS LA English DT Article AB We present a study of the interaction of small amplitude, unsteady, freestream disturbances with a shock wave induced by a wedge in supersonic flow. These disturbances may be acoustic waves, vorticity waves, or entropy waves (or indeed a combination of all three). Their interactions then generate behind the shock disturbances of all three classes, an aspect that is investigated in some detail. Also, the possibility of enhanced mixing owing to additional vorticity produced by the shock-body coupling is investigated. It is shown that disturbances behind the shock may either decay downstream, or alternatively experience sustained oscillations. The precise regimes under which either behaviour is found are stated. C1 OLD DOMINION UNIV,DEPT MATH & STAT,NORFOLK,VA 23529. NASA,LANGLEY RES CTR,INST COMP APPL SCI & ENGN,HAMPTON,VA 23681. RP DUCK, PW (reprint author), UNIV MANCHESTER,DEPT MATH,OXFORD RD,MANCHESTER M13 9PL,LANCS,ENGLAND. NR 24 TC 8 Z9 8 U1 0 U2 1 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0935-4964 J9 THEOR COMP FLUID DYN JI Theor. Comput. Fluid Dyn. PD FEB PY 1995 VL 7 IS 2 BP 119 EP 139 DI 10.1007/BF00311809 PG 21 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA QK529 UT WOS:A1995QK52900003 ER PT J AU ALALUF, M APPELBAUM, J KLIBANOV, L BRINKER, D SCHEIMAN, D CROITORU, N AF ALALUF, M APPELBAUM, J KLIBANOV, L BRINKER, D SCHEIMAN, D CROITORU, N TI AMORPHOUS DIAMOND-LIKE CARBON-FILMS - A HARD ANTI-REFLECTING COATING FOR SILICON SOLAR-CELLS SO THIN SOLID FILMS LA English DT Letter DE AMORPHOUS MATERIALS; DIAMOND; OPTICAL COATINGS; SOLAR CELLS ID SCHOTTKY AB Amorphous diamond-line carbon (a:DLC) films are suitable for use as a protective layer and/or anti-reflecting coating for silicon solar cells. Microhardness tests show a high hardness of about 4700 kg mm(-2) Optical measurements in the visible light on a silicon solar cell without anti-reflecting coating where a:DLC was deposited as an anti-reflecting (AR) coating, show a significant reduction in the reflection of the light of about 25-45% as compared with the reflection from the solar cell before deposition of the a:DLC film. The current-voltage (I-V) characteristics of solar cells without an anti-reflecting coating and with a:DLC as the AR coating layer show an improvement in the short circuit current (from 107 mA to 116 mA) and in the efficiency of the cell by 1% (from 8% to 9%). I-V characteristics of a solar cell with AR coating and deposited a:DLC (400 Angstrom thickness) over that film as a protective coating, show a slight reduction of the short circuit current (from 168 mA to 145 mA), and the efficiency of the solar cell decreases (16% to 14%). However, the microhardness was significantly increased. C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. RP ALALUF, M (reprint author), TEL AVIV UNIV,FAC ENGN,DEPT ELECT ENGN PHYS ELECTR,IL-69978 RAMAT AVIV,ISRAEL. NR 9 TC 30 Z9 32 U1 0 U2 6 PU ELSEVIER SCIENCE SA LAUSANNE PI LAUSANNE 1 PA PO BOX 564, 1001 LAUSANNE 1, SWITZERLAND SN 0040-6090 J9 THIN SOLID FILMS JI Thin Solid Films PD FEB 1 PY 1995 VL 256 IS 1-2 BP 1 EP 3 DI 10.1016/0040-6090(95)80024-7 PG 3 WC Materials Science, Multidisciplinary; Materials Science, Coatings & Films; Physics, Applied; Physics, Condensed Matter SC Materials Science; Physics GA QF102 UT WOS:A1995QF10200001 ER PT J AU WATSON, AB TURANO, K AF WATSON, AB TURANO, K TI THE OPTIMAL MOTION STIMULUS SO VISION RESEARCH LA English DT Article DE EFFICIENCY; RECEPTIVE FIELD; MOTION FILTER; VISION; TEMPORAL; SPATIAL; BANDWIDTH; GABOR ID SPATIAL-FREQUENCY SELECTIVITY; MACAQUE VISUAL-CORTEX; HUMAN-VISION; RECEPTIVE-FIELDS; SIMPLE CELLS; SUMMATION; DETECTORS; CHANNELS; MODELS; CAT AB Contrast energy thresholds were measured for discriminating the direction of a drifting sinusoidal grating multiplied by an independently drifting space-time Gaussian (a generalized Gabor). We argue that the stimulus with the lowest contrast energy threshold identifies the receptive field of the most efficient linear motion filter. This optimal motion stimulus is found to be at 3 c/deg and 5 Hz, with a width and height of 0.44 deg and a duration of 0.133 sec, corresponding to spatial and temporal bandwidths of 1.1 and 2.5 octaves, respectively. The spectral receptive field is aligned more nearly to the Cartesian axes than to the velocity contour. C1 JOHNS HOPKINS UNIV,SCH MED,WILMER INST,BALTIMORE,MD 21205. RP WATSON, AB (reprint author), NASA,AMES RES CTR,MAIL STOP 262-2,MOFFETT FIELD,CA 94035, USA. NR 46 TC 72 Z9 72 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0042-6989 J9 VISION RES JI Vision Res. PD FEB PY 1995 VL 35 IS 3 BP 325 EP 336 DI 10.1016/0042-6989(94)00182-L PG 12 WC Neurosciences; Ophthalmology SC Neurosciences & Neurology; Ophthalmology GA QC070 UT WOS:A1995QC07000002 PM 7892728 ER PT J AU ASKER, JR AF ASKER, JR TI MISSION-63 TO TEST UNITED-STATES RUSSIAN TEAMING SO AVIATION WEEK & SPACE TECHNOLOGY LA English DT Article RP ASKER, JR (reprint author), NASA,LYNDON B JOHNSON SPACE CTR,HOUSTON,TX 77058, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU MCGRAW HILL INC PI NEW YORK PA 1221 AVENUE OF THE AMERICAS, NEW YORK, NY 10020 SN 0005-2175 J9 AVIAT WEEK SPACE TEC JI Aviat. Week Space Technol. PD JAN 30 PY 1995 VL 142 IS 5 BP 36 EP 38 PG 3 WC Engineering, Aerospace SC Engineering GA QD740 UT WOS:A1995QD74000024 ER PT J AU KULKARNI, M NOOR, AK AF KULKARNI, M NOOR, AK TI SENSITIVITY ANALYSIS OF THE NONLINEAR DYNAMIC VISCOPLASTIC RESPONSE OF 2-D STRUCTURES WITH RESPECT TO MATERIAL PARAMETERS SO INTERNATIONAL JOURNAL FOR NUMERICAL METHODS IN ENGINEERING LA English DT Article DE SENSITIVITY; NONLINEAR DYNAMIC RESPONSE; VISCOPLASTICITY; FINITE ELEMENTS; GENERALIZED PLANE STRESS ID SYSTEMS AB A computational procedure is presented for evaluating the sensitivity coefficients of the viscoplastic response of structures subjected to dynamic loading. A state of plane stress is assumed to exist in the structure, a velocity strain-Cauchy stress formulation is used, and the geometric non-linearities arising from large strains are incorporated. The Jaumann rate is used as a frame indifferent stress rate. The material model is chosen to be isothermal viscoplasticity, and an associated flow rule is used with a von Mises effective stress. The equations of motion emanating from a finite element semi-discretization are evaluated using a direct different scheme with a implicit stress update. The sensitivity coefficients are evaluated using a direct differentiation approach. Since the domain of integration is the current configuration, the sensitivity coefficients of the spatial derivatives of the shape functions must be included. Numerical results are presented for a thin plate with a central circular cutout subjected to an in-plane compressive loading. The sensitivity coefficients are generated by evaluating the derivatives of the response quantities with respect to Young's modulus, and two of the material parameters characterizing the viscoplastic response. Time histories of the response and sensitivity coefficients, and spatial distributions at selected times are presented. RP KULKARNI, M (reprint author), UNIV VIRGINIA,CTR COMPUTAT STRUCT TECHNOL,NASA,LANGLEY RES CTR,HAMPTON,VA 23681, USA. NR 15 TC 8 Z9 8 U1 1 U2 2 PU JOHN WILEY & SONS LTD PI W SUSSEX PA BAFFINS LANE CHICHESTER, W SUSSEX, ENGLAND PO19 1UD SN 0029-5981 J9 INT J NUMER METH ENG JI Int. J. Numer. Methods Eng. PD JAN 30 PY 1995 VL 38 IS 2 BP 183 EP 198 DI 10.1002/nme.1620380203 PG 16 WC Engineering, Multidisciplinary; Mathematics, Interdisciplinary Applications SC Engineering; Mathematics GA QF611 UT WOS:A1995QF61100002 ER PT J AU CESS, RD ZHANG, MH MINNIS, P CORSETTI, L DUTTON, EG FORGAN, BW GARBER, DP GATES, WL HACK, JJ HARRISON, EF JING, X KIEHL, JT LONG, CN MORCRETTE, JJ POTTER, GL RAMANATHAN, V SUBASILAR, B WHITLOCK, CH YOUNG, DF ZHOU, Y AF CESS, RD ZHANG, MH MINNIS, P CORSETTI, L DUTTON, EG FORGAN, BW GARBER, DP GATES, WL HACK, JJ HARRISON, EF JING, X KIEHL, JT LONG, CN MORCRETTE, JJ POTTER, GL RAMANATHAN, V SUBASILAR, B WHITLOCK, CH YOUNG, DF ZHOU, Y TI ABSORPTION OF SOLAR-RADIATION BY CLOUDS - OBSERVATIONS VERSUS MODELS SO SCIENCE LA English DT Article ID SATELLITE; BUDGET AB There has been a long history of unexplained anomalous absorption of solar radiation by clouds. Collocated satellite and surface measurements of solar radiation at five geographically diverse locations showed significant solar absorption by clouds, resulting in about 25 watts per square meter more global-mean absorption by the cloudy atmosphere than predicted by theoretical models. It has often been suggested that tropospheric aerosols could increase cloud absorption. But these aerosols are temporally and spatially heterogeneous, whereas the observed cloud absorption is remarkably invariant with respect to season and location. Although its physical cause is unknown, enhanced cloud absorption substantially alters our understanding of the atmosphere's energy budget. C1 NASA,LANGLEY RES CTR,DIV ATMOSPHER SCI,HAMPTON,VA 23665. LAWRENCE LIVERMORE NATL LAB,PROGRAM CLIMATE MODEL DIAG & INTERCOMPARISON,LIVERMORE,CA 94550. NOAA,ENVIRONM RES LABS,CLIMATE MONITORING & DIAGNOST LAB,BOULDER,CO 80303. BUR METEOROL,MELBOURNE,VIC 3001,AUSTRALIA. LOCKHEED ENGN & SCI CO,HAMPTON,VA 23666. NATL CTR ATMOSPHER RES,BOULDER,CO 80307. PENN STATE UNIV,DEPT METEOROL,UNIVERSITY PK,PA 16802. EUROPEAN CTR MEDIUM RANGE WEATHER FORECASTS,READING RG2 9AX,BERKS,ENGLAND. UNIV CALIF SAN DIEGO,SCRIPPS INST OCEANOG,CTR CLOUDS CHEM & CLIMATE,LA JOLLA,CA 92126. RP CESS, RD (reprint author), SUNY STONY BROOK,MARINE SCI RES CTR,INST TERR & PLANETARY ATMOSPHERES,STONY BROOK,NY 11794, USA. RI Garber, Donald/D-7427-2015; Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 NR 16 TC 335 Z9 344 U1 2 U2 39 PU AMER ASSOC ADVAN SCIENCE PI WASHINGTON PA 1333 H ST NW, WASHINGTON, DC 20005 SN 0036-8075 J9 SCIENCE JI Science PD JAN 27 PY 1995 VL 267 IS 5197 BP 496 EP 499 DI 10.1126/science.267.5197.496 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA QD403 UT WOS:A1995QD40300034 PM 17788783 ER PT J AU HSU, KJ DEMORE, WB AF HSU, KJ DEMORE, WB TI RATE CONSTANTS AND TEMPERATURE DEPENDENCES FOR THE REACTIONS OF HYDROXYL RADICAL WITH SEVERAL HALOGENATED METHANES, ETHANES, AND PROPANES BY RELATIVE RATE MEASUREMENTS SO JOURNAL OF PHYSICAL CHEMISTRY LA English DT Article ID TRANSITION-STATE-THEORY; F-SUBSTITUTED METHANES; GAS-PHASE REACTIONS; OH RADICALS; ATMOSPHERIC LIFETIMES; RATE COEFFICIENTS; KINETICS; CH3CCL3; CH3CHF2; HYDROCHLOROFLUOROCARBONS AB Rate constants of 15 OH reactions with halogen-substituted alkanes, C1 to C3, were studied using a relative rate technique in the temperature range 283-403 K. Compounds studied were CHF2Cl (22), CHF2Br (22B), CH3F (41), CH2F2 (32), CHF3 (23), CHClFCCl2F (122a), CHCl2CF3 (123), CHClFCF3 (124), CH3CF3 (143a), CH3CH2F (161), CF3CHFCF3 (227ea), CF3CH2CF3 (236fa), CF3CHFCHF2 (236ea), and CHF2CF2CH2F (245ca). Using CH4, CH3CCl3, CF3CF2H, and C2H6 as primary reference standards (JPL 92-20 rate constants), absolute rate constants are derived. Results are in good agreement with previous experimental results for six of the compounds studied, including CHF2Cl, CHF2Br, CH2F2, CH3CF3, CHFClCFCl2, and CF3CHFCF3. For the remainder the relative rate constants are lower than those derived from experiments in which OH loss was used to measure the reaction rate. Comparisons of the derived Arrhenius A factors with previous literature transition-state calculations(2,3) show order of magnitude agreement in most cases. However, the experimental A factors show a much closer proportionality to the number of H atoms in the molecule than is evident from the transition state calculations. For most of the compounds studied, an A factor of (8 +/- 3)E-13 cm(3)/(molecule s) per C-H bond is observed. A new measurement of the ratio k(CH3CCl3)/k(CH4) is reported that is in good agreement with previous data. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 39 TC 80 Z9 81 U1 1 U2 6 PU AMER CHEMICAL SOC PI WASHINGTON PA PO BOX 57136, WASHINGTON, DC 20037-0136 SN 0022-3654 J9 J PHYS CHEM-US JI J. Phys. Chem. PD JAN 26 PY 1995 VL 99 IS 4 BP 1235 EP 1244 DI 10.1021/j100004a025 PG 10 WC Chemistry, Physical SC Chemistry GA QD441 UT WOS:A1995QD44100025 ER PT J AU RUBINCAM, DP AF RUBINCAM, DP TI ASTEROID ORBIT EVOLUTION DUE TO THERMAL DRAG SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID SOLAR-SYSTEM; METEORITES; RADIATION; EARTH AB Thermal drag, a variant of the Yarkovsky effect, may act on small asteroids with sizes from a few meters to a few tens of meters. Yarkovsky thermal drag comes from an asteroid's absorbing sunlight in the visible and reradiating it in the infrared. Since the infrared photons have momentum, by action-reaction, they kick the asteroid when they leave its surface. The reradiation, which is asymmetric in latitude over the asteroid, gives a net force along the asteroid's pole. Due to the asteroid's thermal inertia, averaging this force over one orbital period produces a net drag if the spin axis has a component in the orbital plane. A regolith-free basaltic asteroid 60 m in radius can shrink its semimajor axis by 2 AU (the distance from the asteroid belt to the Earth) over the age of the solar system. Regolith-free iron asteroids evolve at about half the rate of basaltic ones. These calculations ignore planetary perturbations, collisions, erosion, etc. The rate of evolution varies inversely with the asteroid's radius for the size range considered here, so that smaller objects evolve faster than larger ones. The rate-radius relation fails for objects smaller than a few meters because the thermal skin depth becomes comparable to the size of the asteroid. Basaltic asteroids covered by regoliths more than a few centimeters deep evolve much more slowly than regolith-free ones. Thermal drag tends to circularize orbits. It can increase or decrease orbital inclinations. An object whose spin axis points in random directions over its lifetime displays little change in orbital inclination. Thermal drag appears to have little to do with the delivery of chondrites from the asteroid belt; the thermal drag timescale (10(8) years for meter-sized objects) is long compared with their cosmic ray exposure ages, and aphelia in the asteroid belt are not expected for mature thermal drag orbits. However, Yarkovsky thermal drag may act on the recently discovered near-Earth asteroids, which have radii of 10-30 m. Asteroid 1992 DA, for instance, might have its orbit shrunk by 0.1 AU in 3 x 10(7) years, removing it from an Earth-crossing orbit. The near-Earth asteroids also tend to have small to moderate orbital eccentricities, as expected for highly evolved thermal drag objects. However, the time needed to bring them in from the asteroid belt (about 10(9) years) is long compared with the collisional and dynamical lifetimes (both about 10(8) years) for Earth-crossing objects, arguing against their emplacement by thermal drag. RP RUBINCAM, DP (reprint author), NASA,GODDARD SPACE FLIGHT CTR,TERR PHYS LAB,GEODYNAM BRANCH,CODE 921,GREENBELT,MD 20771, USA. RI Rubincam, David/D-2918-2012 NR 31 TC 80 Z9 81 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-PLANET JI J. Geophys. Res.-Planets PD JAN 25 PY 1995 VL 100 IS E1 BP 1585 EP 1594 DI 10.1029/94JE02411 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA QF758 UT WOS:A1995QF75800006 ER PT J AU BURRIS, J HEAPS, W AF BURRIS, J HEAPS, W TI TEMPORAL VARIATIONS IN THE SPECTRAL OUTPUT OF A XENON FLUORIDE EXCIMER-LASER SO APPLIED OPTICS LA English DT Note DE EXCIMER LASER; REMOTE SENSING; LIDAR AB The behavior of a xenon fluoride excimer laser's spectral output as a function of the gas fill's age has been measured, and significant variations have been found. The output was preferentially shifted from the 348-nm band into the 351-nm band. RP BURRIS, J (reprint author), NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHER CHEM & DYNAM BRANCH,GREENBELT,MD 20771, USA. NR 2 TC 5 Z9 5 U1 0 U2 0 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 SN 0003-6935 J9 APPL OPTICS JI Appl. Optics PD JAN 20 PY 1995 VL 34 IS 3 BP 426 EP 427 PG 2 WC Optics SC Optics GA QC465 UT WOS:A1995QC46500006 PM 20963133 ER PT J AU BUOTE, DA TSAI, JC AF BUOTE, DA TSAI, JC TI THE RELIABILITY OF X-RAY CONSTRAINTS OF INTRINSIC CLUSTER SHAPES SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, CLUSTERS, GENERAL; X-RAYS, GALAXIES ID NONROTATING STELLAR-SYSTEMS; SHELL-ORBIT MODELS; SPHERICAL GALAXIES; ABELL CLUSTERS; COMA CLUSTER; DARK MATTER; HOT PLASMA; SUBSTRUCTURE; A2256; MASS AB Using the simulation of Katz & White (1993) we have tested the viability of X-ray analysis for constraining the intrinsic shapes of clusters of galaxies considering the effects of both substructure and steep temperature gradients. We restrict our analysis to the aggregate shapes of clusters on scales of r similar to 1-2 Mpc in order to reduce our sensitivity to subclustering in the core. For low redshifts (z less than or similar to 0.25) the X-ray method accurately measures the true ellipticity of the three-dimensional cluster dark matter provided the inclination of the cluster is known to within similar to 30 degrees; assuming the gas is isothermal adds only small errors to the derived shapes. At higher redshifts the X-ray method yields unreliable results since the gas does not trace the cluster gravitational potential. We proffer some necessary conditions for the reliability of X-ray methods characterized by both the amount of substructure in the X-ray surface brightness images and the shapes of the isophotes. We conclude that measurements of the aggregate shapes of clusters on scales r similar to 1-2 Mpc are insensitive to core substructure representing scales of a few hundred kpc. Therefore our results suggest that the X-ray measurements of aggregate cluster shapes by Fabricant, Rybicki, & Gorenstein (1984) & Buote & Canizares (1992) are valid provided that they do not suffer from serious projection effects. A substantial number of Abell clusters observed with the ROSAT PSPC will be amenable to X-ray shape analysis. C1 MIT,CTR SPACE RES 37241,CAMBRIDGE,MA 02139. NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. RP BUOTE, DA (reprint author), MIT,DEPT PHYS,77 MASSACHUSETTS AVE,CAMBRIDGE,MA 02139, USA. NR 55 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 JAN 20 PY 1995 VL 439 IS 1 BP 29 EP 41 DI 10.1086/175148 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QC786 UT WOS:A1995QC78600004 ER PT J AU RAKOS, KD SCHOMBERT, JM AF RAKOS, KD SCHOMBERT, JM TI COLOR EVOLUTION FROM Z=0 TO Z=1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, EVOLUTION; GALAXIES, PHOTOMETRY ID NARROW-BAND PHOTOMETRY; HIGH-REDSHIFT GALAXIES; ELLIPTICAL GALAXIES; DISTANT CLUSTERS; DISK GALAXIES; RICH CLUSTERS; POPULATION; SPECTROSCOPY; CATALOG; MODEL AB Rest frame Stromgren photometry (3500 Angstrom, 4100 Angstrom, 4750 Angstrom, and 5500 Angstrom) is presented for 509 galaxies in 17 rich clusters between z = 0 and z = 1 as a test of color evolution. Our observations confirm a strong, rest frame, Butcher-Oemler effect where the fraction of blue galaxies increases from 20% at z = 0.4 to 80% at z = 0.9. We also find that a majority of these blue cluster galaxies are composed of normal disk or post-starburst systems based on color criteria. When comparing our colors to the morphological results from HST imaging, we propose that the blue cluster galaxies are a population of late-type, low surface brightness objects which fade and are then destroyed by the cluster tidal field. After isolating the red objects from Butcher-Oemler objects, we have compared the mean color of these old, non-star-forming objects with spectral energy distribution models in the literature as a test for passive galaxy evolution in ellipticals. We find good agreement with single-burst models which predict a mean epoch of galaxy formation at z = 5. Tracing the red envelope for ellipticals places the earliest epoch of galaxy formation at z = 10. C1 CALTECH,JET PROP LAB,CTR INFRARED PROC & ANAL,PASADENA,CA 91125. RP RAKOS, KD (reprint author), UNIV VIENNA,INST ASTRON,TURKENSCHANZSTR 17,A-1180 VIENNA,AUSTRIA. NR 50 TC 133 Z9 134 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 1995 VL 439 IS 1 BP 47 EP 59 DI 10.1086/175150 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QC786 UT WOS:A1995QC78600006 ER PT J AU TEGLER, SC WEINTRAUB, DA RETTIG, TW PENDLETON, YJ WHITTET, DCB KULESA, CA AF TEGLER, SC WEINTRAUB, DA RETTIG, TW PENDLETON, YJ WHITTET, DCB KULESA, CA TI EVIDENCE FOR CHEMICAL-PROCESSING OF PRECOMETARY ICY GRAINS IN CIRCUMSTELLAR ENVIRONMENTS OF PRE-MAIN-SEQUENCE STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; DUST, EXTINCTION; INFRARED, STARS; ISM, INDIVIDUAL (TAURUS DARK CLOUD); ISM, MOLECULES; STARS, PRE-MAIN-SEQUENCE ID YOUNG STELLAR OBJECTS; TAURUS DARK CLOUDS; Z-CANIS MAJORIS; NEAR-INFRARED SPECTROPHOTOMETRY; TIME-DEPENDENT CHEMISTRY; HIGH-SPATIAL-RESOLUTION; DENSE MOLECULAR CLOUDS; FU-ORIONIS STARS; HL-TAURI; L1551 IRS-5 AB We report the detection of a broad absorption feature near 2166 cm(-1) in the spectrum of the Taurus cloud source Elias 18. This pre-main-sequence source is the second in Taurus, the third in our survey, and the fifth known in the sky to show the broad 2166 cm(-1) absorption feature. Of equal importance, this feature is not seen toward several other embedded sources in our survey, nor is it seen toward the source Elias 16, located behind the Taurus cloud. Laboratory experiments with interstellar ice analogs show that such a feature is associated with a complex C=N containing compound [called X(C=N)] that results from high-energy processing (ultraviolet irradiation or ion bombardment) of simple ice components into more complex, organic components. We find a nonlinear anticorrelation between the abundance of X(C=N) and frozen CO in nonpolar lattices. We find no correlation between the abundance of X(C=N) and frozen CO in polar lattices. Because the abundances of frozen CO and H2O are strongly correlated with each other and with visual extinction toward sources embedded in and located behind the Taurus molecular cloud, these ice components usually are associated with intracloud material. Our results indicate that X(C=N) molecules result from chemical processing of dust grains dominated by nonpolar icy mantles in the local environments of pre-main-sequence stars. Such processing of icy grains in the early solar system may be an important source of organic compounds observed in minor solar system bodies. The delivery of these organic compounds to the surface of the primitive Earth through comet impacts may have provided the raw materials for prebiotic chemistry. C1 VANDERBILT UNIV,DEPT PHYS & ASTRON,NASHVILLE,TN 37235. NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. RENSSELAER POLYTECH INST,DEPT PHYS,TROY,NY 12180. RP TEGLER, SC (reprint author), UNIV NOTRE DAME,DEPT PHYS & ASTRON,NOTRE DAME,IN 46556, USA. OI Whittet, Douglas/0000-0001-8539-3891 NR 78 TC 75 Z9 75 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 JAN 20 PY 1995 VL 439 IS 1 BP 279 EP 287 DI 10.1086/175171 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QC786 UT WOS:A1995QC78600027 ER PT J AU FORD, LA BAND, DL MATTESON, JL BRIGGS, MS PENDLETON, GN PREECE, RD PACIESAS, WS TEEGARDEN, BJ PALMER, DM SCHAEFER, BE CLINE, TL FISHMAN, GJ KOUVELIOTOU, C MEEGAN, CA WILSON, RB LESTRADE, JP AF FORD, LA BAND, DL MATTESON, JL BRIGGS, MS PENDLETON, GN PREECE, RD PACIESAS, WS TEEGARDEN, BJ PALMER, DM SCHAEFER, BE CLINE, TL FISHMAN, GJ KOUVELIOTOU, C MEEGAN, CA WILSON, RB LESTRADE, JP TI BATSE OBSERVATIONS OF GAMMA-RAY BURST SPECTRA .2. PEAK ENERGY EVOLUTION IN BRIGHT, LONG BURSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA RAYS, BURSTS; METHODS, DATA ANALYSIS ID STARS; PULSARS; MODEL AB We investigate spectral evolution in 37 bright, long gamma-ray bursts observed with the BATSE spectroscopy detectors. High-resolution spectra are characterized by the energy of the peak of nu F(n)u, and the evolution of this quantity is examined relative to the emission intensity. In most cases it is found that this peak energy either rises with or slightly precedes major intensity increases and softens for the remainder of the pulse. Interpulse emission is generally harder early in the burst. For bursts with multiple intensity pulses, later spikes tend to be softer than earlier ones, indicating that the energy of the peak of nu F(n)u is bounded by an envelope which decays with time. Evidence is found that bursts in which the bulk of the flux comes well after the event which triggers the instrument tend to show less peak energy variability and are not as hard as several bursts in which the emission occurs promptly after the trigger. Several recently proposed burst models are examined in light of these results and no qualitative conflicts with the observations presented here are found. C1 UNIV ALABAMA,HUNTSVILLE,AL 35899. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,GREENBELT,MD 20771. MISSISSIPPI STATE UNIV,MISSISSIPPI STATE,MS 39762. RP FORD, LA (reprint author), UNIV CALIF SAN DIEGO,CTR ASTROPHYS & SPACE SCI 0111,LA JOLLA,CA 92093, USA. OI Preece, Robert/0000-0003-1626-7335 NR 45 TC 213 Z9 219 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 1995 VL 439 IS 1 BP 307 EP 321 DI 10.1086/175174 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QC786 UT WOS:A1995QC78600030 ER PT J AU SCHLEGEL, EM BARRETT, PE DEJAGER, OC CHANMUGAM, G HUNTER, S MATTOX, J AF SCHLEGEL, EM BARRETT, PE DEJAGER, OC CHANMUGAM, G HUNTER, S MATTOX, J TI GAMMA-RAY EMISSION FROM CATACLYSMIC VARIABLES .1. THE COMPTON EGRET SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA RAYS, OBSERVATIONS; NOVAE, CATACLYSMIC VARIABLES; RADIATION MECHANISMS, NONTHERMAL; SURVEYS ID DOUBLE RADIO-SOURCES; BG CANIS-MINORIS; ACCRETION DISK; AE-AQUARII; PARTICLE-ACCELERATION; DEGENERATE STARS; GALACTIC PLANE; AM HERCULIS; MODEL; TEV AB We report the results of the first gamma-ray survey of cataclysmic variables (CVs) using observations obtained with the EGRET instrument on the Compton Observatory. We briefly describe the theoretical models that are applicable to gamma-ray emission from CVs. These models are particularly relevant to magnetic CVs containing asynchronously rotating white dwarfs. No magnetic CV was detected with an upper limit on the flux at 1 GeV of similar to 2 x 10(-8) cm(-2) s(-1), which corresponds to an upper limit on the gamma-ray luminosity of similar to 10(31) ergs s(-1), assuming a typical CV distance of 100 pc. C1 POTCHEFSTROOM UNIV CHRISTIAN HIGHER EDUC,DEPT PHYS,POTCHEFSTROOM 2520,SOUTH AFRICA. LOUISIANA STATE UNIV,DEPT PHYS & ASTRON,BATON ROUGE,LA 70803. RP SCHLEGEL, EM (reprint author), NASA,GODDARD SPACE FLIGHT CTR,GRO SCI SUPPORT CTR,CODE 668,GREENBELT,MD 20771, USA. RI Hunter, Stanley/D-2942-2012 NR 71 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 JAN 20 PY 1995 VL 439 IS 1 BP 322 EP 329 DI 10.1086/175175 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QC786 UT WOS:A1995QC78600031 ER PT J AU HOWELL, SB SZKODY, P CANNIZZO, JK AF HOWELL, SB SZKODY, P CANNIZZO, JK TI TREMENDOUS OUTBURST AMPLITUDE DWARF NOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCRETION, ACCRETION DISKS; BINARIES, CLOSE; NOVAE, CATACLYSMIC VARIABLES ID HIGH GALACTIC LATITUDE; FAINT CATACLYSMIC VARIABLES; TIME-RESOLVED PHOTOMETRY; URSAE MAJORIS STARS; LONG-TERM BEHAVIOR; ACCRETION DISKS; CLOSE BINARIES; PG 0134+070; SS-CYGNI; MODEL AB For many years, observers have noted the existence of a number of tremendous outburst amplitude dwarf novae. We present a summary of the known observational parameters for these exceptional systems. They show outburst amplitudes of 6-10 mag, have rare outbursts (interoutburst times being months to decades), and only seem to exist in dwarf novae with short orbital periods. We calculate new accretion disk models which can reproduce their outburst behavior very well. It appears that these dwarf novae have low mass transfer rates at minimum, and the viscosity during quiescence is about 10 times smaller than for other dwarf novae. Their relation to SU UMa stars is discussed. C1 UNIV WASHINGTON,DEPT ASTRON,SEATTLE,WA 98195. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP HOWELL, SB (reprint author), PLANETARY SCI INST,620 N 6TH AVE,TUCSON,AZ 85705, USA. NR 84 TC 113 Z9 114 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 JAN 20 PY 1995 VL 439 IS 1 BP 337 EP 345 DI 10.1086/175177 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QC786 UT WOS:A1995QC78600033 ER PT J AU KASTNER, SO BHATIA, AK AF KASTNER, SO BHATIA, AK TI THE NEUTRAL OXYGEN SPECTRUM .2. PUMPING BY HYDROGEN LYMAN-BETA UNDER THE OPTICALLY THIN CONDITION - A FIRST APPLICATION TO THE CLASSICAL NOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC PROCESSES; NOVAE, CATACLYSMIC VARIABLES ID SPECTROSCOPIC OBSERVATIONS; PW-VULPECULAE; EVOLUTION; SUN; STARS AB A calculation, employing a detailed model of neutral oxygen, is carried out to give fluorescent line intensities expected in a long-proposed photoexcitation by accidental resonance (PAR) process in which hydrogen Lyman-beta photoexcites the oxygen spectrum. The results pertain to the optically thin case but provide an upper limit to the fluorescent intensities which can be attained. They are applied to analyze line ratios involving the strong 8446 Angstrom line observed in classical novae during the diffusion-enhanced and Orion phases. Operation of the PAR process in the novae is verified. It is found that photoexcitation rates in the ejecta reach values greater than 10(-1) s(-1), corresponding to hydrogen Lyman-beta radiation field intensities greater than 1250 ergs cm(-1) s(-1) sr(-1). C1 NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, GREENBELT, MD 20771 USA. RP MATH SCI CONSULTANTS INC, 1-A RIDGE RD, GREENBELT, MD 20770 USA. NR 45 TC 20 Z9 20 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 1995 VL 439 IS 1 BP 346 EP 356 DI 10.1086/175178 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QC786 UT WOS:A1995QC78600034 ER PT J AU SNOWDEN, SL BURROWS, DN SANDERS, WT ASCHENBACH, B PFEFFERMANN, E AF SNOWDEN, SL BURROWS, DN SANDERS, WT ASCHENBACH, B PFEFFERMANN, E TI ROSAT OBSERVATIONS OF THE ERIDANUS SOFT-X-RAY ENHANCEMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE DIFFUSE RADIATION; SUPERNOVA REMNANTS; X-RAYS, ISM ID EXPANDING SHELL; FILAMENTS; NEBULA; CLOUD AB We present maps of the Eridanus soft X-ray enhancement made from the ROSAT all-sky survey data. The maps are in two energy bands: 1/4 keV (0.12-0.284 keV at 10% response, the ROSAT R1 and R2 bands), and 3/4 keV (0.47-1.20 keV at 10% response, the ROSAT R4 and R5 bands). The entire enhancement spans a total of similar to 35 degrees in Galactic latitude and similar to 20 degrees in Galactic longitude, centered at l similar to 200 degrees, b similar to -32 degrees. While the higher spatial resolution of the ROSAT data reveals a pattern of detailed anticorrelations with 100 mu m intensity that was not evident in the HEAO 1 or earlier data, the basic morphology found in previous maps of this enhancement is confirmed. The ROSAT data also clearly show that the X-ray enhancement continues up to the Orion region in the 3/4 keV band, confirming the structure suggested by the Wisconsin sky survey maps. The ROSAT data are consistent with the interpretation of Reynolds and Ogden and Burrows et al, that this enhancement, the higher temperature-component of Burrows et al., is generated for the most part by several-million-degree gas filling a huge interstellar cavity. However, we interpret the low-temperature component discussed by Burrows et al. as part of a more distant large scale (greater than or similar to 30 degrees) diffuse background enhancement. The part of this softer X-ray enhancement examined here appears to be produced by million degree gas in the galactic halo, and is therefore unlikely to be an isolated bubble as suggested by Burrows et al, on the basis of lower resolution HEAO 1 data. C1 PENN STATE UNIV,DEPT ASTRON & ASTROPHYS,UNIVERSITY PK,PA 16802. UNIV WISCONSIN,DEPT PHYS,MADISON,WI 53706. NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY PHYS LAB,GREENBELT,MD 20771. RP SNOWDEN, SL (reprint author), MAX PLANCK INST EXTRATERR PHYS,D-85748 GARCHING,GERMANY. RI Snowden, Steven/D-5292-2012 NR 30 TC 37 Z9 37 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 1995 VL 439 IS 1 BP 399 EP 404 DI 10.1086/175182 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QC786 UT WOS:A1995QC78600038 ER PT J AU GAINES, EE CHENETTE, DL IMHOF, WL JACKMAN, CH WINNINGHAM, JD AF GAINES, EE CHENETTE, DL IMHOF, WL JACKMAN, CH WINNINGHAM, JD TI RELATIVISTIC ELECTRON-FLUXES IN MAY-1992 AND THEIR EFFECT ON THE MIDDLE ATMOSPHERE SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID PRECIPITATION AB Enhancements in the fluxes of relativistic electrons trapped within the Earth's magnetosphere have been measured by the high-energy particle spectrometer, part of the particle environment monitor on the upper atmosphere research satellite (UARS). The largest increase in the electron fluxes with energies greater than 1 MeV observed on UARS from October 1991 through July 1994 was in early May 1992. The fluxes of trapped electrons in the drift loss cone and locally precipitating electrons showed differing buildup and decay rates as a function of invariant latitude. Increases of more than 2 orders of magnitude were observed in drift loss cone fluxes at magnetic latitudes of 40 degrees-66 degrees and in precipitating fluxes from 48 degrees to 66 degrees. The energy flux contained in the most intense local precipitation observed was similar to 0.1 erg cm(-2) s(-1) entering the atmosphere and creating up to 1000 ion pairs cm(-3) s(-1) at 55-km altitude. The daily averaged energy flux from directly precipitating electrons with energies >1 MeV deposited >10(20) erg d(-1) worldwide into the atmosphere for the period May 12-21, 1992, producing >10(31) odd nitrogen molecules below 60-km altitude. C1 NASA, GODDARD SPACE FLIGHT CTR, GREENBELT, MD 20771 USA. SW RES INST, SAN ANTONIO, TX USA. RP GAINES, EE (reprint author), LOCKHEED PALO ALTO RES LABS, DEPT 92120, BLDG, 252, 3251 HANOVER ST, PALO ALTO, CA 94304 USA. RI Jackman, Charles/D-4699-2012 NR 14 TC 37 Z9 37 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JAN 20 PY 1995 VL 100 IS D1 BP 1027 EP 1033 DI 10.1029/94JD02615 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QF627 UT WOS:A1995QF62700003 ER PT J AU HERVIG, ME RUSSELL, JM GORDLEY, LL DANIELS, J DRAYSON, SR PARK, JH AF HERVIG, ME RUSSELL, JM GORDLEY, LL DANIELS, J DRAYSON, SR PARK, JH TI AEROSOL EFFECTS AND CORRECTIONS IN THE HALOGEN OCCULTATION EXPERIMENT SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SULFURIC-ACID; DROPLETS; CLOUDS; GROWTH AB The eruptions of Mt. Pinatubo in June 1991 increased stratospheric aerosol loading by a factor of 30, affecting chemistry, radiative transfer, and remote measurements of the stratosphere. The Halogen Occultation Experiment instrument on board UARS makes measurements globally for inferring profiles of NO2, H2O, O-3, HF, HC1, CH4, NO, and temperature in addition to aerosol extinction at five wavelengths. Understanding and removing the aerosol extinction is essential for obtaining accurate retrievals from the radiometer channels of NO2, H2O and O-3 in the lower stratosphere since these measurements are severely affected by contaminant aerosol absorption. If ignored, aerosol absorption in the radiometer measurements is interpreted as additional absorption by the target gas, resulting in anomalously large mixing ratios. To correct the radiometer measurements for aerosol effects, a retrieved aerosol extinction profile is extrapolated to the radiometer wavelengths and then included as continuum attenuation. The sensitivity of the extrapolations to size distribution and composition is small for certain wavelength combinations, reducing the correction uncertainty. The aerosol corrections extend the usable range of profiles retrieved from the radiometer channels to the tropopause with results that agree well with correlative measurements. In situations of heavy aerosol loading, errors due to aerosol in the retrieved mixing ratios are reduced to values of about 15, 25, and 60% in H2O, O-3, and NO2, respectively, levels that are much less than the correction magnitude. C1 GATS INC, HAMPTON, VA USA. NASA, LANGLEY RES CTR, HAMPTON, VA 23665 USA. UNIV MICHIGAN, ANN ARBOR, MI 48109 USA. RI Daniel, John/D-9324-2011 NR 16 TC 48 Z9 51 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JAN 20 PY 1995 VL 100 IS D1 BP 1067 EP 1079 DI 10.1029/94JD02143 PG 13 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QF627 UT WOS:A1995QF62700006 ER PT J AU LIAO, XH ROSSOW, WB RIND, D AF LIAO, XH ROSSOW, WB RIND, D TI COMPARISON BETWEEN SAGE-II AND ISCCP HIGH-LEVEL CLOUDS .1. GLOBAL AND ZONAL MEAN CLOUD AMOUNTS SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; CIRRUS CLOUDS; STRATOSPHERIC AEROSOL; SATELLITE; DISTRIBUTIONS; CLIMATOLOGY; STATISTICS; RESOLUTION; FIELDS; COVER AB Global high-level clouds identified in Stratospheric Aerosol and Gas Experiment II (SAGE II) occultation measurements for January and July in the period 1985 to 1990 are compared with near-nadir-looking observations from the International Satellite Cloud Climatology Project(ISCCP). Global and zonal mean high-level cloud amounts from the two data sets agree very well, if clouds with layer extinction coefficients of <0.008 km(-1) at 1.02 mu m wavelength are removed from the SAGE II results and all detected clouds are interpreted to have an average horizontal size of about 75 km along the 200 km transmission path length of the SAGE II observations. The SAGE II results are much more sensitive to variations of assumed cloud size than to variations of detection threshold. The geographical distribution of cloud fractions shows good agreement, but systematic regional differences also indicate that the average cloud size varies somewhat among different climate regimes. The more sensitive SAGE II results show that about one third of all high-level clouds are missed by ISCCP but that these clouds have very low optical thicknesses (<0.1 at 0.6 mu m wavelength). SAGE II sampling error in monthly zonal cloud fraction is shown to produce no bias, to be less than the intraseasonal natural variability, but to be comparable with the natural variability at longer time scales. RP LIAO, XH (reprint author), NASA, GODDARD INST SPACE STUDIES, SCI SYST & APPLICAT INC, 2880 BROADWAY, NEW YORK, NY 10025 USA. RI Rossow, William/F-3138-2015 NR 28 TC 89 Z9 91 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JAN 20 PY 1995 VL 100 IS D1 BP 1121 EP 1135 DI 10.1029/94JD02429 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QF627 UT WOS:A1995QF62700010 ER PT J AU LIAO, XH ROSSOW, WB RIND, D AF LIAO, XH ROSSOW, WB RIND, D TI COMPARISON BETWEEN SAGE-II AND ISCCP HIGH-LEVEL CLOUDS .2. LOCATING CLOUD TOPS SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID STRATOSPHERIC AEROSOL; SATELLITE; RESOLUTION AB A comparison is made of the vertical distribution of high-level cloud tops derived from the Stratospheric Aerosol and Gas Experiment II (SAGE II) occultation measurements and from the International Satellite Cloud Climatology Project (ISCCP) for all Julys and Januarys in 1985 to 1990. The results suggest that ISCCP overestimates the pressure of high-level clouds by up to 50-150 mbar, particularly at low latitudes. This is caused by the frequent presence of clouds with diffuse tops (>50% time when cloudy events are observed). The averaged vertical extent of the diffuse top is about 1.5 km. At midlatitudes where the SAGE II and ISCCP cloud top pressure agree best, clouds with distinct tops reach a maximum relative proportion of the total level cloud amount (about 30-40%), and diffuse-topped clouds are reduced to their minimum(30-40%). The ISCCP-defined cloud top pressure should be regarded not as the material physical height of the clouds but as the level which emits the same infrared radiance as observed. SAGE II and ISCCP cloud top pressures agree for clouds with distinct tops. There is also an indication that the cloud top pressures of optically thin clouds not overlying thicker clouds are poorly estimated by ISCCP at middle latitudes. The average vertical extent of these thin clouds is about 2.5 km. RP LIAO, XH (reprint author), NASA, GODDARD INST SPACE STUDIES, SCI SYST & APPLICAT INC, 2880 BROADWAY, NEW YORK, NY 10025 USA. RI Rossow, William/F-3138-2015 NR 24 TC 50 Z9 52 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JAN 20 PY 1995 VL 100 IS D1 BP 1137 EP 1147 DI 10.1029/94JD02430 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QF627 UT WOS:A1995QF62700011 ER PT J AU ZHANG, YC ROSSOW, WB LACIS, AA AF ZHANG, YC ROSSOW, WB LACIS, AA TI CALCULATION OF SURFACE AND TOP OF ATMOSPHERE RADIATIVE FLUXES FROM PHYSICAL QUANTITIES BASED ON ISCCP DATA SETS .1. METHOD AND SENSITIVITY TO INPUT DATA UNCERTAINTIES SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID VAPOR ABSORPTION-COEFFICIENTS; GENERAL-CIRCULATION MODELS; INCIDENT SOLAR-RADIATION; WATER-VAPOR; INFRARED CONTINUUM; SATELLITE DATA; RADIANCE MEASUREMENTS; OPTICAL-PROPERTIES; BUDGET EXPERIMENT; GLOBAL RADIATION AB Upwelling and downwelling, shortwave and longwave radiative fluxes are calculated at the top of the atmosphere and at the surface using a complete radiative transfer model and observations of the physical properties of the surface, atmosphere, and clouds based on the International Satellite Cloud Climatology Project (ISCCP) data sets. Results are obtained every three hours over the whole globe for every third month from April 1985 to January 1989. Sensitivity studies are conducted to assess the uncertainties in calculated fluxes caused by the estimated uncertainties in the measurement or specification of the input quantities. Except in the polar regions, uncertainties in cloud properties are no longer the predominant source of radiative flux uncertainty, even at the surface; rather they produce uncertainties similar in magnitude to those caused by atmospheric and surface properties. The largest uncertainty in upwelling shortwave (SW) fluxes (approximate to 10 - 15 W/m(2), regional daily mean) is caused by uncertainties in land surface albedo, whereas the largest uncertainty in downwelling SW at the surface (approximate to 5 - 10 W/m(2), regional daily mean) is related to cloud detection errors. The uncertainty of upwelling longwave (LW) fluxes (approximate to 10 - 20 W/m(2), regional daily mean) depends on the accuracy of the surface temperature for the surface LW fluxes and the atmospheric temperature for the top of atmosphere LW fluxes. The dominant source of uncertainty in downwelling LW fluxes at the surface (approximate to 10 - 15 W/m(2)) is uncertainty in atmospheric temperature and, secondarily, atmospheric humidity; clouds play little role except in the polar regions. The uncertainties of the individual flux components and the total net fluxes are largest over land (15 - 20 W/m(2)) because of uncertainties in surface albedo (especially its spectral dependence) and surface temperature and emissivity (including its spectral dependence). Clouds are the most important modulator of the SW fluxes, but over land areas, uncertainties in net SW at the surface depend almost as much on uncertainties in surface albedo. Although atmospheric and surface temperature variations cause larger LW flux variations, the most notable feature of the net LW fluxes is the changing relative importance of clouds and water vapor with latitude. Uncertainty in individual flux values is dominated by sampling effects because of large natural variations, but uncertainty in monthly mean fluxes is dominated by bias errors in the input quantities. RP COLUMBIA UNIV, NASA, GODDARD INST SPACE STUDIES, 2880 BROADWAY, NEW YORK, NY 10025 USA. RI Lacis, Andrew/D-4658-2012; Rossow, William/F-3138-2015 NR 85 TC 182 Z9 188 U1 5 U2 18 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JAN 20 PY 1995 VL 100 IS D1 BP 1149 EP 1165 DI 10.1029/94JD02747 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QF627 UT WOS:A1995QF62700012 ER PT J AU ROSSOW, WB ZHANG, YC AF ROSSOW, WB ZHANG, YC TI CALCULATION OF SURFACE AND TOP OF ATMOSPHERE RADIATIVE FLUXES FROM PHYSICAL QUANTITIES BASED ON ISCCP DATA SETS .2. VALIDATION AND FIRST RESULTS SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID BUDGET EXPERIMENT; SOLAR IRRADIANCE; DIURNAL VARIABILITY; SATELLITE DATA; SEASONAL-VARIATION; CLIMATE RESEARCH; CLOUD VARIATIONS; REGIONAL CLOUD; MODEL; ERBE AB We use global, multiyear observations of the properties of clouds, the atmosphere, and the surface to calculate global shortwave (SW) and longwave (LW) fluxes at the top of the atmosphere and at the surface at a resolution of 280 km and 3 hours for every third month from April 1985 to January 1989. Our validation studies suggest that the specification of cloud effects is no longer the dominant uncertainty in reconstructing the radiative fluxes at the top of atmosphere and at the surface. Rather cloud property uncertainties are now roughly equal contributors to the flux uncertainty, along with surface and atmospheric properties. Overall, the estimated uncertainties in regional, monthly mean fluxes, based on comparisons to more direct measurements, are as follows: for S up arrow(t), 11 W/m(2) bias with a rms scatter of 7 W/m(2) (the bias may be as little as 5 W/m(2)); for L up arrow(t), -1 W/m(2) bias with a rms scatter of 4 W/m(2); for S down arrow(s), 10 - 20 W/m(2) bias with a rms scatter of 10 - 15 W/m(2) (the bias may only be approximate to 10 W/m(2) caused by aerosols); for ST, approximate to 3 W/m(2) bias with a rms scatter of 10 W/m(2); for L down arrow(s), probably < 15 W/m(2) bias (but with variable sign) with a rms scatter of 15 W/m(2) (bias and scatter depend most on atmospheric temperature uncertainties); and for LT less than or similar to 12 W/m(2) and < 24 W/m(2) for combined bias and scatter over oceans and land, respectively (very sensitive to surface temperature determinations). The resulting SW and LW flux data sets suggest the following conclusions: (1) The net SW heating of Earth appears predominantly at the surface, whereas the net LW cooling arises predominantly from the atmosphere. The net cooling effect of clouds on top of atmospheric radiation appears primarily at the surface rather than in the atmosphere. (2) Clouds have almost no net effect on the global mean radiation balance of the atmosphere, but they enhance the latitudinal gradient in the LW cooling and reinforce the radiative forcing for the mean atmospheric circulation. Clouds act to mute seasonal contrasts however. (3) Clouds enhance the land-ocean contrasts of the atmospheric cooling, reinforcing the growth of standing eddy motions; but reduce land-ocean contrasts of the surface heating. C1 COLUMBIA UNIV, DEPT APPL PHYS, NEW YORK, NY 10027 USA. RP ROSSOW, WB (reprint author), NASA, GODDARD INST SPACE STUDIES, 2880 BROADWAY, NEW YORK, NY 10025 USA. RI Rossow, William/F-3138-2015 NR 81 TC 213 Z9 217 U1 3 U2 15 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JAN 20 PY 1995 VL 100 IS D1 BP 1167 EP 1197 DI 10.1029/94JD02746 PG 31 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QF627 UT WOS:A1995QF62700013 ER PT J AU MERRITT, DA HAYES, JM MARIAS, DJD AF MERRITT, DA HAYES, JM MARIAS, DJD TI CARBON ISOTOPIC ANALYSIS OF ATMOSPHERIC METHANE BY ISOTOPE-RATIO-MONITORING GAS-CHROMATOGRAPHY MASS-SPECTROMETRY SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID HYDROCARBONS; HYDROGEN; ORIGINS AB Less than 15 min are required for the determination of delta(13)C(PDB) With a precision of 0.2%(0) (1 delta, single measurement) in 5-mL samples of air containing CH4 at natural levels (1.7 ppm). An analytical system including a sample-introduction unit incorporating a preparative gas chromatograph (GC) column for separation of CH4 from N-2, O-2, and Ar is described. The 15-min procedure includes time for operation of that system, high-resolution chromatographic separation of the CH,, on-line combustion and purification of the products, and isotopic calibration. Analyses of standards demonstrate that systematic errors are absent and that there is no dependence of observed values of delta on sample size. For samples containing 100 ppm or more CH4, preconcentration is not required and the analysis time is less than 5 min. The system utilizes a commercially available, high-sensitivity isotope-ratio mass spectrometer. For optimal conditions of sample handling and combustion, performance of the system is within a factor of 2 of the shot-noise limit. The potential exists therefore for analysis of samples as small as 15 pmol CH4 With a standard deviation of 20 000 km s(-1), and for NGC 5548 (z = 0.017) that the line is at 6.15 keV with a FWHM of > 35 000 km s(-1). The line centroids are shifted by < 0.2 keV with respect to the expected rest-frame energy of a fluorescent line from cold material. The widths are considerably larger than the full widths of the optical or UV lines found in these objects of similar to 15 000 km s(-1). The intrinsic line profiles are not well determined, but are consistent with models of lines from the inner regions (< 100 Schwarzschild radii) of accretion discs inclined at similar to 20 degrees-30 degrees. The discovery of such broad lines now opens up the immediate surroundings of accreting black holes for detailed study. C1 UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 0HA,ENGLAND. NAGOYA UNIV,DEPT ASTROPHYS,NAGOYA,AICHI 464,JAPAN. INST PHYS & CHEM RES,WAKO,SAITAMA 35101,JAPAN. INST SPACE & ASTRONAUT SCI,SAGAMIHARA,KANAGAWA 229,JAPAN. RP MUSHOTZKY, RF (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,CODE 666,GREENBELT,MD 20771, USA. NR 24 TC 71 Z9 71 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 JAN 15 PY 1995 VL 272 IS 2 BP L9 EP L12 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QC748 UT WOS:A1995QC74800002 ER PT J AU CAMPBELL, S YEH, PC GU, C HE, QB AF CAMPBELL, S YEH, PC GU, C HE, QB TI FIDELITY OF IMAGE-RESTORATION BY PARTIAL PHASE-CONJUGATION THROUGH MULTIMODE FIBERS SO OPTICS COMMUNICATIONS LA English DT Article ID POLARIZATION AB We investigate the fidelity of image restoration under conditions of partial phase conjugation through a random medium. For the first time, the conjugated image-to-background ratio is experimentally measured as an evaluation of the phase conjugate mirror's fidelity. Output signal-to-noise ratio and information throughput are also considered as functions of aperture limitations at the various planes of the optical system. C1 PENN STATE UNIV,DEPT ELECT ENGN,UNIVERSITY PK,PA 16802. CALTECH,JET PROP LAB,PASADENA,CA 91109. RP CAMPBELL, S (reprint author), UNIV CALIF SANTA BARBARA,DEPT ELECT & COMP ENGN,SANTA BARBARA,CA 93106, USA. RI Yeh, Pochi/A-2109-2010 NR 10 TC 6 Z9 6 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0030-4018 J9 OPT COMMUN JI Opt. Commun. PD JAN 15 PY 1995 VL 114 IS 1-2 BP 50 EP 56 DI 10.1016/0030-4018(94)00522-V PG 7 WC Optics SC Optics GA QD108 UT WOS:A1995QD10800009 ER PT J AU DOWNIE, JD AF DOWNIE, JD TI OPTICAL LOGARITHMIC TRANSFORMATION OF SPECKLE IMAGES WITH BACTERIORHODOPSIN FILMS SO OPTICS LETTERS LA English DT Article AB The application of logarithmic transformations to speckle images is sometimes desirable in converting the speckle noise distribution into an additive, constant-variance noise distribution. The optical transmission properties of some bacteriorhodopsin films are well suited to implement such a transformation optically in a parallel fashion. I present experimental results of the optical conversion of a speckle image into a transformed image with signal-independent noise statistics, using the real-time photochromic properties of bacteriorhodopsin. The original and transformed noise statistics are confirmed by histogram analysis. RP DOWNIE, JD (reprint author), NASA,AMES RES CTR,M-S 269-3,MOFFETT FIELD,CA 94035, USA. NR 8 TC 4 Z9 5 U1 0 U2 0 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD JAN 15 PY 1995 VL 20 IS 2 BP 201 EP 203 DI 10.1364/OL.20.000201 PG 3 WC Optics SC Optics GA QD368 UT WOS:A1995QD36800030 PM 19859134 ER PT J AU LAMOURI, A KRAINSKY, IL PETUKHOV, AG LAMBRECHT, WRL SEGALL, B AF LAMOURI, A KRAINSKY, IL PETUKHOV, AG LAMBRECHT, WRL SEGALL, B TI UNOCCUPIED ELECTRONIC RESONANCES OF SC ADSORBED ON W(001) BY K-RESOLVED INVERSE-PHOTOEMISSION SO PHYSICAL REVIEW B LA English DT Article ID WORK-FUNCTION; TUNGSTEN; SURFACE; CATHODES; SPECTROSCOPY; STATES; BARIUM; NICKEL; BA C1 NASA, LEWIS RES CTR, CLEVELAND, OH 44135 USA. RP CASE WESTERN RESERVE UNIV, DEPT PHYS, CLEVELAND, OH 44106 USA. RI Lambrecht, Walter/O-1083-2016 NR 30 TC 4 Z9 4 U1 0 U2 2 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 EI 1550-235X J9 PHYS REV B JI Phys. Rev. B PD JAN 15 PY 1995 VL 51 IS 3 BP 1803 EP 1808 DI 10.1103/PhysRevB.51.1803 PG 6 WC Physics, Condensed Matter SC Physics GA QH790 UT WOS:A1995QH79000048 ER PT J AU IWAMOTO, N QIN, LT FUKUGITA, M TSURUTA, S AF IWAMOTO, N QIN, LT FUKUGITA, M TSURUTA, S TI NEUTRINO MAGNETIC-MOMENT AND NEUTRON-STAR COOLING SO PHYSICAL REVIEW D LA English DT Article ID X-RAY; GAUGE THEORIES; ROSAT OBSERVATIONS; GAMMA-RAYS; PULSAR; PSR-0656+14; EMISSION; GEMINGA; MATTER; MUON C1 KYOTO UNIV,YUKAWA INST THEORET PHYS,KYOTO 60601,JAPAN. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB ES65,HUNTSVILLE,AL 35812. MONTANA STATE UNIV,DEPT PHYS,BOZEMAN,MT 59717. INST ADV STUDY,PRINCETON,NJ 08540. RP IWAMOTO, N (reprint author), UNIV TOLEDO,DEPT PHYS & ASTRON,TOLEDO,OH 43606, USA. NR 42 TC 8 Z9 8 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 1995 VL 51 IS 2 BP 348 EP 352 DI 10.1103/PhysRevD.51.348 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA QE570 UT WOS:A1995QE57000011 ER PT J AU LIDSEY, JE WAGA, I AF LIDSEY, JE WAGA, I TI ANDANTE REGIME OF SCALAR FIELD-DYNAMICS IN THE CHAOTIC INFLATIONARY UNIVERSE SO PHYSICAL REVIEW D LA English DT Article ID POWER-LAW INFLATION; EXPONENTIAL POTENTIALS; PERTURBATIONS; MODELS; FLUCTUATIONS C1 FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. FED UNIV RIO DE JANEIRO,INST FIS,BR-21943 RIO JANEIRO,BRAZIL. RI Waga, Ioav/B-6288-2014 NR 39 TC 5 Z9 5 U1 0 U2 1 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 1995 VL 51 IS 2 BP 444 EP 449 DI 10.1103/PhysRevD.51.444 PG 6 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA QE570 UT WOS:A1995QE57000019 ER PT J AU GENTHON, C ARMENGAUD, A AF GENTHON, C ARMENGAUD, A TI GCM SIMULATIONS OF ATMOSPHERIC TRACERS IN THE POLAR LATITUDES - SOUTH-POLE (ANTARCTICA) AND SUMMIT (GREENLAND) CASES SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article; Proceedings Paper CT International Symposium on the Ecological Effects of Arctic Airborne Contaminants CY OCT 04-08, 1993 CL REYKJAVIK, ICELAND SP US EPA, NORDIC COUNCIL MINISTERS, ICELAND MINST ENVIRONM, NORDIC AIR & OCEAN GRP, INDIAN & NO AFFAIRS CANADA ARCTIC ENVIRONM STRATEGY, US DEPT STATE, USA, COLD REG RES & ENGN LAB, NATL SCI FDN US, DIV POLAR PROGRAMS, MINIST ENVIRONM, FINLAND, SWEDISH MINIST ENVIRONM & NAT RESOURCES, BOWLING GREEN STATE UNIV, UNIV ALASKA, GEOPHYS INST, FAIRBANKS DE GCM; AEROSOLS; RADIOACTIVE TRACERS; ANTARCTICA; GREENLAND ID GENERAL-CIRCULATION MODEL; DESERT DUST; AEROSOLS AB Simulation results from two global atmospheric tracer/climate models in the interior of the two major ice sheets at high northern and southern latitudes are presented and discussed. The models are based on two existing general circulation models (GCMs) of the atmosphere, complemented with tracer formulations (sources, transport, mixing, deposition, etc.). The seasonal and shorter term variability of desert dust, sea salt, Rn-222, Pb-210, and Be-7 has been studied at the South Pole in Antarctica and at Summit in Greenland. This choice of tracers and test regions serves to focus on the interactions between atmospheric parameters (e.g. the strong and durable surface inversions characteristic of the ice sheets) and tracers, and to limit other influences such as source variability and chemistry. Comparison with available observations is not consistently favorable. Short-term variability in the atmosphere (Rn-222 and Pb-210) appears qualitatively reasonable. Seasonal cycles are in some instances opposite to those observed, and mean deposition is clearly too high. The coarseness of model resolution at the high latitudes and the difficulty of setting up efficient formulations for microphysical tracer processes (e.g. dry and wet deposition) are major sources of problems. If these obstacles are overcome, the combined tracer/climate modelling approach can offer quantitative interpretation of the observed features of atmospheric contaminants, or sensitive tests of GCM simulated atmospheric circulation. C1 NASA, GODDARD INST SPACE STUDIES, NEW YORK, NY 10025 USA. RP GENTHON, C (reprint author), LAB GLACIOL & GEOPHYS ENVIRONM, CNRS, BP96, F-38402 ST MARTIN DHERES, FRANCE. NR 33 TC 7 Z9 7 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD JAN 15 PY 1995 VL 160-61 BP 101 EP 116 DI 10.1016/0048-9697(95)04348-5 PG 16 WC Environmental Sciences SC Environmental Sciences & Ecology GA QD143 UT WOS:A1995QD14300011 ER PT J AU PUESCHEL, RF KINNE, SA AF PUESCHEL, RF KINNE, SA TI PHYSICAL AND RADIATIVE PROPERTIES OF ARCTIC ATMOSPHERIC AEROSOLS SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article; Proceedings Paper CT International Symposium on the Ecological Effects of Arctic Airborne Contaminants CY OCT 04-08, 1993 CL REYKJAVIK, ICELAND SP US EPA, NORDIC COUNCIL MINISTERS, ICELAND MINST ENVIRONM, NORDIC AIR & OCEAN GRP, INDIAN & NO AFFAIRS CANADA ARCTIC ENVIRONM STRATEGY, US DEPT STATE, USA, COLD REG RES & ENGN LAB, NATL SCI FDN US, DIV POLAR PROGRAMS, MINIST ENVIRONM, FINLAND, SWEDISH MINIST ENVIRONM & NAT RESOURCES, BOWLING GREEN STATE UNIV, UNIV ALASKA, GEOPHYS INST, FAIRBANKS DE LIGHT EXTINCTION; CLIMATE; AEROSOLS; SULFURIC ACID; SOOT ID STRATOSPHERIC AEROSOLS; PARTICULATE CARBON; LIGHT-ABSORPTION; SOLAR-RADIATION; EL CHICHON; CLIMATE; HAZE; PARTICLES; SULFATE; SOOT AB Atmospheric aerosols sampled in the Arctic Basin by impactors have been analyzed for total aerosol and its black carbon fraction. The mass of black carbon aerosol in the lower troposphere is 1% (1 g black carbon in 100 g total aerosol), reduced to one part in 10(4) in the stratosphere. The aerosol single scatter albedos vary between 1.0 in the stratosphere, currently dominated by high light scattering due to Pinatubo volcanic aerosol, and 0.94 in the lower troposphere. The aerosol has the potential to regionally warm the earth-atmosphere system because of the high surface albedo of snow-covered surfaces in the Arctic. RP PUESCHEL, RF (reprint author), NASA, AMES RES CTR, MS-254-4, MOFFETT FIELD, CA 94035 USA. NR 54 TC 14 Z9 15 U1 4 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD JAN 15 PY 1995 VL 160-61 BP 811 EP 824 DI 10.1016/0048-9697(95)04414-V PG 14 WC Environmental Sciences SC Environmental Sciences & Ecology GA QD143 UT WOS:A1995QD14300077 ER PT J AU COPI, CJ SCHRAMM, DN TURNER, MS AF COPI, CJ SCHRAMM, DN TURNER, MS TI BIG-BANG NUCLEOSYNTHESIS AND THE BARYON DENSITY OF THE UNIVERSE SO SCIENCE LA English DT Article ID METAL-DEFICIENT DWARFS; PRIMORDIAL NUCLEOSYNTHESIS; DARK-MATTER; GALACTIC HALO; IRAS GALAXIES; STARS; ABUNDANCES; BERYLLIUM; LITHIUM; ORIGIN AB For almost 30 years, the predictions of big-bang nucleosynthesis have been used to test the big-bang model to within a fraction of a second of the bang. The agreement between the predicted and observed abundances of deuterium, helium-3, helium-4, and lithium-7 confirms the standard cosmology model and allows accurate determination of the baryon density, between 1.7 x 10(-31) and 4.1 x 10(-31) grams per cubic centimeter (corresponding to about 1 to 15 percent of the critical density). This measurement of the density of ordinary matter is pivotal to the establishment of two dark-matter problems: (i) most of the baryons are dark, and (ii) if the total mass density is greater than about 15 percent of the critical density, as many determinations indicate, the bulk of the dark matter must be ''nonbaryonic,'' composed of elementary particles left from the earliest moments. C1 FERMILAB NATL ACCELERATOR LAB, NASA, FERMILAB ASTROPHYS CTR, BATAVIA, IL 60510 USA. UNIV CHICAGO, ENRICO FERMI INST, DEPT ASTRON & ASTROPHYS, CHICAGO, IL 60637 USA. RP COPI, CJ (reprint author), UNIV CHICAGO, DEPT PHYS, CHICAGO, IL 60637 USA. NR 84 TC 327 Z9 327 U1 0 U2 4 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JAN 13 PY 1995 VL 267 IS 5195 BP 192 EP 199 DI 10.1126/science.7809624 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA QB153 UT WOS:A1995QB15300023 PM 7809624 ER PT J AU HARPER, CL NYQUIST, LE BANSAL, B WIESMANN, H SHIH, CY AF HARPER, CL NYQUIST, LE BANSAL, B WIESMANN, H SHIH, CY TI RAPID ACCRETION AND EARLY DIFFERENTIATION OF MARS INDICATED BY ND-142 ND-144 IN SNC METEORITES SO SCIENCE LA English DT Article ID ND ISOTOPIC EVOLUTION; SM-ND; MARTIAN ORIGIN; PB SYSTEMATICS; SHERGOTTITES; PLANET; AGE; ACHONDRITES; CHONDRITES; ABUNDANCES AB Small differences in the ratio of neodymium-142 to neodymium-144 in early formed mantle reservoirs in planetary bodies are the result of in situ decay of the extinct radionuclide samarium-146 and can be used to constrain early planetary differentiation and therefore the time scale of planetary accretion. The martian meteorite Nakhla (similar to 1.3 billion years old), the type sample of the nakhlite subgroup of the Shergottite-Nakhlite-Chassigny (SNC) meteorites, exhibits a 59 +/- 13 parts per million excess in the ratio of neodymium-142 to neodymium-144 relative to normal neodymium. This anomaly records differentiation in the martian mantle before 4539 million years ago and implies that Mars experienced no giant impacts at any time later than 27 million years after the origin of the solar system. C1 NASA, LYNDON B JOHNSON SPACE CTR, HOUSTON, TX 77058 USA. LOCKHEED ENGN & SCI CO, HOUSTON, TX 77058 USA. RP HARVARD UNIV, DEPT EARTH & PLANETARY SCI, 20 OXFORD ST, CAMBRIDGE, MA 02138 USA. NR 59 TC 117 Z9 117 U1 0 U2 6 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD JAN 13 PY 1995 VL 267 IS 5195 BP 213 EP 217 DI 10.1126/science.7809625 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA QB153 UT WOS:A1995QB15300027 PM 7809625 ER PT J AU SMITH, GD JAFFE, RL YOON, DY AF SMITH, GD JAFFE, RL YOON, DY TI CONFORMATIONS OF 1,2-DIMETHOXYETHANE IN THE GAS AND LIQUID-PHASES FROM MOLECULAR-DYNAMICS SIMULATIONS SO JOURNAL OF THE AMERICAN CHEMICAL SOCIETY LA English DT Note C1 IBM CORP,ALMADEN RES CTR,DIV RES,SAN JOSE,CA 95120. NASA,AMES RES CTR,INST THERMOSCI,STC 230-3,MOFFETT FIELD,CA 94035. NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 16 TC 62 Z9 62 U1 0 U2 4 PU AMER CHEMICAL SOC PI WASHINGTON PA PO BOX 57136, WASHINGTON, DC 20037-0136 SN 0002-7863 J9 J AM CHEM SOC JI J. Am. Chem. Soc. PD JAN 11 PY 1995 VL 117 IS 1 BP 530 EP 531 DI 10.1021/ja00106a061 PG 2 WC Chemistry, Multidisciplinary SC Chemistry GA QC061 UT WOS:A1995QC06100061 ER PT J AU LONSDALE, CJ SMITH, HE LONSDALE, CJ AF LONSDALE, CJ SMITH, HE LONSDALE, CJ TI ULTRALUMINOUS INFRARED GALAXIES AND THE RADIOOPTICAL CORRELATION FOR QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE INFRARED, GALAXIES; QUASARS, GENERAL; RADIO CONTINUUM, GALAXIES ID ACTIVE GALACTIC NUCLEI; X-RAY-SPECTRA; ENERGY-DISTRIBUTIONS; CONTINUUM; ABSORPTION; EMISSION AB Through analysis of available optical spectrophotometric data and radio flux density measurements in the literature, it is demonstrated that a good correlation exists between the radio power and bolometric luminosity of the optically-selected QSOs in the Bright Quasar Sample (BQS) of Schmidt and Green (1983). This correlation, noted previously by others as a correlation with absolute B-magnitude, is shown to be robust, and to be independent of a variety of assumptions used in the calculation of the bolometric luminosity. The correlation is present for the entire BQS sample, but is improved when QSOs with high values of radio-to-optical flux density (radio-loud) are excluded. Using this correlation, radio measurements can therefore be used to predict the bolometric luminosity of quasars even if their optical and UV continua are not directly observable. We have recently used VLBI meausurements of a sample of ultraluminous infrared galaxies to infer the likely existence of radio-quiet AGNs deeply enshrouded in dust within their nuclei (Lonsdale, Smith, and Lonsdale 1993). We employ the radio-bolometric luminosity correlation for the BQS quasars to test whether these hypothetical buried AGNs can be energetically responsible for the observed far-infrared luminosities of the ultraluminous infrared galaxies. The ultraluminous infrared galaxies are shown to follow the same relation between radio core power and bolometric luminosity as the radio-quiet QSOs, suggesting that buried AGNs can account for essentially all the observed infrared luminosity, and raising the possibility that any starburst which may be in progress may not be energetically dominant. The broader implications of the radio-optical correlation in quasars for AGNs and luminous infrared galaxy models and the use of radio astronomy as a probe of the central powerhouse in radio quiet AGNs and luminous infrared galaxies are briefly discussed. C1 UNIV CALIF SAN DIEGO, CTR ASTROPHYS & SPACE SCI, LA JOLLA, CA 92093 USA. UNIV CALIF SAN DIEGO, DEPT PHYS, LA JOLLA, CA 92093 USA. MIT, HAYSTACK OBSERV, WESTFORD, MA 01886 USA. RP LONSDALE, CJ (reprint author), CALTECH, CTR INFRARED PROC & ANAL, JET PROPULS LAB, 100-22, PASADENA, CA 91125 USA. NR 28 TC 41 Z9 41 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 JAN 10 PY 1995 VL 438 IS 2 BP 632 EP 642 DI 10.1086/175106 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA906 UT WOS:A1995QA90600010 ER PT J AU WEYMANN, R RAUCH, M WILLIAMS, R MORRIS, S HEAP, S AF WEYMANN, R RAUCH, M WILLIAMS, R MORRIS, S HEAP, S TI NEW OBSERVATIONS WITH THE HST GODDARD HIGH-RESOLUTION SPECTROGRAPH OF THE LOW-REDSHIFT LYMAN-ALPHA CLOUDS IN THE 3C-273 LINE-OF-SIGHT SO ASTROPHYSICAL JOURNAL LA English DT Article DE QUASARS, ABSORPTION LINES; QUASARS, INDIVIDUAL (3C 273); ULTRAVIOLET, GALAXIES ID VIRGO CLUSTER; GALAXIES; 3C-273; EMISSION; TELESCOPE; ABSORBERS; SPECTRUM AB We present spectra of 3C 273 between 1216 and 1250 Angstrom obtained in the (pre-COSTAR [Corrective Optics Space Telescope Axial Replacement instrument]) configuration of the GHRS, taken with the G160M grating, with a resolution of approximate to 20 km s(-1). The two strong Ly alpha lines at velocities of similar to 1000 and similar to 1600 km s(-1) are well fitted with Voigt profiles and yield column densities, Doppler parameters and redshifts of log N(H I) = 14.19 +/- 0.04, V-Dop = 40.7 +/- 3.0 km s(-1), V = 1012.4 +/- 2.0 km s(-1), and log N(H I) = 14.22 +/- 0.07, V-Dop 34.2 +/- 3.3 km s(-1) and V = 1582.0 +/- 2.0 km s(-1), respectively. Motivated by the initial announcement by Williams and Schommer of detectable Ha emission associated with the similar to 1600 km s(-1) cloud, we discuss the difficulty of finding models which can account for emission of that magnitude given the observed neutral hydrogen column density, though a recent reobservation by these authors has shown the initial detection to be spurious. The C/H abundance ratio is probably less than about one-fourth of the solar abundance in these clouds, although this result is very uncertain and model dependent. C1 SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. DOMINION ASTROPHYS OBSERV,VICTORIA,BC V8X 4M6,CANADA. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP WEYMANN, R (reprint author), OBSERV CARNEGIE INST WASHINGTON,813 SANTA BARBARA ST,PASADENA,CA 91101, USA. RI Morris, Simon/G-7981-2011 OI Morris, Simon/0000-0003-4866-110X NR 35 TC 34 Z9 34 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 1995 VL 438 IS 2 BP 650 EP 658 DI 10.1086/175108 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA906 UT WOS:A1995QA90600012 ER PT J AU RADECKE, HD BERTSCH, DL DINGUS, BL FICHTEL, CE HARTMAN, RC HUNTER, SD KANBACH, G KNIFFEN, DA LIN, YC MATTOX, JR MAYERHASSELWANDER, HA MICHELSON, PF VONMONTIGNY, C NOLAN, PL SCHNEID, E THOMPSON, DJ AF RADECKE, HD BERTSCH, DL DINGUS, BL FICHTEL, CE HARTMAN, RC HUNTER, SD KANBACH, G KNIFFEN, DA LIN, YC MATTOX, JR MAYERHASSELWANDER, HA MICHELSON, PF VONMONTIGNY, C NOLAN, PL SCHNEID, E THOMPSON, DJ TI EGRET DETECTION OF THE BLAZAR PKS-0420-014 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA RAYS, OBSERVATIONS; QUASARS, INDIVIDUAL (PKS 0420-014) ID EXTRAGALACTIC RADIO-SOURCES; ACTIVE GALACTIC NUCLEI; GAMMA-RAY EMISSION; ENERGY; TELESCOPE; MODEL; MULTIFREQUENCY; CONTINUUM; RADIATION; SPECTRA AB During its full-sky survey, the EGRET high-energy instrument aboard the Compton Gamma-Ray Observatory detected gamma-ray emission in the energy range above 30 MeV from a source identified as the blazar PKS 0420-014. This object was observed during two separate viewing periods in 1992 February/March and May/June. An intensity decrease above 100 MeV of a factor of at least 1.5 from a maximum of (5.0 +/- 1.4) x 10(-7) photons cm(-2) s(-1) was observed during that time interval indicating extensive variability. The photon spectrum in the range between 30 and 10,000 MeV at the time of the maximum intensity is well represented by a power law with an exponent of -1.9 +/- 0.3. Some similarities with other EGRET detected blazars are briefly discussed. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. STANFORD UNIV,HANSEN EXPTL PHYS LAB,STANFORD,CA 94305. GRUMMAN AEROSP CORP,BETHPAGE,NY 11714. NASA,GODDARD SPACE FLIGHT CTR,CSC,COMPTON OBSERV SCI SUPPORT CTR,ASTRON PROGRAMS,GREENBELT,MD 20771. HAMPDEN SYDNEY COLL,HAMPDEN SYDNEY,VA 23943. NASA,GODDARD SPACE FLIGHT CTR,UNIV SPACE RES ASSOC,GREENBELT,MD 20771. RP RADECKE, HD (reprint author), MAX PLANCK INST EXTRATERR PHYS,D-85740 GARCHING,GERMANY. RI Nolan, Patrick/A-5582-2009; Hunter, Stanley/D-2942-2012; Thompson, David/D-2939-2012; OI Thompson, David/0000-0001-5217-9135; Dingus, Brenda/0000-0001-8451-7450 NR 49 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 JAN 10 PY 1995 VL 438 IS 2 BP 659 EP 662 DI 10.1086/175109 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA906 UT WOS:A1995QA90600013 ER PT J AU MADEJSKI, GM ZDZIARSKI, AA TURNER, TJ DONE, C MUSHOTZKY, RF HARTMAN, RC GEHRELS, N CONNORS, A FABIAN, AC NANDRA, K CELOTTI, A REES, MJ JOHNSON, WN GROVE, JE STARR, CH AF MADEJSKI, GM ZDZIARSKI, AA TURNER, TJ DONE, C MUSHOTZKY, RF HARTMAN, RC GEHRELS, N CONNORS, A FABIAN, AC NANDRA, K CELOTTI, A REES, MJ JOHNSON, WN GROVE, JE STARR, CH TI JOINT ROSAT-COMPTON GRO OBSERVATIONS OF THE X-RAY-BRIGHT SEYFERT-GALAXY IC-4329A SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, INDIVIDUAL (IC 4329A, IC 4329); GALAXIES, SEYFERT; X-RAYS, GALAXIES; GAMMA RAYS, OBSERVATIONS ID COLD MATTER; IC-4329A; QUASARS; SPECTRA; NUCLEI; OSSE AB We report a simultaneous ROSAT and GRO observation of the X-ray-bright Seyfert galaxy IC 4329A. For the GRO OSSE detector, we also present the sum of the data for this and earlier observations. The overall spectrum is very well described as a power law with an energy spectral index of similar to 1 absorbed at low energies plus a strong Compton reflection component, typical for Seyfert 1 galaxies. The low energy absorption can be well described by a sum of a neutral column density of similar to 3 x 10(21) cm(-2), most of which is associated with the edge-on galactic disk of IC 4329A, plus an edgelike feature at similar to 700 eV; this feature implies either complex absorption (due to additional ionized material, or due to partial covering), or a soft excess. The data only weakly constrain the presence of a high-energy cutoff in the underlying power law; they are compatible with an exponential cutoff at any energy E(c) greater than or similar to 100 keV. The relative steepness of the OSSE data, with the power-law energy index of 1.6 +/- 0.2, can be accounted for entirely by the contribution of the high-energy tail of the reflection component when E(c) --> infinity. (We find that the definite cutoff at an energy E(c) similar to 130 keV suggested in the recently published analysis of the OSSE data for this object is due to a data reduction error.) Including nonsimultaneous Ginga observations with 2 keV fluxes matching well that of ROSAT gives us likely broadband X-ray/gamma-ray spectra of the object from similar to 0.1 keV up to several hundred keV. Joint spectral analysis of the data sets from the three instruments gives results similar to those from ROSAT/OSSE only, except that the cutoff energy is now constrained to be at 250 keV less than or similar to E(c) less than or similar to 1700 keV. The constraint on E(c) markedly distinguishes this object from NGC 4151, where E(c) was lower, similar to 50 keV; this has implications for emission models for AGNs as well as for their contribution to the X-ray background. We also report the ROSAT spectrum of the companion object to the Seyfert galaxy, the elliptical galaxy IC 4329 located similar to 3' away. Its spectrum is well described by an optically thin thermal plasma with kT = 0.9 keV, with a 0.1-2 keV flux of 8 x 10(-13) ergs cm(-2) s(-1), corresponding to a luminosity of similar to 8 x 10(41) ergs s(-1). C1 NICHOLAS COPERNICUS ASTRON CTR,PL-00716 WARSAW,POLAND. UNIV LEICESTER,DEPT PHYS,LEICESTER LE1 7RH,LEICS,ENGLAND. UNIV NEW HAMPSHIRE,CTR SPACE SCI,DURHAM,NH 03824. UNIV CAMBRIDGE,INST ASTRON,CAMBRIDGE CB3 0HA,ENGLAND. USN,RES LAB,EO HULBURT CTR SPACE RES,WASHINGTON,DC 20375. UNIV SPACE RES ASSOC,COLUMBIA,MD. COMP SCI CORP,EL SEGUNDO,CA 90245. RP MADEJSKI, GM (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. RI Gehrels, Neil/D-2971-2012; Johnson, Neil/G-3309-2014; done, chris/D-4605-2016 OI done, chris/0000-0002-1065-7239 NR 22 TC 61 Z9 61 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 JAN 10 PY 1995 VL 438 IS 2 BP 672 EP 679 DI 10.1086/175111 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA906 UT WOS:A1995QA90600015 ER PT J AU PETUCHOWSKI, SJ BENNETT, CL AF PETUCHOWSKI, SJ BENNETT, CL TI NEUTRAL GAS CONTRIBUTIONS TO [S-II]-EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC PROCESSES; ISM, ABUNDANCES; SUPERNOVA REMNANTS ID SUPERNOVA-REMNANTS; PHOTODISSOCIATION REGIONS; INTERSTELLAR-MEDIUM; LINE PROPERTIES; ATOMIC SULFUR; H-I; GALAXIES; ABSORPTION; ABUNDANCES; NITROGEN AB Emission in the forbidden lines of ionized sulfur arises in both predominantly ionized and predominantly neutral regions. The separation of [S II] emission from supernova remnants into nearly orthogonal dependences on [O I] and a power of [N II]/H alpha is discussed. [S II] may be excited via photoionization into forbidden-line-emitting states in regions devoid of electronic excitation of [O I]. Emission along ''background'' lines of sight in the Milky Way and in extragalactic ''froth'' is considered in terms of contributions of neutral gas. RP PETUCHOWSKI, SJ (reprint author), NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,MC 685,GREENBELT,MD 20771, USA. NR 36 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 JAN 10 PY 1995 VL 438 IS 2 BP 735 EP 739 DI 10.1086/175118 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA906 UT WOS:A1995QA90600022 ER PT J AU WOODWARD, CE GREENHOUSE, MA GEHRZ, RD PENDLETON, YJ JOYCE, RR VANBUREN, D FISCHER, J JENNERJOHN, NJ KAMINSKI, CD AF WOODWARD, CE GREENHOUSE, MA GEHRZ, RD PENDLETON, YJ JOYCE, RR VANBUREN, D FISCHER, J JENNERJOHN, NJ KAMINSKI, CD TI THE TEMPORAL EVOLUTION OF THE 1-5-MICRON SPECTRUM OF V1974-CYGNI (NOVA-CYGNI 1992) SO ASTROPHYSICAL JOURNAL LA English DT Article DE INFRARED, STARS; NOVAE, CATACLYSMIC VARIABLES; STARS, ABUNDANCES STARS, INDIVIDUAL (NOVA CYGNI 1992) ID INFRARED CORONAL LINES; HERCULIS 1991; NEON NOVA; SPECTROSCOPY; OXYGEN; SPECTROPHOTOMETRY; PHOTOMETRY; MAGNESIUM; EMISSION AB We present 1-5 mu m moderate- and high-resolution infrared spectra of the ONeMg nova V1974 (Nova Cygni 1992) obtained at multiple epochs during an approximate to 500 day period after outburst. During the first 80 days, the spectra exhibited continuum emission from thermal bremsstrahlung (free-free radiation) with prominent recombination line emission from hydrogen, helium, nitrogen, and oxygen. The measured FWHM of these recombination lines suggests that the initial velocity of the ejecta was approximate to 2400-3400 km s(-1). We estimate from the hydrogen recombination line ratios that the density of the ionized shell at this epoch was approximate to 10(9) cm(-3), with an effective electron temperature of approximate to 5 x 10(3) K. As the temporal evolution of the ejecta progressed, the hydrogen and helium lines diminished in intensity, and coronal lines of aluminum, calcium, magnesium, neon, and sulfur appeared by approximate to day 80. The coronal line emission phase persisted for over 400 days. During this epoch, no significant dust formation occurred. We find that the ejecta of V1974 Cyg were overabundant in aluminum with respect to silicon by a factor of approximate to 5 and in magnesium with respect to silicon by a factor of greater than or equal to 3 relative to the solar photosphere. Comparison of our observed overabundances with recent model predictions of elemental synthesis in ONeMg outbursts suggests that the accreted envelope on V1974 Cyg was close to solar composition and that the precursor ONeMg white dwarf had a mass of approximate to 1 M.. C1 SMITHSONIAN INST,NATL AIR & SPACE MUSEUM,ASTROPHYS LAB,MRC 321,WASHINGTON,DC 20560. UNIV MINNESOTA,SCH PHYS & ASTRON,DEPT ASTRON,MINNEAPOLIS,MN 55455. NASA,AMES RES CTR,DIV SPACE SCI,MOFFETT FIELD,CA 94035. KITT PEAK NATL OBSERV,TUCSON,AZ 85726. CALTECH,PASADENA,CA 94305. USN,RES LAB,DIV REMOTE SENSING,WASHINGTON,DC 20375. SAN FRANCISCO STATE UNIV,DEPT PHYS,SAN FRANCISCO,CA 94037. NASA,IRTF,HONOLULU,HI 96822. RP WOODWARD, CE (reprint author), UNIV WYOMING,DEPT PHYS & ASTRON,WYOMING INFRARED OBSERV,LARAMIE,WY 82071, USA. NR 64 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 JAN 10 PY 1995 VL 438 IS 2 BP 921 EP 931 DI 10.1086/175134 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA906 UT WOS:A1995QA90600038 ER PT J AU CASSINELLI, JP COHEN, DH MACFARLANE, JJ DREW, JE LYNASGRAY, AE HOARE, MG VALLERGA, JV WELSH, BY VEDDER, PW HUBENY, I LANZ, T AF CASSINELLI, JP COHEN, DH MACFARLANE, JJ DREW, JE LYNASGRAY, AE HOARE, MG VALLERGA, JV WELSH, BY VEDDER, PW HUBENY, I LANZ, T TI EUVE SPECTROSCOPY OF EPSILON-CANIS-MAJORIS (B2-II) FROM 70-ANGSTROM TO 730-ANGSTROM SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, GENERAL; LINE, IDENTIFICATION; STARS, ATMOSPHERES; STARS, EARLY-TYPE STARS, INDIVIDUAL (EPSILON CANIS MAJORIS); STARS, MASS LOSS ID MODEL STELLAR ATMOSPHERES; RADIATION-DRIVEN WINDS; HOT LUMINOUS STARS; EXTREME-ULTRAVIOLET; EFFECTIVE TEMPERATURES; BOWEN FLUORESCENCE; ANGULAR DIAMETERS; MASS-LOSS; LINE; EMISSION AB We present spectra of the brightest stellar source of extreme ultraviolet (EUV) radiation longward of 400 Angstrom, the B2 II star, epsilon CMa. These data were taken with the three spectrometers aboard the NASA Extreme Ultraviolet Explorer satellite (EUVE) during the first cycle of pointed observations. We report on our initial studies of the continuum and line spectrum of the stellar photosphere in the 320 to 730 Angstrom region, and on the wind emission lines observed in the 170-375 Angstrom region. This is the first EUV spectrum of an early-type star, and thus makes epsilon CMa the most comprehensively observed B star from the X-ray to infrared regimes. The radiation in both the H Lyman continuum and He I continuum (shortward of 504 Angstrom) are found to be significantly greater than predicted by both LTE and non-LTE model atmospheres. Since epsilon CMa also exhibits a mid-infrared excess, this points to the outer layers being warmer than the models indicate. The anomalously large Lyman continuum flux, combined with the very low column density measured in the direction toward this star implies that it is the dominant source of hydrogen ionization of the local interstellar medium in the immediate vicinity of the sun. All of the lines predicted to be strong from model atmospheres are present and several wind absorption features are also identified. We have detected emission lines from highly ionized iron, ranging from Fe+8 to Fe+15, which arise in the X-ray producing region. The lines are consistent with the ROSAT PSPC observations if a multi-temperature emission model is used, and the assumption is made that there is significant absorption beyond that of the neutral phase of the ISM. The EUV spectrum shows a strong He II Lyman-alpha emission at 304 Angstrom. This line cannot be formed in the upper regions of the photosphere, but rather is due to the recombination of He++, which is itself produced by the X-ray and EUV (lambda < 228 Angstrom) radiation present in the outer atmosphere. The spectrum also shows strong O III 374 Angstrom line emission produced by the Bowen fluorescence mechanism, which has not previously been observed in the spectra of hot stars. C1 UNIV OXFORD,DEPT ASTROPHYS,OXFORD OX1 3RH,ENGLAND. MAX PLANCK INST ASTRON,D-69117 HEIDELBERG,GERMANY. EUREKA SCI,OAKLAND,CA 94602. UNIV CALIF BERKELEY,SPACE SCI LAB,BERKELEY,CA 94720. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP CASSINELLI, JP (reprint author), UNIV WISCONSIN,DEPT ASTRON,475 N CHARTER ST,MADISON,WI 53706, USA. NR 56 TC 74 Z9 74 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 JAN 10 PY 1995 VL 438 IS 2 BP 932 EP 949 DI 10.1086/175135 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA906 UT WOS:A1995QA90600039 ER PT J AU MOORE, RL LAROSA, TN ORWIG, LE AF MOORE, RL LAROSA, TN ORWIG, LE TI THE WALL OF RECONNECTION-DRIVEN MAGNETOHYDRODYNAMIC TURBULENCE IN A LARGE SOLAR-FLARE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCELERATION OF PARTICLES; MHD; SUN, FLARES; TURBULENCE ID X-RAY OBSERVATIONS; FILAMENT ERUPTIONS; MAGNETIC-FIELDS; IMPULSIVE PHASE; ENERGY-RELEASE; MODEL; PROMINENCES; CORONA AB LaRosa & Moore (1993) recently proposed that the bulk dissipation of magnetic field that is required for the electron energization in the explosive phase of solar flares occurs in a ''fat current sheet,'' a wall of cascading MHD turbulence sustained by highly disordered driven reconnection of opposing magnetic fields impacting at a turbulent boundary layer. In two-ribbon eruptive flares, this turbulent reconnection wall is supposed to develop at the usual reconnection site in the standard model for these flares; that is, the reconnection wall stands in the vertical magnetic rent made by the eruption of the sheared core of the preflare closed bipolar field. Here, we use the well-observed great two-ribbon eruptive flare of 1984 April 24/25 to assess the feasibility of both (1) the standard model for the overall three-dimensional form and action of the magnetic field and (2) the turbulent reconnection wall within it. The observed aspects of this flare that we use are (1) the preflare photospheric vector magnetic field; (2) the occurrence of a flare spray and the size, form, and spreading of the chromospheric flare ribbons; and (3) the rate of production of hard (greater than or similar to 25 keV) X-rays in the explosive phase of the flare. We find (1) that the morphology of this flare closely matched that of the standard model; (2) the preflare sheared core field had enough nonpotential magnetic energy to power the flare; (3) the model turbulent wall required to achieve the flare's peak dissipative power easily fit within the overall span of the flaring magnetic field; (4) this wall was thick enough to have turbulent eddies large enough (diameters similar to 10(8) cm) to produce the similar to 10(26) ergs energy release fragments typically observed in the explosive phase of flares; (5) the aspect ratio (thickness/vertical extent) of the turbulent reconnection wall was in the 0.1-1 range expected by (Packer 1973). We therefore conclude that the viability of our version of the standard model (i.e., having the magnetic field dissipation occur in our turbulent reconnection wall) is well confirmed by this typical great two-ribbon eruptive flare. C1 KENNESAW STATE COLL, DEPT BIOL & PHYS SCI, MARIETTA, GA 30061 USA. NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, GREENBELT, MD 20771 USA. RP MOORE, RL (reprint author), NASA, GEORGE C MARSHALL SPACE FLIGHT CTR, SPACE SCI LAB, ES52, HUNTSVILLE, AL 35812 USA. NR 48 TC 30 Z9 30 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 JAN 10 PY 1995 VL 438 IS 2 BP 985 EP 996 DI 10.1086/175140 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA906 UT WOS:A1995QA90600044 ER PT J AU GEORGE, IM TURNER, TJ NETZER, H AF GEORGE, IM TURNER, TJ NETZER, H TI THE DISCOVERY OF AN O-VII EMISSION-LINE IN THE ASCA SPECTRUM OF THE SEYFERT-GALAXY NGC-3783 SO ASTROPHYSICAL JOURNAL LA English DT Article DE GALAXIES, ACTIVE; GALAXIES, INDIVIDUAL (NGC-3783); GALAXIES, NUCLEI; X-RAYS, GALAXIES ID RAY AB We report the first observation of an O VII 0.57 keV emission line in a Seyfert 1 galaxy. NGC 3783 was observed by ASCA twice over a period of 4 days in 1993 December. The source exhibited a approximately 30% change in intensity between the two observations, with most of the variability taking place as a result of steepening of the continuum less-than-or-similar-to 1 keV. Spectra from both observations show intense absorption features in the 0.5-1.5 keV band, which can be well fitted by an ionized absorber model of solar composition, column density of 10(22.2) cm-2 and ionization parameter of approximately 7-8; the strongest absorption features being due to O VII and O VIII. Two emission features are also seen in the spectra which we identify as O VII 0.57 keV (equivalent width congruent-to 36 eV) and O VIII 0.65 keV (equivalent width congruent-to 11 eV). We find these features are at the intensity predicted by the above ionized absorber model when the covering factor is close to unity. We also show that the 3-6 keV continuum of the source is well fitted by a GAMMA = 1.3-1.4 power-law continuum, a narrow neutral iron K-shell fluorescence line and a strong iron K-shell absorption edge, possibly corresponding to highly ionized iron. The intensity of neither of these K-shell features can be explained by the ionized absorber, and thus must be from a separate component. C1 TEL AVIV UNIV,BEVERLY & RAMOND SACKLER FAC EXACT SCI,SCH PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. TEL AVIV UNIV,BEVERLY & RAMOND SACKLER FAC EXACT SCI,WISE OBSERV,IL-69978 TEL AVIV,ISRAEL. RP GEORGE, IM (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,CODE 668,GREENBELT,MD 20771, USA. NR 15 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 JAN 10 PY 1995 VL 438 IS 2 BP L67 EP L70 DI 10.1086/187717 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA907 UT WOS:A1995QA90700005 ER PT J AU PRESTWICH, AH GUIMOND, SJ LUGINBUHL, CB JOY, M AF PRESTWICH, AH GUIMOND, SJ LUGINBUHL, CB JOY, M TI ROSAT HRI IMAGES OF ABELL-85 AND ABELL-496 - EVIDENCE FOR HOMOGENEITIES IN COOLING FLOWS SO ASTROPHYSICAL JOURNAL LA English DT Article DE COOLING FLOWS; GALAXIES, CLUSTERS, GENERAL; INTERGALACTIC MEDIUM; X-RAYS, GALAXIES ID X-RAY; FILAMENTS; GALAXIES AB We present ROSAT high-resolution images of two clusters of galaxies with cooling flows, Abell 496 and Abell 85. In these clusters, X-ray emission on small scales above the general cluster emission is significant at the 3 sigma level. There is no evidence for optical counterparts. If real, the enhancements may be associated with clumps of gas at a lower temperature and higher density than the ambient medium, or hotter, denser gas perhaps compressed by magnetic fields. These observations can be used to test models of how thermal instabilities form and evolve in cooling flows. C1 USN OBSERV,FLAGSTAFF STN,FLAGSTAFF,AZ 86002. NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB,HUNTSVILLE,AL 35812. RP PRESTWICH, AH (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138, USA. NR 12 TC 14 Z9 15 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 1995 VL 438 IS 2 BP L71 EP & DI 10.1086/187718 PN 2 PG 0 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA907 UT WOS:A1995QA90700006 ER PT J AU FABRIKANT, AL AF FABRIKANT, AL TI HARBOR OSCILLATIONS GENERATED BY SHEAR-FLOW SO JOURNAL OF FLUID MECHANICS LA English DT Article ID SHORT-WAVE GROUPS AB A new mechanism that could be responsible for excitation of long-period oscillations in partially enclosed harbours is discussed. This mechanism is based on the interaction between a shear flow and the harbour-basin natural mode and does not suppose any external exciting forces caused by wind waves, tsunami, etc. The growth rate of harbour oscillations is found in terms of a plane-wave reflection coefficient integrated on the wavenumber spectrum of the oscillating outflow field near the harbour entrance. Analytical considerations for simple shear flows (vortex sheet and jet) show that the growth rate changes its sign depending on the ratio of oscillation frequency to flow speed. RP FABRIKANT, AL (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 32 TC 13 Z9 13 U1 0 U2 1 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0022-1120 J9 J FLUID MECH JI J. Fluid Mech. PD JAN 10 PY 1995 VL 282 BP 203 EP 217 DI 10.1017/S0022112095000103 PG 15 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA QD789 UT WOS:A1995QD78900010 ER PT J AU WEYGANDT, JH MEHTA, RD AF WEYGANDT, JH MEHTA, RD TI 3-DIMENSIONAL STRUCTURE OF STRAIGHT AND CURVED PLANE WAKES SO JOURNAL OF FLUID MECHANICS LA English DT Article ID MIXING LAYER; TURBULENT WAKE; TRANSITION; CURVATURE; AIRFOIL; STREAM AB The formation and evolution of the three-dimensional structure of straight and mildly curved (b/(R) over bar < 2 %) flat plate wakes at relatively high Reynolds numbers (Re-b = 28 000) have been studied through detailed measurements of the mean and fluctuating velocities. In both cases, the role of initial conditions was examined by generating wakes from untripped (laminar) and tripped (turbulent) initial boundary layers. The curved wake was affected by the angular momentum instability such that the inside half of the wake was unstable, whereas the outside half was stable. In both the straight and curved untripped wakes, large spanwise variations, in the form of 'pinches' and 'crests', were observed in the contours of mean velocity and Reynolds stresses. Well-organized, 'spatially stationary' streamwise vorticity was generated in the near-field region in the form of quadrupoles, to which the spanwise variations in the velocity contours were attributed. The presence of mean streamwise vorticity had a significant effect on the wake growth and defect decay rates, mainly by providing additional entrainment. In the straight wake, the mean streamwise vorticity decayed on both sides of the wake such that it had decayed completely by the far-field region. However, in the curved case, the mean streamwise vorticity on the unstable side decayed at a rate significantly lower than that on the stable side. Despite the decay of mean streamwise vorticity, the spanwise variations persisted into the far wake in both cases. The effects of curvature were also apparent in the Reynolds stress results which showed that the levels on the unstable side were increased significantly compared to those on the stable side, with the effect much stronger in the initially laminar wake. With the initial boundary layers tripped, spatially stationary streamwise vortex structures were not observed in either the straight or curved wakes and the velocity contours appeared nominally two-dimensional. This result further confirms the strong dependency of the three-dimensional structure of plane wakes on initial conditions. C1 STANFORD UNIV,JIAA,DEPT AERONAUT & ASTRONAUT,STANFORD,CA 94305. NASA,AMES RES CTR,FLUID MECH LAB,MOFFETT FIELD,CA 94035. NR 38 TC 26 Z9 26 U1 0 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH STREET, NEW YORK, NY 10011-4211 SN 0022-1120 J9 J FLUID MECH JI J. Fluid Mech. PD JAN 10 PY 1995 VL 282 BP 279 EP 311 DI 10.1017/S0022112095000140 PG 33 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA QD789 UT WOS:A1995QD78900014 ER PT J AU MEARINI, GT KRAINSKY, IL DAYTON, JA WANG, YX ZORMAN, CA ANGUS, JC ANDERSON, DF AF MEARINI, GT KRAINSKY, IL DAYTON, JA WANG, YX ZORMAN, CA ANGUS, JC ANDERSON, DF TI STABLE SECONDARY-ELECTRON EMISSION FROM CHEMICAL-VAPOR-DEPOSITED DIAMOND FILMS COATED WITH ALKALI-HALIDES SO APPLIED PHYSICS LETTERS LA English DT Article C1 CASE WESTERN RESERVE UNIV,CLEVELAND,OH 44106. FERMILAB NATL ACCELERATOR LAB,BATAVIA,IL 60510. RP MEARINI, GT (reprint author), NASA,LEWIS RES CTR,CLEVELAND,OH 44135, USA. NR 12 TC 26 Z9 27 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD JAN 9 PY 1995 VL 66 IS 2 BP 242 EP 244 DI 10.1063/1.113559 PG 3 WC Physics, Applied SC Physics GA QA698 UT WOS:A1995QA69800044 ER PT J AU GUADAGNINI, R SCHATZ, GC WALCH, SP AF GUADAGNINI, R SCHATZ, GC WALCH, SP TI GLOBAL POTENTIAL-ENERGY SURFACES FOR THE LOWEST (1)A', (3)A'', AND (1)A'' STATES OF HNO SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID CONFIGURATION-INTERACTION CALCULATIONS; TRANSFER COLLISIONS; NO; REPRESENTATION C1 NASA, AMES RES CTR, INST THERMOSCI, MOFFETT FIELD, CA 94035 USA. RP NORTHWESTERN UNIV, DEPT CHEM, EVANSTON, IL 60208 USA. NR 27 TC 71 Z9 74 U1 1 U2 12 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 JAN 8 PY 1995 VL 102 IS 2 BP 774 EP 783 DI 10.1063/1.469191 PG 10 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA QA679 UT WOS:A1995QA67900019 ER PT J AU GUADAGNINI, R SCHATZ, GC WALCH, SP AF GUADAGNINI, R SCHATZ, GC WALCH, SP TI QUASI-CLASSICAL TRAJECTORY STUDIES OF N+OH, O+NH, AND H+NO COLLISIONS USING GLOBAL AB-INITIO POTENTIAL-ENERGY SURFACES SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID REACTIONS N+OH->NO+H; NO; STATE; HNO; NH C1 NASA,AMES RES CTR,INST THERMOSCI,MOFFETT FIELD,CA 94035. RP GUADAGNINI, R (reprint author), NORTHWESTERN UNIV,DEPT CHEM,EVANSTON,IL 60208, USA. NR 24 TC 30 Z9 32 U1 0 U2 8 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 8 PY 1995 VL 102 IS 2 BP 784 EP 791 DI 10.1063/1.469192 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA QA679 UT WOS:A1995QA67900020 ER PT J AU FRANCISCO, JS RICHARDSON, SL AF FRANCISCO, JS RICHARDSON, SL TI DETERMINATION OF THE CC BOND-DISSOCIATION ENERGY IN CYANOGEN SO JOURNAL OF CHEMICAL PHYSICS LA English DT Note ID PHOTOCHEMISTRY; TITAN; CN C1 HOWARD UNIV,CTR STUDY TERR & EXTRATERR ATMOSPHERES,WASHINGTON,DC 20059. HOWARD UNIV,SCH ENGN,DEPT ELECT ENGN,WASHINGTON,DC 20059. RP FRANCISCO, JS (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 9 TC 8 Z9 8 U1 1 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 JAN 8 PY 1995 VL 102 IS 2 BP 1100 EP 1101 DI 10.1063/1.469460 PG 2 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA QA679 UT WOS:A1995QA67900056 ER PT J AU SMITH, GD LUDOVICE, PJ JAFFE, RL YOON, DY AF SMITH, GD LUDOVICE, PJ JAFFE, RL YOON, DY TI CONFORMATIONS OF 2,4-DICHLOROPENTANE AND 2,4,6-TRICHLOROHEPTANE AND A FORCE-FIELD FOR POLY(VINYL CHLORIDE) BASED UPON AB-INITIO ELECTRONIC-STRUCTURE CALCULATIONS SO JOURNAL OF PHYSICAL CHEMISTRY LA English DT Article ID SIMULATIONS AB The conformational properties of 2,4-dichloropentane (DCP) and 2,4,6-trichloroheptane (TCH) have been investigated in detail through ab initio electronic structure calculations as a critical step in the development of an accurate classical force field for poly(vinyl chloride). The conformational energies for DCP, obtained with a 6-31G*(*) basis set with electron correlation effects considered at the MP2 level, yield a value of E(eta) = -0.9 kcal/mol, denoting the energy of the racemic tt conformer relative to the meso tg conformer. This value is in excellent agreement with ca. -0.85 kcal/mol deduced previously from stereochemical epimerization experiments; The conformational energies calculated for TCH with a 6-31G* basis set at the MP2 level also yield stereochemical equilibrium results in good agreement with experiment. The analysis of TCH conformational energies in terms of a rotational isomeric state (RIS) model shows that a second-order RIS representation is not adequate due to significant Coulombic interactions involving chlorine atoms that depend on the conformations of four intervening skeletal bonds. The intermolecular interactions for model complexes of 2-chloropropane/2-chloropropane and 1,3-dichloropropane/2-chloropropane, determined at the MP2 level using a 6-31G*(*) basis set, indicate that the strength of the chlorine-methylene hydrogen interaction is comparable to that of the chlorine-methine hydrogen interaction. Moreover, the ab initio calculated energies, geometries, and dipole moments of DCP, together with the complex energies, have been employed to derive a conformational energy force field. The force field was found to reproduce well the conformational energies of TCH as determined from ab initio calculations and has been applied in simulations of poly(vinyl chloride) melt chains. C1 IBM CORP, ALMADEN RES CTR, SAN JOSE, CA 95120 USA. NASA, AMES RES CTR, INST THERMOSCI, MOFFETT FIELD, CA 94035 USA. NR 12 TC 20 Z9 20 U1 0 U2 1 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0022-3654 J9 J PHYS CHEM-US JI J. Phys. Chem. PD JAN 5 PY 1995 VL 99 IS 1 BP 164 EP 172 DI 10.1021/j100001a029 PG 9 WC Chemistry, Physical SC Chemistry GA QB567 UT WOS:A1995QB56700029 ER PT J AU MARCAIDE, JM ALBERDI, A ROS, E DIAMOND, P SCHMIDT, B SHAPIRO, II BAATH, L DAVIS, RJ DEBRUYN, AG ELOSEGUI, P GUIRADO, JC JONES, DL KRICHBAUM, TP MANTOVANI, F PRESTON, RA RATNER, MI RIUS, A ROGERS, AEE SCHILIZZI, RT TRIGILIO, C WHITNEY, AR WITZEL, A ZENSUS, A AF MARCAIDE, JM ALBERDI, A ROS, E DIAMOND, P SCHMIDT, B SHAPIRO, II BAATH, L DAVIS, RJ DEBRUYN, AG ELOSEGUI, P GUIRADO, JC JONES, DL KRICHBAUM, TP MANTOVANI, F PRESTON, RA RATNER, MI RIUS, A ROGERS, AEE SCHILIZZI, RT TRIGILIO, C WHITNEY, AR WITZEL, A ZENSUS, A TI DISCOVERY OF SHELL-LIKE RADIO-STRUCTURE IN SN1993J SO NATURE LA English DT Article ID SUPERNOVAE; EMISSION; REMNANTS; MODEL AB SUPERNOVA explosions are poorly understood, partly because of difficulties in modelling them theoretically(1), and partly because there have been no supernovae observed in our Galaxy since the invention of the telescope. But the recent discovery(2) of supernova SN1993J in the nearby galaxy M81 offers an opportunity to investigate the evolution of the remnant, and its interaction with the surrounding interstellar medium, at high resolution. Here we present radio observations of SN1993J, made using very-long-baseline interferometry, which show the development of a shell structure. This 8-month-old radio shell is the youngest ever discovered in a supernova. The data suggest that the supernova explosion and the expanding shell of the remnant have nearly spherical symmetry, with small deviations where some parts of the shell are brighter than others. If these deviations arise because of variations in the density of the shell, this may reconcile earlier reports of symmetric radio emission(3) with the observed optical asymmetry(4,5), as the density variations could easily cause the latter. We infer that the radio emission is generated at the interface(6-9), where the surrounding gas is shocked by the ejecta. C1 HARVARD SMITHSONIAN CTR ASTROPHYS,CAMBRIDGE,MA 02138. CSIC,INST ASTROFIS ANDALUCIA,E-18080 GRANADA,SPAIN. NATL RADIO ASTRON OBSERV,SOCORRO,NM 87801. ONSALA SPACE OBSERV,S-43992 ONSALA,SWEDEN. UNIV MANCHESTER,NUFFIELD RADIO ASTRON LABS,MACCLESFIELD SK11 9DL,CHESHIRE,ENGLAND. NETHERLANDS FDN RES ASTRON,7990 AA DWINGELOO,NETHERLANDS. CALTECH,JET PROP LAB,PASADENA,CA 91109. MAX PLANCK INST RADIOASTRON,D-53010 BONN,GERMANY. CNR,IST RADIOASTRON,I-40129 BOLOGNA,ITALY. FAC CIENCIAS MATEMAT MADRID,INST ASTRON & GEODESIA,E-28040 MADRID,SPAIN. JOINT INST VLBI EUROPE,7790 AA DWINGELOO,NETHERLANDS. CNR,IST RADIOASTRON,NOTO,ITALY. MIT,HAYSTACK OBSERV,WESTFORD,MA 01886. RP MARCAIDE, JM (reprint author), UNIV VALENCIA,DEPT ASTRON,E-46100 BURJASSOT,SPAIN. OI Schmidt, Brian/0000-0001-6589-1287; Ros, Eduardo/0000-0001-9503-4892 NR 23 TC 43 Z9 43 U1 0 U2 5 PU MACMILLAN MAGAZINES LTD PI LONDON PA 4 LITTLE ESSEX STREET, LONDON, ENGLAND WC2R 3LF SN 0028-0836 J9 NATURE JI Nature PD JAN 5 PY 1995 VL 373 IS 6509 BP 44 EP 45 DI 10.1038/373044a0 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA QA239 UT WOS:A1995QA23900048 ER PT J AU ELLIOT, JL OLKIN, CB DUNHAM, EW FORD, CH GILMORE, DK KURTZ, D LAZZARO, D RANK, DM TEMI, P BANDYOPADHYAY, RM BARROSO, J BARUCCI, A BOSH, AS BUIE, MW BUS, SJ DAHN, CC FORYTA, DW HUBBARD, WB LOPES, DF MARCIALIS, RL MCDONALD, SW MILLIS, RL REITSEMA, H SCHLEICHER, DG SICARDY, B STONE, RPS WASSERMAN, LH AF ELLIOT, JL OLKIN, CB DUNHAM, EW FORD, CH GILMORE, DK KURTZ, D LAZZARO, D RANK, DM TEMI, P BANDYOPADHYAY, RM BARROSO, J BARUCCI, A BOSH, AS BUIE, MW BUS, SJ DAHN, CC FORYTA, DW HUBBARD, WB LOPES, DF MARCIALIS, RL MCDONALD, SW MILLIS, RL REITSEMA, H SCHLEICHER, DG SICARDY, B STONE, RPS WASSERMAN, LH TI JET-LIKE FEATURES NEAR THE NUCLEUS OF CHIRON SO NATURE LA English DT Article ID 2060 CHIRON; COMET HALLEY; 2060-CHIRON; PHOTOMETRY; CCD AB CONSIDERED as a comet, the object 2060 Chiron is unusual in two respects: it exhibits outbursts at very large distances from the Sun(1-3), and its nucleus is much larger than that of any other known comet(4,5). It is, however, similar in size to the recently discovered Kuiper-belt objects(6)-a population of objects with orbits beyond Neptune, which are a possible source of short-period comets. This has led to the conjecture that Chiron is related to these objects, but its chaotic orbit has brought it much closer to the Sun(7). Here we report observations of a recent stellar occultation by Chiron which permit the identification of several features associated with Chiron's coma. The observation of discrete, jet-like features provides evidence that the coma material originates from just a few, small active areas, rather than from uniform sublimation, and that the particles in at least one of these features have radii greater than 0.25 mu m. The observations also suggest the presence of material in the plane of Chiron's orbit and are consistent with a gravitationally bound coma, Finally, the present data, and those from a previous occultation(8), constrain the radius of Chiron to lie between 83 and 156 km. C1 MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. LOWELL OBSERV, FLAGSTAFF, AZ 86001 USA. NASA, AMES RES CTR, MOFFETT FIELD, CA 94035 USA. SETI INST, MT VIEW, CA 94043 USA. UNIV CALIF SANTA CRUZ, LICK OBSERV, SANTA CRUZ, CA 95064 USA. UNIV CAPE TOWN, RONDEBOSCH 7700, SOUTH AFRICA. DAF, OBSERV NACL, CNPQ, BR-20921 RIO DE JANEIRO, BRAZIL. OBSERV PARIS, F-92195 MEUDON, FRANCE. USN OBSERV, FLAGSTAFF, AZ 86002 USA. UFPR, CTR POLITECN, DEPT FIS, BR-80000 CURITIBA, PARANA, BRAZIL. UNIV ARIZONA, LUNAR & PLANETARY LAB, TUCSON, AZ 85721 USA. PIMA COMMUNITY COLL, TUCSON, AZ 85709 USA. BALL AEROSP SYST GRP, BOULDER, CO 80306 USA. UNIV PARIS 06, UFR PHYS 924, F-75252 PARIS, FRANCE. UNIV CALIF SANTA CRUZ, LICK OBSERV, MT HAMILTON, CA 95140 USA. RP ELLIOT, JL (reprint author), MIT, DEPT EARTH ATMOSPHER & PLANETARY SCI, CAMBRIDGE, MA 02139 USA. RI Lazzaro, Daniela/I-3509-2012 OI Lazzaro, Daniela/0000-0002-4470-6043 NR 24 TC 28 Z9 28 U1 0 U2 1 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JAN 5 PY 1995 VL 373 IS 6509 BP 46 EP 49 DI 10.1038/373046a0 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA QA239 UT WOS:A1995QA23900049 ER PT J AU THANEDAR, PB CHAMIS, CC AF THANEDAR, PB CHAMIS, CC TI RELIABILITY CONSIDERATIONS IN COMPOSITE LAMINATE TAILORING SO COMPUTERS & STRUCTURES LA English DT Article ID OPTIMIZATION AB In this study, a structural synthesis procedure has been developed to tailor composite laminates to meet the reliability-based (ply) strength requirements and achieve desirable laminate responses. Specifically, the main thrust of the paper is to demonstrate how to integrate optimization techniques in the probabilistic composite laminate tailoring process. The question of reliability arises in fiber composite analysis and design because of the inherent scatter that is observed in the constituent (fiber and matrix) material properties during experimentation. Symmetric and asymmetric composite laminates subject to mechanical loadings are considered as application examples. These application examples illustrate the effectiveness and ease with which reliability considerations can be integrated in the design optimization model for composite laminate tailoring. C1 NASA,LEWIS RES CTR,CLEVELAND,OH. RP THANEDAR, PB (reprint author), SAN JOSE STATE UNIV,SAN JOSE,CA 95192, USA. NR 14 TC 7 Z9 7 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0045-7949 J9 COMPUT STRUCT JI Comput. Struct. PD JAN 3 PY 1995 VL 54 IS 1 BP 131 EP 139 DI 10.1016/0045-7949(94)00302-J PG 9 WC Computer Science, Interdisciplinary Applications; Engineering, Civil SC Computer Science; Engineering GA QA558 UT WOS:A1995QA55800013 ER PT J AU ELLIS, J SCHRAMM, DN AF ELLIS, J SCHRAMM, DN TI COULD A NEARBY SUPERNOVA EXPLOSION HAVE CAUSED A MASS EXTINCTION SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article ID SOLAR ULTRAVIOLET-RADIATION; POLYETHYLENE BAGS; OZONE DEPLETION; GEMINGA AB We examine the possibility that a nearby supernova explosion could have caused one or more of the mass extinctions identified by paleontologists. We discuss the possible rate of such events in the light of the recent suggested identification of Geminga as a supernova remnant less than 100 parsec (pc) away and the discovery of a millisecond pulsar about 150 pc away and observations of SN 1987A. The fluxes of gamma-radiation and charged cosmic rays on the Earth are estimated, and their effects on the Earth's ozone layer are discussed. A supernova explosion of the order of 10 pc away could be expected as often as every few hundred million years and could destroy the ozone layer for hundreds of years, letting in potentially lethal solar ultraviolet radiation. In addition to effects on land ecology, this could entail mass destruction of plankton and reef communities, with disastrous consequences for marine life as well. A supernova extinction should be distinguishable from a meteorite impact such as the one that presumably killed the dinosaurs at the ''KT boundary.'' The recent argument that the KT event was exceedingly large and thus quite rare supports the need for other catastrophic events. C1 UNIV CHICAGO,DEPT ASTRON & ASTROPHYS,CHICAGO,IL 60637. FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. RP ELLIS, J (reprint author), CERN,EUROPEAN ORG NUCL RES,DIV THEORET PHYS,CH-1211 GENEVA 23,SWITZERLAND. NR 24 TC 63 Z9 64 U1 2 U2 19 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 JAN 3 PY 1995 VL 92 IS 1 BP 235 EP 238 DI 10.1073/pnas.92.1.235 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA QB238 UT WOS:A1995QB23800048 PM 11607506 ER PT J AU ASKER, JR AF ASKER, JR TI NASA CONFIRMS CFCS CAUSE OZONE LOSS SO AVIATION WEEK & SPACE TECHNOLOGY LA English DT Article RP ASKER, JR (reprint author), NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU MCGRAW HILL INC PI NEW YORK PA 1221 AVENUE OF THE AMERICAS, NEW YORK, NY 10020 SN 0005-2175 J9 AVIAT WEEK SPACE TEC JI Aviat. Week Space Technol. PD JAN 2 PY 1995 VL 142 IS 1 BP 58 EP 58 PG 1 WC Engineering, Aerospace SC Engineering GA QB299 UT WOS:A1995QB29900035 ER PT J AU MATSUDA, T SMITH, GD WINKLER, RG YOON, DY AF MATSUDA, T SMITH, GD WINKLER, RG YOON, DY TI STOCHASTIC DYNAMICS SIMULATIONS OF N-ALKANE MELTS CONFINED BETWEEN SOLID-SURFACES - INFLUENCE OF SURFACE-PROPERTIES AND COMPARISON WITH SCHEUTJENS-FLEER THEORY SO MACROMOLECULES LA English DT Article ID MONTE-CARLO SIMULATIONS; POLYMER MELTS; MOLECULAR ARRANGEMENTS; 2 PLATES; CONFORMATIONS; POLYMETHYLENE; MODEL AB Stochastic dynamics simulations of n-alkane melts (C13H28 and C28H58) confined between solid surfaces have been performed in order to study the influence of the surface structure and interactions on the structural and dynamic properties of the chain molecules at the interfaces. Moreover, these simulation results have been compared with the predictions of the Scheutjens-Fleer lattice theory in order to investigate the general applicability of the theory in predicting the conformational properties of real (atomistic) melt chains at the interfaces. The n-alkane chains are described as mass points (united atoms) linearly connected by rigid bonds and subjected to bond bending, torsional, and nonbonded interaction potentials. For repulsive surfaces, an atomistic, ordered surface was found to yield the same static and dynamic properties of the chains as a flat, structureless surface. The presence of a strongly attractive surface was found to increase layering of both monomers and entire n-alkane molecules at the surface. Chains with only ends strongly attractive to the surfaces (sticky ends) exhibited an increased probability of long tails and loops and a decreased probability of long trains. However, no significant change in the strong preference for trains comprised of entire molecules was seen. Comparison of neutral surface and sticky end simulations with Scheutjens-Fleer self-consistent-field lattice theory predictions revealed that the theory reproduces quite well the behavior of tails, loops, and trains seen from atomistic simulations of C28H58. C1 IBM CORP,ALMADEN RES CTR,SAN JOSE,CA 95120. UNITIKA CO LTD,CTR RES & DEV,UJI,KYOTO 611,JAPAN. NASA,AMES RES CTR,INST THERMOSCI,MOFFETT FIELD,CA 94035. UNIV ULM,THEORET PHYS ABT,W-7900 ULM,GERMANY. RI Winkler, Roland/G-4059-2013 OI Winkler, Roland/0000-0002-7513-0796 NR 24 TC 36 Z9 36 U1 1 U2 3 PU AMER CHEMICAL SOC PI WASHINGTON PA PO BOX 57136, WASHINGTON, DC 20037-0136 SN 0024-9297 J9 MACROMOLECULES JI Macromolecules PD JAN 2 PY 1995 VL 28 IS 1 BP 165 EP 173 DI 10.1021/ma00105a022 PG 9 WC Polymer Science SC Polymer Science GA QA750 UT WOS:A1995QA75000022 ER PT B AU Lowry, MR VanBaalen, J AF Lowry, MR VanBaalen, J GP IEEE COMP SOC TI META-AMPHION: Synthesis of efficient domain-specific program synthesis systems SO 10TH KNOWLEDGE-BASED SOFTWARE ENGINEERING CONFERENCE, PROCEEDINGS LA English DT Proceedings Paper CT 10th Knowledge-Based Software Engineering Conference CY NOV 12-15, 1995 CL BOSTON, MA SP USAF, Rome Lab, AAAI, ACM SIGART, ACM SIGSOFT, IEEE Comp Soc C1 NASA,AMES RES CTR,RECOM TECHNOL,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E, COMPUTER SOC PRESS PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, LOS ALAMITOS, CA 90720 BN 0-8186-7204-8 PY 1995 BP 2 EP 10 DI 10.1109/KBSE.1995.490113 PG 9 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering SC Computer Science GA BF53Q UT WOS:A1995BF53Q00001 ER PT S AU FAYYAD, UM AF FAYYAD, UM GP IEEE TI A MACHINE LEARNING APPROACH TO THE ANALYSIS OF LARGE IMAGE DATABASES SO 11TH CONFERENCE ON ARTIFICIAL INTELLIGENCE FOR APPLICATIONS, PROCEEDINGS SE PROCEEDINGS: CONFERENCE ON ARTIFICIAL INTELLIGENCE FOR APPLICATIONS LA English DT Proceedings Paper CT 11th Conference on Artificial Intelligence for Applications CY FEB 20-23, 1995 CL LOS ANGELES, CA SP IEEE, COMP SOC, TECH COMM PATTERN ANAL & MACHINE INTELLIGENCE C1 JET PROP LAB,MACHINE LEARNING SYST GRP,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E, COMPUTER SOC PRESS PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, LOS ALAMITOS, CA 90720 SN 1043-0989 BN 0-8186-7070-3 J9 PR CONF ART INT APPL PY 1995 BP R10 EP R10 PG 1 WC Computer Science, Artificial Intelligence SC Computer Science GA BC93C UT WOS:A1995BC93C00001 ER PT J AU ZINN, HP AF ZINN, HP GP AMER METEOROL SOC TI Lagrangian analysis of the upper general circulation SO 11TH SYMPOSIUM ON BOUNDARY LAYERS AND TURBULENCE LA English DT Proceedings Paper CT 11th Symposium on Boundary Layers and Turbulence CY MAR 27-31, 1995 CL CHARLOTTE, NC SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,GODDARD INST SPACE STUDIES,NEW YORK,NY 10025. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 200 EP 203 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BD28J UT WOS:A1995BD28J00057 ER PT J AU CONSIDINE, GD CURRY, JA AF CONSIDINE, GD CURRY, JA GP AMER METEOROL SOC TI Impact of boundary layer dynamics on cloud droplet spectra SO 11TH SYMPOSIUM ON BOUNDARY LAYERS AND TURBULENCE LA English DT Proceedings Paper CT 11th Symposium on Boundary Layers and Turbulence CY MAR 27-31, 1995 CL CHARLOTTE, NC SP Amer Meteorol Soc C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23665. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 244 EP 247 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BD28J UT WOS:A1995BD28J00069 ER PT J AU ZINN, HP AF ZINN, HP GP AMER METEOROL SOC TI An efficient planetary boundary layer model for general circulation models SO 11TH SYMPOSIUM ON BOUNDARY LAYERS AND TURBULENCE LA English DT Proceedings Paper CT 11th Symposium on Boundary Layers and Turbulence CY MAR 27-31, 1995 CL CHARLOTTE, NC SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,INST SPACE STUDIES,NEW YORK,NY 10025. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 270 EP 273 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BD28J UT WOS:A1995BD28J00074 ER PT S AU EVANS, JA PRUSHA, SL AF EVANS, JA PRUSHA, SL BE ElGenk, MS TI NASA MISSIONS OF THE FUTURE SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 7 EP 13 PN 1 & 2 PG 7 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00002 ER PT S AU JUHASZ, AJ ROVANG, RD AF JUHASZ, AJ ROVANG, RD BE ElGenk, MS TI DEVELOPMENT OF LIGHTWEIGHT PROTOTYPE CARBON-CARBON HEAT PIPE WITH INTEGRAL FINS AND METAL FOIL LINER SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 135 EP 143 PN 1 & 2 PG 9 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00020 ER PT S AU HARRIS, HM AF HARRIS, HM BE ElGenk, MS TI SCIENCE OPPORTUNITIES THROUGH NUCLEAR POWER IN SPACE SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 161 EP 168 PN 1 & 2 PG 8 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00023 ER PT S AU BOROWSKI, SK AF BOROWSKI, SK BE ElGenk, MS TI ROBOTIC PLANETARY SCIENCE MISSIONS ENABLED WITH SMALL NTR ENGINE STAGE TECHNOLOGIES SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 311 EP 319 PN 1 & 2 PG 9 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00046 ER PT S AU EMRICH, WJ AF EMRICH, WJ BE ElGenk, MS TI DESIGN CONSIDERATIONS FOR MARS TRANSFER VEHICLES USING NUCLEAR THERMAL PROPULSION SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 395 EP 400 PN 1 & 2 PG 6 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00058 ER PT S AU BOROWSKI, SK CULVER, DW BULMAN, MJ AF BOROWSKI, SK CULVER, DW BULMAN, MJ BE ElGenk, MS TI HUMAN EXPLORATION AND SETTLEMENT OF THE MOON USING LUNOX-AUGMENTED NTR PROPULSION SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 NASA,CLEVELAND,OH 44135. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 409 EP 420 PN 1 & 2 PG 12 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00060 ER PT S AU ROM, FE FINNEGAN, PM GUMTO, KH AF ROM, FE FINNEGAN, PM GUMTO, KH BE ElGenk, MS TI NASA-LEWIS IN-PILE HIGH TEMPERATURE REACTOR MELTDOWN CONTAINMENT EXPERIMENT SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 NASA,LERC,VENICE,FL 34292. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 577 EP 582 PN 1 & 2 PG 6 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00080 ER PT S AU TRUSCELLO, VC MONDT, JF FUJITA, T AF TRUSCELLO, VC MONDT, JF FUJITA, T BE ElGenk, MS TI COMMERCIAL TECHNOLOGIES FROM THE SP-100 PROGRAM SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 1 U2 1 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 633 EP 640 PN 1 & 2 PG 8 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00089 ER PT S AU PANT, A SERA, G AF PANT, A SERA, G BE ElGenk, MS TI COMMERCIALIZATION OF SOLAR SPACE POWER SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 TEXAS A&M UNIV,TEXAS ENGN EXTENS SERV,NASA,KMIDCONTINENT TECHNOL TRANSFER CTR,COLLEGE STN,TX 77843. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 669 EP 674 PN 1 & 2 PG 6 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00094 ER PT S AU DUKE, MB AF DUKE, MB BE ElGenk, MS TI A 1ST STEP TOWARD LUNAR DEVELOPMENT - PROJECT PELE SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 NASA,SA JOHNSON SPACE CTR,HOUSTON,TX 77058. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 987 EP 993 PN 1 & 2 PG 7 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00138 ER PT S AU LANDIS, GA BAILEY, SG AF LANDIS, GA BAILEY, SG BE ElGenk, MS TI ADVANCES IN SOLAR CELL TECHNOLOGY SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 1001 EP 1010 PN 1 & 2 PG 10 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00140 ER PT S AU LANDIS, GA BAILEY, SG AF LANDIS, GA BAILEY, SG BE ElGenk, MS TI USE OF ADVANCED SOLAR CELLS FOR COMMERCIAL COMMUNICATION SATELLITES SO 12TH SYMPOSIUM ON SPACE NUCLEAR POWER AND PROPULSION, PTS 1 AND 2 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 12th Symposium on Space Nuclear Power and Propulsion/Conference on Alternative Power from Space (APFS)/Conference on Accelerator-Driven Transmutation Technologies and Applications (A-DTTA) CY JAN 08-12, 1995 CL ALBUQUERQUE, NM SP INST SPACE & NUCL POWER STUDIES, BALLISTIC MISSILE DEF ORG, NASA, NASA, LEWIS RES CTR, US DOE, LOS ALAMOS NATL LAB, US DOE, SANDIA NATL LABS, USAF, PHILLIPS LAB, USAF, WRIGHT LAB, AMER INST AERONAUT & ASTRONAUT, AMER INST CHEM ENGINEERS, HEAT TRANSFER & ENERGY CONVERS DIV, AMER NUCL SOC, ANS TRINITY SECT, AMER SOC MECH ENGINEERS, NUCL ENGN DIV, AMER SOC MECH ENGINEERS, HEAT TRANSFER DIV, AMER SOC TESTING & MAT, COMM E 10 NUCL TECHNOL & APPL, INT ASTRONAUT FEDERAT, NEW MEXICO ACAD SCI C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-427-9 J9 AIP CONF PROC PY 1995 IS 324 BP 1011 EP 1015 PN 1 & 2 PG 5 WC Engineering, Aerospace; Energy & Fuels; Nuclear Science & Technology SC Engineering; Energy & Fuels; Nuclear Science & Technology GA BC86M UT WOS:A1995BC86M00141 ER PT B AU Jones, DR Young, SD AF Jones, DR Young, SD GP AMER INST AERONAUT & ASTRONAUT TI Flight demonstration of integrated airport surface automation concepts SO 14TH DASC - DIGITAL AVIONICS SYSTEMS CONFERENCE, AIAA/IEEE LA English DT Proceedings Paper CT AIAA/IEEE 14th Digital Avionics Systems Conference (14th DASC) CY NOV 05-09, 1995 CL CAMBRIDGE, MA SP Amer Inst Aeronaut & Astronaut, IEEE C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23681. NR 0 TC 1 Z9 1 U1 0 U2 2 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-3050-1 PY 1995 BP 77 EP 82 PG 6 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE61E UT WOS:A1995BE61E00013 ER PT B AU Brown, TK Donaldson, JA AF Brown, TK Donaldson, JA GP AMER INST AERONAUT & ASTRONAUT TI Fault protection architecture for the command and data subsystem on the Cassini Spacecraft SO 14TH DASC - DIGITAL AVIONICS SYSTEMS CONFERENCE, AIAA/IEEE LA English DT Proceedings Paper CT AIAA/IEEE 14th Digital Avionics Systems Conference (14th DASC) CY NOV 05-09, 1995 CL CAMBRIDGE, MA SP Amer Inst Aeronaut & Astronaut, IEEE C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-3050-1 PY 1995 BP 158 EP 163 PG 6 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE61E UT WOS:A1995BE61E00027 ER PT B AU Brown, GM Bernard, DE Rasmussen, RD AF Brown, GM Bernard, DE Rasmussen, RD GP AMER INST AERONAUT & ASTRONAUT TI Attitude and articulation control for the Cassini Spacecraft: A fault tolerance overview SO 14TH DASC - DIGITAL AVIONICS SYSTEMS CONFERENCE, AIAA/IEEE LA English DT Proceedings Paper CT AIAA/IEEE 14th Digital Avionics Systems Conference (14th DASC) CY NOV 05-09, 1995 CL CAMBRIDGE, MA SP Amer Inst Aeronaut & Astronaut, IEEE C1 CALTECH,JET PROP LAB,PASADENA,CA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-3050-1 PY 1995 BP 184 EP 192 PG 9 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE61E UT WOS:A1995BE61E00032 ER PT B AU Boyd, MA Monahan, CM AF Boyd, MA Monahan, CM GP AMER INST AERONAUT & ASTRONAUT TI Developing integrated hardware software reliability models: Difficulties and issues SO 14TH DASC - DIGITAL AVIONICS SYSTEMS CONFERENCE, AIAA/IEEE LA English DT Proceedings Paper CT AIAA/IEEE 14th Digital Avionics Systems Conference (14th DASC) CY NOV 05-09, 1995 CL CAMBRIDGE, MA SP Amer Inst Aeronaut & Astronaut, IEEE C1 NASA,AMES RES CTR,DIV COMPUTAT SCI,MOFFETT FIELD,CA 94035. NR 0 TC 1 Z9 1 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-3050-1 PY 1995 BP 193 EP 198 PG 6 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE61E UT WOS:A1995BE61E00033 ER PT B AU Hoy, HH Lam, T AF Hoy, HH Lam, T GP AMER INST AERONAUT & ASTRONAUT TI CH-47D computer graphics generated display monitor SO 14TH DASC - DIGITAL AVIONICS SYSTEMS CONFERENCE, AIAA/IEEE LA English DT Proceedings Paper CT AIAA/IEEE 14th Digital Avionics Systems Conference (14th DASC) CY NOV 05-09, 1995 CL CAMBRIDGE, MA SP Amer Inst Aeronaut & Astronaut, IEEE C1 NASA,AMES RES CTR,WESTERN AEREONAUT TEST RANGE BRANCH,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-3050-1 PY 1995 BP 311 EP 313 PG 3 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE61E UT WOS:A1995BE61E00050 ER PT B AU Shalom, E AF Shalom, E GP AMER INST AERONAUT & ASTRONAUT TI The Input Output Unit for the Attitude and Articulation Control Subsystem on the Cassini spacecraft SO 14TH DASC - DIGITAL AVIONICS SYSTEMS CONFERENCE, AIAA/IEEE LA English DT Proceedings Paper CT AIAA/IEEE 14th Digital Avionics Systems Conference (14th DASC) CY NOV 05-09, 1995 CL CAMBRIDGE, MA SP Amer Inst Aeronaut & Astronaut, IEEE C1 CALTECH,JET PROP LAB,AVION SYST & TECHNOL DIV,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-3050-1 PY 1995 BP 347 EP 352 PG 6 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE61E UT WOS:A1995BE61E00057 ER PT B AU Belcastro, CM Fischl, R AF Belcastro, CM Fischl, R GP AMER INST AERONAUT & ASTRONAUT TI Upset detection for closed-loop laboratory HIRF testing of fault tolerant aircraft control computers SO 14TH DASC - DIGITAL AVIONICS SYSTEMS CONFERENCE, AIAA/IEEE LA English DT Proceedings Paper CT AIAA/IEEE 14th Digital Avionics Systems Conference (14th DASC) CY NOV 05-09, 1995 CL CAMBRIDGE, MA SP Amer Inst Aeronaut & Astronaut, IEEE C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23681. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-3050-1 PY 1995 BP 438 EP 447 PG 10 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE61E UT WOS:A1995BE61E00072 ER PT B AU Holloway, CM AF Holloway, CM GP AMER INST AERONAUT & ASTRONAUT TI Ada 95 and safety-critical software SO 14TH DASC - DIGITAL AVIONICS SYSTEMS CONFERENCE, AIAA/IEEE LA English DT Proceedings Paper CT AIAA/IEEE 14th Digital Avionics Systems Conference (14th DASC) CY NOV 05-09, 1995 CL CAMBRIDGE, MA SP Amer Inst Aeronaut & Astronaut, IEEE C1 NASA,LANGLEY RES CTR,ASSESSMENT TECHNOL BRANCH,HAMPTON,VA 23681. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-3050-1 PY 1995 BP 504 EP 509 PG 6 WC Engineering, Aerospace; Engineering, Electrical & Electronic SC Engineering GA BE61E UT WOS:A1995BE61E00081 ER PT B AU Masuoka, PM Hoppin, AD Lowman, PD AF Masuoka, PM Hoppin, AD Lowman, PD GP AMER CONGRESS SURVEYING & MAPPING TI A study of the Sudbury Basin, Ontario, using radar combined with digital elevation data: Preliminary results SO 1995 ACSM/ASPRS ANNUAL CONVENTION & EXPOSITION TECHNICAL PAPERS, VOL 3: ASPRS LA English DT Proceedings Paper CT American-Congress-on-Surveying-and-Mapping 55th Annual Convention/American-Society-for-Photogrammetry-and-Remote-Sensing 61st Annual Convention CY FEB 27-MAR 02, 1995 CL CHARLOTTE, NC SP Amer Congress Surveying & Mapping, Amer Soc Photogrammetry & Remote Sensing C1 NASA,GODDARD SPACE FLIGHT CTR,TERR PHYS LAB,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER CONGRESS SURVEYING & MAPPING PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814-2122 BN 1-57083-017-7 PY 1995 BP 704 EP 713 PG 10 WC Remote Sensing SC Remote Sensing GA BF67F UT WOS:A1995BF67F00023 ER PT B AU PINCK, DS RICE, MD AF PINCK, DS RICE, MD GP IEEE TI K/Ka-band channel characterization for mobile satellite systems SO 1995 IEEE 45TH VEHICULAR TECHNOLOGY CONFERENCE - COUNTDOWN TO THE WIRELESS TWENTY-FIRST CENTURY, VOLS 1-2 LA English DT Proceedings Paper CT 1995 IEEE 45th Vehicular Technology Conference - Countdown to the Wireless 21st-Century CY JUL 25-28, 1995 CL CHICAGO, IL SP IEEE, Vehicular Technol Soc C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-2743-8 PY 1995 BP 981 EP 985 PG 3 WC Engineering, Electrical & Electronic; Remote Sensing; Telecommunications SC Engineering; Remote Sensing; Telecommunications GA BD74Z UT WOS:A1995BD74Z00196 ER PT B AU Duong, TA AF Duong, TA GP IEEE IEEE IEEE IEEE TI Cascade Error Projection: An efficient hardware learning algorithm SO 1995 IEEE INTERNATIONAL CONFERENCE ON NEURAL NETWORKS PROCEEDINGS, VOLS 1-6 LA English DT Proceedings Paper CT 1995 IEEE International Conference on Neural Networks (ICNN 95) CY NOV 27-DEC 01, 1995 CL UNIV W AUSTRAIA, PERTH, AUSTRALIA SP IEEE, Neural Networks Council HO UNIV W AUSTRAIA C1 CALTECH, JET PROP LAB, CTR SPACE MICROELECTR TECHNOL, PASADENA, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-2768-3; 0-7803-2769-1 PY 1995 BP 175 EP 178 PG 4 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BF46H UT WOS:A1995BF46H00034 ER PT B AU Lee, SH Huang, D AF Lee, SH Huang, D GP IEEE IEEE IEEE IEEE TI Dual-mode dynamics neural network (D2NN) for the traveling salesman problem SO 1995 IEEE INTERNATIONAL CONFERENCE ON NEURAL NETWORKS PROCEEDINGS, VOLS 1-6 LA English DT Proceedings Paper CT 1995 IEEE International Conference on Neural Networks (ICNN 95) CY NOV 27-DEC 01, 1995 CL UNIV W AUSTRAIA, PERTH, AUSTRALIA SP IEEE, Neural Networks Council HO UNIV W AUSTRAIA C1 CALTECH, JET PROP LAB, PASADENA, CA 91109 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA BN 0-7803-2768-3; 0-7803-2769-1 PY 1995 BP 1880 EP 1885 PG 6 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BF46H UT WOS:A1995BF46H00362 ER PT B AU JOHNSON, WW SCHROEDER, JA AF JOHNSON, WW SCHROEDER, JA GP IEEE TI Visual-motion cueing in the control of altitude SO 1995 IEEE INTERNATIONAL CONFERENCE ON SYSTEMS, MAN AND CYBERNETICS, VOLS 1-5 LA English DT Proceedings Paper CT 1995 IEEE International Conference on Systems, Man and Cybernetics - Intelligent Systems for the 21st-Century CY OCT 22-25, 1995 CL VANCOUVER, CANADA SP IEEE, Systems Man & Cybernet Soc C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-2560-5 PY 1995 BP 2676 EP 2681 PG 6 WC Computer Science, Artificial Intelligence; Computer Science, Cybernetics; Computer Science, Theory & Methods; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BE26Y UT WOS:A1995BE26Y00466 ER PT B AU Pinelli, TE Kennedy, JM Barclay, RO AF Pinelli, TE Kennedy, JM Barclay, RO GP IEEE TI Workplace communications skills and the value of communications and information use skills instruction - Engineering students' perspectives SO 1995 IEEE INTERNATIONAL PROFESSIONAL COMMUNICATION CONFERENCE, IPCC 95 PROCEEDINGS - SMOOTH SAILING TO THE FUTURE LA English DT Proceedings Paper CT 1995 IEEE International Professional Communication Conference - Smooth Sailing to the Future (IPCC 95) CY SEP 27-29, 1995 CL SAVANNAH, GA SP IEEE, Profess Commun Soc C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23681. NR 0 TC 0 Z9 0 U1 0 U2 1 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-2957-0 PY 1995 BP 161 EP 165 DI 10.1109/IPCC.1995.554892 PG 5 WC Communication; Engineering, Electrical & Electronic SC Communication; Engineering GA BE31H UT WOS:A1995BE31H00034 ER PT S AU CHREN, WA AF CHREN, WA GP IEEE TI One-hot residue coding for high-speed non-uniform pseudo-random test pattern generation SO 1995 IEEE INTERNATIONAL SYMPOSIUM ON CIRCUITS AND SYSTEMS, VOLS 1-3 SE IEEE INTERNATIONAL SYMP ON CIRCUITS AND SYSTEMS LA English DT Proceedings Paper CT 1995 IEEE International Symposium on Circuits and Systems (ISCAS-1995) CY APR 30-MAY 03, 1995 CL SEATTLE, WA SP IEEE Circuits & Syst Soc C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. NR 0 TC 2 Z9 2 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 SN 0277-674X BN 0-7803-2570-2 J9 IEEE INT SYMP CIRC S PY 1995 BP 401 EP 404 PG 4 WC Computer Science, Artificial Intelligence; Computer Science, Hardware & Architecture; Engineering, Manufacturing; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BD85N UT WOS:A1995BD85N00101 ER PT S AU YEH, PS MILLER, WH AF YEH, PS MILLER, WH GP IEEE TI Real time lossless data compression technology for remote-sensing and other applications SO 1995 IEEE INTERNATIONAL SYMPOSIUM ON CIRCUITS AND SYSTEMS, VOLS 1-3 SE IEEE INTERNATIONAL SYMP ON CIRCUITS AND SYSTEMS LA English DT Proceedings Paper CT 1995 IEEE International Symposium on Circuits and Systems (ISCAS-1995) CY APR 30-MAY 03, 1995 CL SEATTLE, WA SP IEEE Circuits & Syst Soc C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NR 0 TC 1 Z9 2 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 SN 0277-674X BN 0-7803-2570-2 J9 IEEE INT SYMP CIRC S PY 1995 BP 1098 EP 1101 PG 4 WC Computer Science, Artificial Intelligence; Computer Science, Hardware & Architecture; Engineering, Manufacturing; Engineering, Electrical & Electronic SC Computer Science; Engineering GA BD85N UT WOS:A1995BD85N00275 ER PT S AU BAUTISTA, JJ HAMAI, M NISHIMOTO, M LASKAR, J SZYDLIK, P LAI, R AF BAUTISTA, JJ HAMAI, M NISHIMOTO, M LASKAR, J SZYDLIK, P LAI, R BE Kirby, L TI ULTRA-LOW NOISE HEMT DEVICE MODELS - APPLICATION OF ON-WAFER CRYOGENIC NOISE ANALYSIS AND IMPROVED PARAMETER EXTRACTION TECHNIQUES SO 1995 IEEE MTT-S INTERNATIONAL MICROWAVE SYMPOSIUM DIGEST, VOLS 1-3 SE IEEE MTT-S INTERNATIONAL MICROWAVE SYMPOSIUM DIGEST LA English DT Proceedings Paper CT 1995 IEEE MTT-S International Microwave Symposium CY MAY 16-20, 1995 CL ORLANDO, FL SP IEEE, Microwave Theory & Tech Soc C1 JET PROP LAB,PASADENA,CA 91109. NR 0 TC 1 Z9 1 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 SN 0149-645X BN 0-7803-2582-6 J9 IEEE MTT-S PY 1995 BP 935 EP 938 PG 4 WC Engineering, Electrical & Electronic SC Engineering GA BD21N UT WOS:A1995BD21N00217 ER PT S AU PEREZ, RM HOPPE, DJ KHAN, AR AF PEREZ, RM HOPPE, DJ KHAN, AR BE Kirby, L TI HIGH POWER AMPLIFIER HARMONIC OUTPUT LEVEL MEASUREMENT SO 1995 IEEE MTT-S INTERNATIONAL MICROWAVE SYMPOSIUM DIGEST, VOLS 1-3 SE IEEE MTT-S INTERNATIONAL MICROWAVE SYMPOSIUM DIGEST LA English DT Proceedings Paper CT 1995 IEEE MTT-S International Microwave Symposium CY MAY 16-20, 1995 CL ORLANDO, FL SP IEEE, Microwave Theory & Tech Soc C1 JET PROP LAB,PASADENA,CA 91109. NR 0 TC 1 Z9 1 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 SN 0149-645X BN 0-7803-2582-6 J9 IEEE MTT-S PY 1995 BP 1609 EP 1611 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA BD21N UT WOS:A1995BD21N00375 ER PT B AU BORDEN, T BLAKELY, M ALKALAJ, L AF BORDEN, T BLAKELY, M ALKALAJ, L GP ISHM - THE MICROELECTRONICS SOC TI THERMAL AND STRUCTURAL ANALYSIS OF THE ADVANCED FLIGHT COMPUTER MULTICHIP MODULE SO 1995 INTERNATIONAL CONFERENCE ON MULTICHIP MODULES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT 1995 International Conference on Multichip Modules CY APR 19-21, 1995 CL DENVER, CO SP ISHM, The Microelectronics Soc, Int Electr Packaging Soc, Electr Ind Assoc, IEEE, Components Packaging & Mfg Technol Soc, Semiconductor Equipment & Mat Int, Personal Comp Memory Card Int Assoc C1 JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-930815-42-4 J9 P SOC PHOTO-OPT INS PY 1995 VL 2575 BP 12 EP 17 PG 6 WC Engineering, Manufacturing; Engineering, Electrical & Electronic; Materials Science, Ceramics; Materials Science, Coatings & Films SC Engineering; Materials Science GA BD26Z UT WOS:A1995BD26Z00003 ER PT B AU Garrison, A Shaw, H Banker, J Miller, R Stopper, H AF Garrison, A Shaw, H Banker, J Miller, R Stopper, H GP MICROELECTRON SOC TI Flexible, cost-effective multichip modules for space applications SO 1995 INTERNATIONAL SYMPOSIUM ON MICROELECTRONICS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT 1995 International Symposium on Microelectronics CY OCT 24-26, 1995 CL LOS ANGELES, CA SP Microelectron Soc, Soc Photo Opt Instrumentat Engineers DE multichip module; antifuse; programmable substrate; rapid prototyping; reliability C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-930815-44-0 J9 P SOC PHOTO-OPT INS PY 1995 VL 2649 BP 257 EP 259 PG 3 WC Engineering, Electrical & Electronic; Materials Science, Multidisciplinary; Optics SC Engineering; Materials Science; Optics GA BE81F UT WOS:A1995BE81F00045 ER PT J AU Peterson, WL AF Peterson, WL GP SOC ALLIED WEIGHTS ENGINEERS, INC TI Using Microsoft Excel and Word as weight control tools SO 1995 SAWE CONFERENCE PAPERS LA English DT Proceedings Paper CT 54th Annual International Conference of Society-of-Allied-Weights-Engineers CY MAY 22-24, 1995 CL HUNTSVILLE, AL SP Soc Allied Weights Engineers Inc C1 NASA,LYNDON B JOHNSON SPACE CTR,HOUSTON,TX 77058. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOCIETY ALLIED WEIGHTS ENGINEERS PI LA MESA PA 5530 AZTEC DR, LA MESA, CA 91942 PY 1995 BP 267 EP 279 PG 13 WC Engineering, Aerospace SC Engineering GA BE84B UT WOS:A1995BE84B00009 ER PT J AU Peterson, WL AF Peterson, WL GP SOC ALLIED WEIGHTS ENGINEERS, INC TI Putting the SAWE on the Internet SO 1995 SAWE CONFERENCE PAPERS LA English DT Proceedings Paper CT 54th Annual International Conference of Society-of-Allied-Weights-Engineers CY MAY 22-24, 1995 CL HUNTSVILLE, AL SP Soc Allied Weights Engineers Inc C1 NASA,LYNDON B JOHNSON SPACE CTR,HOUSTON,TX 77058. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOCIETY ALLIED WEIGHTS ENGINEERS PI LA MESA PA 5530 AZTEC DR, LA MESA, CA 91942 PY 1995 BP 323 EP 342 PG 20 WC Engineering, Aerospace SC Engineering GA BE84B UT WOS:A1995BE84B00012 ER PT S AU Brown, JA AF Brown, JA GP AACE INT TI 240 aerospace cost indexes and escalation SO 1995 TRANSACTIONS OF AACE INTERNATIONAL - PROCEEDINGS OF THE 39TH ANNUAL MEETING OF AACE INTERNATIONAL SE TRANSACTIONS OF THE AMERICAN ASSOCIATION OF COST ENGINEERS LA English DT Proceedings Paper CT 39th Annual Meeting of the AACE-International CY JUN 25-28, 1995 CL ST LOUIS, MO SP Amer Assoc Cost Engineers Int C1 NASA,KENNEDY SPACE CTR,FL 32899. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER ASSOC COST ENGINEERS PI MORGANTOWN PA 209 PRAIRIE AVE, SUITE 100, PO BOX 1557, MORGANTOWN, WV 26507-1557 SN 0065-7158 BN 1-885517-01-7 J9 TRANS ANNU MEET AMER PY 1995 BP 132 EP 137 PG 6 WC Engineering, Industrial SC Engineering GA BF66A UT WOS:A1995BF66A00031 ER PT B AU Wilson, LF Nicol, DM AF Wilson, LF Nicol, DM BE Alexopoulos, C Kang, K Lilegdon, WR Goldsman, D TI Automated load balancing in SPEEDES SO 1995 WINTER SIMULATION CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 1995 Winter Simulation Conference CY DEC 03-06, 1995 CL ARLINGTON, VA C1 NASA,LANGLEY RES CTR,INST COMP APPLICAT SCI & ENGN,HAMPTON,VA 23681. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-3018-8 PY 1995 BP 590 EP 596 PG 7 WC Computer Science, Interdisciplinary Applications; Engineering, Industrial; Engineering, Manufacturing SC Computer Science; Engineering GA BE92P UT WOS:A1995BE92P00092 ER PT B AU Chamberlain, RG Braun, JE Firnett, PJ AF Chamberlain, RG Braun, JE Firnett, PJ BE Alexopoulos, C Kang, K Lilegdon, WR Goldsman, D TI Byning the earth SO 1995 WINTER SIMULATION CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 1995 Winter Simulation Conference CY DEC 03-06, 1995 CL ARLINGTON, VA C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-3018-8 PY 1995 BP 1215 EP 1221 PG 7 WC Computer Science, Interdisciplinary Applications; Engineering, Industrial; Engineering, Manufacturing SC Computer Science; Engineering GA BE92P UT WOS:A1995BE92P00186 ER PT B AU Yang, S Lau, KM SankarRao, M AF Yang, S Lau, KM SankarRao, M GP AMER METEOROL SOC TI Variability of the Asian monsoon: Phenomena and mechanisms SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 38 EP 40 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00015 ER PT J AU Chao, WC Deng, LT AF Chao, WC Deng, LT GP AMER METEOROL SOC TI On the origin of the Madden-Julian oscillation SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. NR 0 TC 2 Z9 2 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 156 EP 157 PG 2 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00058 ER PT B AU Lau, WKM Wu, HT AF Lau, WKM Wu, HT GP AMER METEOROL SOC TI Local and remote forcings associated with tropical convection, atmospheric wind divergence and sea surface temperature SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 158 EP 160 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00059 ER PT J AU Tokay, A Short, DA Williams, CR Ecklund, WL Gage, KS AF Tokay, A Short, DA Williams, CR Ecklund, WL Gage, KS GP AMER METEOROL SOC TI Intercomparison of convective vs stratiform precipitation classification from surface measured drop size distributions and wind profiler data SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,TRMM OFF,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 263 EP 266 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00097 ER PT J AU Short, DA Kucera, PA Thiele, OW AF Short, DA Kucera, PA Thiele, OW GP AMER METEOROL SOC TI Patterns of rainfall from shipborne radar data for the COARE Intensive Observing Period SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,TROP RAINFALL MEASURING MISSION,ATMOSPHERES LAB,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 273 EP 276 PG 4 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00100 ER PT J AU Wang, Y Tao, WK Simpson, J AF Wang, Y Tao, WK Simpson, J GP AMER METEOROL SOC TI The impact of ocean surface fluxes on a cloud system development SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 277 EP 279 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00101 ER PT J AU Hsu, CS Liu, WT AF Hsu, CS Liu, WT GP AMER METEOROL SOC TI Tropical cyclone intensity from scatterometer winds SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 286 EP 288 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00104 ER PT J AU Heymsfield, GM Shepherd, JM Spinhirne, J AF Heymsfield, GM Shepherd, JM Spinhirne, J GP AMER METEOROL SOC TI Vertical precipitation structure obtained from ER-2 remote sensing observations for the COARE 22 February 1993 case SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NR 0 TC 1 Z9 1 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 289 EP 291 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00105 ER PT J AU Rodgers, EB Pierce, H Adler, RF AF Rodgers, EB Pierce, H Adler, RF GP AMER METEOROL SOC TI Tropical cyclones' contribution to climatological rainfall as obtained from satellites SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 348 EP 350 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00126 ER PT J AU Karyampudi, VM Lai, G Manobianco, J Koch, S AF Karyampudi, VM Lai, G Manobianco, J Koch, S GP AMER METEOROL SOC TI Sensitivity of Hurricane Florence (1988) development to initial conditions, assimilation of satellite-derived rainfall rates and convective parameterization schemes SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,SCI SYST APPLICAT INC,ATMOSPHERES LAB,GREENBELT,MD 20771. NR 0 TC 1 Z9 1 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 386 EP 388 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00140 ER PT B AU Sui, CH Lau, KM Takayabu, Y AF Sui, CH Lau, KM Takayabu, Y GP AMER METEOROL SOC TI Multi-scale air-sea exchanges in TOGA-COARE SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 515 EP 517 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00184 ER PT J AU Chou, SH Shie, CL Atlas, RM Ardizzone, J AF Chou, SH Shie, CL Atlas, RM Ardizzone, J GP AMER METEOROL SOC TI Impact of the December 1992 westerly wind burst on evaporation determined from SSMI data SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 535 EP 537 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00192 ER PT B AU Krishnakumar, V Lau, KM AF Krishnakumar, V Lau, KM GP AMER METEOROL SOC TI Possible role of symmetric instability in monsoon transition SO 21ST CONFERENCE ON HURRICANES AND TROPICAL METEOROLOGY LA English DT Proceedings Paper CT 21st Conference on Hurricanes and Tropical Meteorology CY APR 24-28, 1995 CL MIAMI, FL SP Amer Meteorol Soc C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. RI Lau, William /E-1510-2012 OI Lau, William /0000-0002-3587-3691 NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108 PY 1995 BP 594 EP 596 PG 3 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA BF11X UT WOS:A1995BF11X00212 ER PT B AU Krizmanic, JF Davis, AJ Barbier, LM Christian, ER Golden, RL Hof, M Krombel, KE Labrador, AW Mewaldt, RA Mitchell, JW Ormes, JF Rasmussen, IL Reimer, O Schindler, SM Simon, M Stochaj, SJ Streitmatter, RE Webber, WR AF Krizmanic, JF Davis, AJ Barbier, LM Christian, ER Golden, RL Hof, M Krombel, KE Labrador, AW Mewaldt, RA Mitchell, JW Ormes, JF Rasmussen, IL Reimer, O Schindler, SM Simon, M Stochaj, SJ Streitmatter, RE Webber, WR GP INT UNION PURE & APPL PHYS TI Measurement of the cosmic ray induced muon flux through the atmosphere using IMAX SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 1: HE SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB Measurements of both the positive and negative components of the atmospheric muon flux have been performed using the Isotope Matter Antimatter eXperiment (IMAX). The experiment was flown from Lynn Lake, Manitoba, Canada (56 degrees latitude, geomagnetic cutoff approximate to 100 MV) on July 16-17, 1992 and experienced a 7+ hour ascent from approximately 0.3 km to 36 bm above sea level. Preliminary measurements of the muon flux and charge ratio in the momentum interval 0.42 --> 0.47 GeV/c at the top of instrument (TOI) as a function of atmospheric depth are presented. The relevance of these results in the context of the atmospheric neutrino anomaly is discussed. RP Krizmanic, JF (reprint author), NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771, USA. RI Christian, Eric/D-4974-2012 OI Christian, Eric/0000-0003-2134-3937 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 593 EP 596 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94B UT WOS:A1995BG94B00159 ER PT J AU Bhat, PN Fishman, GJ Meegan, CA Wilson, RB Paciesas, WS AF Bhat, PN Fishman, GJ Meegan, CA Wilson, RB Paciesas, WS GP INT UNION PURE & APPL PHYS TI Morphological study of short gamma ray bursts SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 2: OG SESSIONS (OG 1 - OG 6) - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB Gamma Ray Bursts (GRB) of duration less than about 2 s, detected by the Burst and Transient Source Experiment (BATSE) on board the Compton Gamma Ray Observatory have been selected for temporal analysis. These bursts constitute nearly 25% of the total and presumably form a separate class. Several parameters to describe the complexity and rapidity based on the burst temporal structure are derived and their dependence on other temporal and spectral properties are explored. A parameter is derived for each burst to characterize its spectral evolution based on its Light curves in 4 energy channels. Bursts detected during April 1991. and March 1993 have been analysed yielding a sample size of 51 bursts. It has been found that the burst complexity is independent of its spectral content. The spectral evolution of short sh bursts Is same as that of longer bursts. Also a systematic search for a coherent emission of gamma- rays in short bursts yielded a negative result. RP Bhat, PN (reprint author), NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB,ES-66,HUNTSVILLE,AL 35812, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 53 EP 56 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94C UT WOS:A1995BG94C00014 ER PT J AU Graziani, C Lamb, DQ AF Graziani, C Lamb, DQ GP INT UNION PURE & APPL PHYS TI Likelihood methods and classical burster repetition SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 2: OG SESSIONS (OG 1 - OG 6) - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB We develop a likelihood methodology which can be used to search for evidence of burst repetition in the BATSE catalog, and to study the properties of the repetition signal. We use a simplified model of burst repetition in which a number N-r of sources which repeat a fixed number of times N-rep are superposed upon a number N-nr of non-repeating sources. The instrument exposure is explicitly taken into account. By computing the likelihood for the data, we construct a probability distribution in parameter space that may be used to infer the probability that a repetition signal is present, and to estimate the values of the repetition parameters. The likelihood function contains contributions from all the bursts, irrespective of the size of their positional errors - the more uncertain a burst's position is, the less constraining is its contribution. Thus this approach makes maximal use of the data, and avoids the ambiguities of sample selection associated with data cuts on error circle size. We present the results of tests of the technique using synthetic data sets. RP Graziani, C (reprint author), NASA,GODDARD SPACE FLIGHT CTR,NRC,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 84 EP 87 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94C UT WOS:A1995BG94C00022 ER PT B AU Hunter, SD AF Hunter, SD GP INT UNION PURE & APPL PHYS TI EGRET observations of the galactic plane diffuse radiation and implications for the cosmic ray electron to proton ratio SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 2: OG SESSIONS (OG 1 - OG 6) - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB Observations with the EGRET telescope reveal the extensive, high-energy gamma ray emission which results from cosmic ray interactions with the photons and interstellar matter in the Galaxy. The spectrum of this diffuse emission yields information about the distribution of cosmic rays in the Galaxy. The average spectrum from the Galactic center region is compared with the prediction of the diffuse gamma-ray emission model of Bertsch et al. [1,2]. The discrepancy between the observed gamma-ray spectrum and the calculated spectrum above about 1 GeV provides evidence that the Galactic average cosmic-ray spectrum is different from the local cosmic-ray spectrum. Below 1 GeV, the calculated spectrum agrees well with the observed spectrum. RP Hunter, SD (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. RI Hunter, Stanley/D-2942-2012 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 182 EP 185 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94C UT WOS:A1995BG94C00047 ER PT B AU Baring, MG Harding, AK AF Baring, MG Harding, AK GP INT UNION PURE & APPL PHYS TI Photon splitting in neutron star magnetospheres SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 2: OG SESSIONS (OG 1 - OG 6) - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB The exotic process of photon splitting could be responsible for the softness of emission in soft gamma repeaters (SGRs), if these sources originate in neutron stars with surface fields above the quantum critical field B-cr = 4.413 x 10(13) Gauss. This process becomes prolific at such field strengths, and its principal effect is to degrade photon energies and thereby soften gamma-ray spectra from neutron stars, in particular down to observed SGR energies for fields exceeding about 100 TeraGauss. Here we consider the influence of the curved dipole field geometry of a neutron star magnetosphere on the photon splitting attenuation length. The dependence of this length on the location of the seed photons and their angular distribution is explored. The calculation is also applied to pulsar scenarios, where the seed photons are hard gamma-rays that are initially beamed close to the field lines. The comparative importance of splitting and single-photon magnetic pair production is assessed. RP Baring, MG (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,CODE 665,GREENBELT,MD 20771, USA. RI Harding, Alice/D-3160-2012 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 271 EP 274 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94C UT WOS:A1995BG94C00070 ER PT J AU ONeill, PM Badhwar, GD AF ONeill, PM Badhwar, GD GP INT UNION PURE & APPL PHYS TI Helium-3 local interstellar spectra derived by demodulating measured spectra SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 2: OG SESSIONS (OG 1 - OG 6) - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB Study of the secondary deuterons and helium-3 provides key parameters related to the propagation of cosmic radiation in the local interstellar (LI) medium. Measurements of helium-3 are relatively clean compared to deuteron measurements and as such provide a more accurate measure of interstellar path length. However, these measurements are made inside the solar system and as such are subject to effects of solar modulation that depend on the charge-to-mass ratio of the particle. In order, therefore, to construct a local interstellar spectrum (LIS) for helium-3, observations taken over different times and different solar cycles have to be combined. By a systematic study of the measured differential energy spectra of protons, helium, oxygen, and iron nuclei taken from 1954 to 1990, we developed a self-consistent model that given the deceleration parameter, phi (MV), provides the galactic cosmic spectra of primary nuclei to root-mean-square accuracy of +/- 10%. We also showed that phi can be derived from the Climax neutron count rates, if the sign of the interplanetary magnetic field, and time delay is taken into account. We have applied this model to all of the observed helium-3 and helium (3+4) measurements in a consistent manner to derive the LIS of helium-3. This spectrum is compared to ''leaky box'' model predictions. RP ONeill, PM (reprint author), NASA,LYNDON B JOHNSON SPACE CTR,HOUSTON,TX 77058, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 610 EP 613 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94C UT WOS:A1995BG94C00159 ER PT B AU Mitchell, JW Barbier, LM Christian, ER Davis, AJ Golden, RL Hof, M Krombel, KE Labrador, AW Menn, W Mewaldt, RA Ormes, JF Rasmussen, IL Reimer, O Schindler, SM Simon, M Stochaj, SJ Streitmatter, RE Webber, WR AF Mitchell, JW Barbier, LM Christian, ER Davis, AJ Golden, RL Hof, M Krombel, KE Labrador, AW Menn, W Mewaldt, RA Ormes, JF Rasmussen, IL Reimer, O Schindler, SM Simon, M Stochaj, SJ Streitmatter, RE Webber, WR GP INT UNION PURE & APPL PHYS TI Cosmic ray antiproton observations by the isotope matter-antimatter experiment; 0.2 to 3.2 GeV SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 3: OG SESSIONS (OG 7 - OG 11), CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB We have positively identified sixteen mass-resolved cosmic ray antiprotons with energies between 0.2 and 3.2 GeV using the IMAX balloon-borne magnetic spectrometer. Mass was determined by velocity vs. magnetic rigidity techniques using a high resolution time-of-flight system and silica aerogel Cherenkov detectors. The antiprotons are clearly separated from the low-mass particle background. Here the measurement technique, data analysis, and resulting proton and antiproton mass histograms are presented. RP Mitchell, JW (reprint author), NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771, USA. RI Christian, Eric/D-4974-2012 OI Christian, Eric/0000-0003-2134-3937 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 72 EP 75 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94D UT WOS:A1995BG94D00019 ER PT J AU Ormes, JF AF Ormes, JF GP INT UNION PURE & APPL PHYS TI A search for cosmic ray antihelium with BESS SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 3: OG SESSIONS (OG 7 - OG 11), CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB We have searched for antihelium in the Galactic Cosmic Rays using data obtained on two flights of the Balloon-borne Experiment with a Superconducting magnetic rigidity Spectrometer (BESS) flown in 1993 and 1994 [1]. No antihelium was observed after selection based on dE/dx, beta and track quality at rigidities between 1 and 19 GV/c. Combined, these flights give an upper limit to the <(HE)over bar /He> ratio of 8. x 10(-6) (95% C.L.) in the cosmic radiation at the top of the atmosphere. RP Ormes, JF (reprint author), NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 92 EP 95 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94D UT WOS:A1995BG94D00024 ER PT J AU Baring, MG Ogilvie, KW Ellison, DC AF Baring, MG Ogilvie, KW Ellison, DC GP INT UNION PURE & APPL PHYS TI Spectral comparison of Monte Carlo simulations of particle acceleration with Ulysses observations of nearby interplanetary shocks SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 3: OG SESSIONS (OG 7 - OG 11), CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB Recent developments in the simulation of particle acceleration at oblique collisionless shocks by the Monte Carlo technique have included the treatment of cases of strong scattering. The simulations make definitive predictions of the spectra of accelerated particles; in this paper we compare such predictions with observations of proton and helium distributions made by the SWIGS ion mass spectrometer on the Ulysses spacecraft at nearby interplanetary shocks. Upstream measurements of the solar wind and magnetic field determine the shock parameters, and the input particles are drawn from convected Maxwellians, representing solar wind particles. Good agreement between simulation predictions and downstream spectral measurements is obtained by allowing the ratio of the mean free path length for scattering to the proton gyroradius to vary to optimize the fit to the data; in the case of the April 7, 1991 shock this ratio is around 4, corresponding to the case of strong scattering. RP Baring, MG (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 229 EP 232 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94D UT WOS:A1995BG94D00059 ER PT J AU Baring, MG Riitano, AM AF Baring, MG Riitano, AM GP INT UNION PURE & APPL PHYS TI Test particle energy gains at oblique shocks using the adiabatic approximation SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 3: OG SESSIONS (OG 7 - OG 11), CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB The adiabatic approximation is a popular and convenient choice in models of diffusive shock acceleration for describing how particles reflect off and transmit through shock transitions. Discontinuous shocks violate the principle of the adiabatic assumption, since the field structure varies on scales that are smaller than a particle's gyroradius. The seriousness of this violation can be assessed by comparing flux-weighted average energy gains for particles interacting with the shock as calculated using the adiabatic approximation and also using gyrohelix computations. These averages are principal quantities influencing the shape of the distribution of accelerated particles. In this paper, we derive the expressions for these average energy gains under the adiabatic approximation for later use in energy gain comparisons. This is the first work to obtain such flux-weighted averages for general particle speeds in non-relativistic shocks. RP Baring, MG (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,CODE 665,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 289 EP 292 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94D UT WOS:A1995BG94D00074 ER PT J AU Wiedenbeck, ME Milliken, B AF Wiedenbeck, ME Milliken, B GP INT UNION PURE & APPL PHYS TI Balloon flight tests of a gas-ionization-chamber-based isotope spectrometer SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 3: OG SESSIONS (OG 7 - OG 11), CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB The performance of the ''Tracking Heavy Isotope Spectrometer Telescope for Low Energies'' (THISTLE) is being investigated using data from a balloon flight carried out in 1993. We discuss the instrument design and show examples of its operation. Results of additional analysis will be presented at the conference. RP Wiedenbeck, ME (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 611 EP 614 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94D UT WOS:A1995BG94D00155 ER PT B AU Christian, ER Mitchell, JW Baker, R Goodwin, P Nace, R Smith, R AF Christian, ER Mitchell, JW Baker, R Goodwin, P Nace, R Smith, R GP INT UNION PURE & APPL PHYS TI A telemetry/frame sync board for use in balloon payloads SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 3: OG SESSIONS (OG 7 - OG 11), CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB We have designed and built a telemetry/frame synchronizer board for use on the ISOMAX balloon experiment that may also have application in other payloads. The ISOMAX telemetry board is software configurable to either transmit or receive telemetry and commands, or send or receive a test pattern. The board is PC-ISA based and versions exist in a PC/104 form factor and on an AT card The boards include dual 1K x 16 bit FIFOs for transmit and receive with half full flags that can generate an interrupt. A 16-bit CRC can also be automatically generated at the end of each frame. RP Christian, ER (reprint author), NASA,GODDARD SPACE FLIGHT CTR,CODE 660,GREENBELT,MD 20771, USA. RI Christian, Eric/D-4974-2012 OI Christian, Eric/0000-0003-2134-3937 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 623 EP 626 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94D UT WOS:A1995BG94D00158 ER PT J AU Derrickson, JH Eby, PB Parnell, TA Wu, JS Gregory, JC Takahashi, Y AF Derrickson, JH Eby, PB Parnell, TA Wu, JS Gregory, JC Takahashi, Y GP INT UNION PURE & APPL PHYS TI Direct Coulomb electron pairs for energy measurement - Design considerations SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 3: OG SESSIONS (OG 7 - OG 11), CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB Direct Coulomb electron pairs produced along heavy ion tracks occur with sufficient frequency above approximate to 10(13) eV/n to allow consideration of this effect for energy measurements. Recent calculations and experimental measurements have resolved earlier discrepancies between various calculations and measurements, and possible background effects have been extensively investigated. Characteristics of the direct pairs and the principal background (knock-on electrons) are discussed. Calculations and simulations fdr a particular passive detector arrangement are described. RP Derrickson, JH (reprint author), NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 641 EP 644 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94D UT WOS:A1995BG94D00162 ER PT J AU Ng, CK Reames, DV AF Ng, CK Reames, DV GP INT UNION PURE & APPL PHYS TI Interplanetary transport coefficient in an extended quasi-linear theory SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB We study the effect of the medium-scale fluctuation of the interplanetary magnetic held (IMF) on the transport of 'solar' energetic protons (SEP) in an extended quasi-linear theory (EQLT). This significantly broadens the wave-particle resonance function for SEP, removing the resonance gap and infinite mean free path lambda predicted by the standard quasi-linear theory (SQLT) in the presence of wave dissipation. RP Ng, CK (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,CODE 661,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 253 EP 256 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00068 ER PT J AU Barbier, LM Ng, CK Reames, DV AF Barbier, LM Ng, CK Reames, DV GP INT UNION PURE & APPL PHYS TI Multispacecraft studies of coronal mass ejection associated energetic particle events SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB The observations of energetic particle events associated with Coronal Mass Ejections (CMEs) from single spacecraft are limited since they cannot distinguish spatial and temporal variations. We examine several multispacecraft particle intensity time profiles in CME associated events, and show how the most important features in the intensity profiles (gradual or sharp rise, etc.) can be explained simply by understanding where the spacecraft magnetically connects to the CME driven shock relative to the ejecta. Interestingly enough, we find that well behind the CME shock even widely separated spacecraft see the same intensity profiles. RP Barbier, LM (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,CODE 661,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 365 EP 368 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00096 ER PT J AU Richardson, IG Cane, HV AF Richardson, IG Cane, HV GP INT UNION PURE & APPL PHYS TI Anisotropies of solar particle onsets observed within ejecta SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB Around 30% of solar energetic particle events which onset inside ejecta exhibit unusual flows from the east of the Sun. Such flows are rarely found in similar events outside ejecta. The observations are consistent with the presence of looped magnetic structures in ejecta. RP Richardson, IG (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 373 EP 376 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00098 ER PT B AU Cane, HV Richardson, IG Wibberenz, G AF Cane, HV Richardson, IG Wibberenz, G GP INT UNION PURE & APPL PHYS TI The response of energetic particles to the presence of ejecta material SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB We have made a study of the behaviour of particle densities during the passage of ejecta Ejecta may cause deceases at all energies. Inside ejecta, up to rigidities of about 0.5 GV, the intensity drops to <30% of the pre-ejecta level At high rigidities the size of the decrease is proportional to similar to P--0.7. For a sample of smaller, less energetic events the size of the decrease is proportional to the maximum magnetic field strength in the ejecta We investigate the predictions of a simple model in which a cylinder gradually Ils with particles via perpendicular diffusion. RP Cane, HV (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 377 EP 380 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00099 ER PT B AU Christian, ER Cummings, AC Stone, EC AF Christian, ER Cummings, AC Stone, EC GP INT UNION PURE & APPL PHYS TI The reappearance of anomalous cosmic ray hydrogen SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB New observations from the Cosmic Ray Subsystem (CRS) on the Voyager spacecraft clearly show that anomalous cosmic ray hydrogen has reappeared, clearing up a controversy that has existed since the previous solar minimum [1, 2]. The new observations are consistent with the evidence for anomalous cosmic ray hydrogen seen in the 1987 solar minimum. Comparison of the anomalous and galactic cosmic ray modulation for the two solar minima indicates that there is substantial modulation of the galactic cosmic rays beyond the solar wind termination shock. RP Christian, ER (reprint author), NASA,GODDARD SPACE FLIGHT CTR,CODE 661,GREENBELT,MD 20771, USA. RI Christian, Eric/D-4974-2012 OI Christian, Eric/0000-0003-2134-3937 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 816 EP 819 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00222 ER PT J AU Richardson, IG Cane, HV AF Richardson, IG Cane, HV GP INT UNION PURE & APPL PHYS TI Regions of abnormally low proton temperature as signatures of ejecta in the solar wind and their solar cycle dependence SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB We show that the occurrence of intervals of abnormally low proton temperatures in the OMNI solar wind data from 1965 to 1990 is correlated with solar activity levels, and discuss the association of such regions with other ejecta-associated phenomena such as bidirectional particle flows and ''local'' high energy particle depressions. RP Richardson, IG (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 868 EP 871 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00235 ER PT J AU Cane, HV Richardson, IG vonRosenvinge, TT AF Cane, HV Richardson, IG vonRosenvinge, TT GP INT UNION PURE & APPL PHYS TI Short-term cosmic ray decreases: 1964-1994 SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB We have made a study of >3% short-term (<20 day) cosmic ray decreases observed by mid-latitude neutron monitors during the years 1964-1994. Following our previous work we have used the associated low energy (<100 MeV) particles to determine the relative roles of shocks, ejecta and corotating high speed streams in causing the decreases. We illustrate that very energetic shocks can influence the cosmic ray intensity at remote locations. RP Cane, HV (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 872 EP 875 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00236 ER PT J AU Richardson, IG Cane, HV AF Richardson, IG Cane, HV GP INT UNION PURE & APPL PHYS TI Corotating >60 MeV/amu cosmic ray depressions observed by spacecraft anti-coincidence guards SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB Using counting rates of > 60 MeV/amu ions from spacecraft anti-coincidence guards, we examine the detailed relationship between corotating high-speed stream structure and cosmic ray depressions. RP Richardson, IG (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 960 EP 963 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00258 ER PT J AU Badhwar, GD ONeill, PM Cucinotta, FA Weyland, M AF Badhwar, GD ONeill, PM Cucinotta, FA Weyland, M GP INT UNION PURE & APPL PHYS TI Space shuttle measurements of the galactic cosmic radiation linear energy transfer spectra over a solar cycle and their comparison with radiation transport model SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB A problem of considerable interest for radiation risk estimation of crew members on exploratory class missions is the accuracy of current models of the galactic cosmic radiation (GCR) environment and transport models. A systematic experimental evaluation of these models using data obtained from a tissue equivalent proportional counter (TEPC) flown on 15 Space Shuttle nights from April 1990 to February 1994, showed that the models predict, on average, absorbed dose and dose equivalent to +/- 10% of the observed values. There is, however, systematic underestimation of calculated dose as the level of solar modulation approaches the solar minimum. The observed fluxes are higher than the calculated fluxes by factors of 1.5-2.7, and suggest the need to improve the geomagnetic transmission functions. RP Badhwar, GD (reprint author), NASA,LYNDON B JOHNSON SPACE CTR,HOUSTON,TX 77058, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 1118 EP 1121 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00299 ER PT B AU Cooper, JF Guzik, TG Wefel, JP Pyle, KR Richardson, IG AF Cooper, JF Guzik, TG Wefel, JP Pyle, KR Richardson, IG GP INT UNION PURE & APPL PHYS TI Polar cap intensity structures during the 22 July 1982 flare: Correlation to interplanetary fluxes and anisotropies SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB Simultaneous measurements of solar energetic proton and helium nuclei were made during the 22 July 1982 solar energetic particle event from low earth orbit across the poles by the S81-1 satellite and in the upstream solar wind by the IMP-8 and ISEE-3 satellites. The extremely high anisotropies of the interplanetary ions were correlated in time to sharply variable intensity structures of ions penetrating magnetosphere to the low altitude polar cap. Apparently, many of the ions had direct and immediate access to the polar caps via IMF-geomagnetic held line connection near Earth for a northward IMF configuration. RP Cooper, JF (reprint author), NASA,GODDARD SPACE FLIGHT CTR,SPACE PHYS DATA FACIL,HUGHES STX CORP,GREENBELT,MD 20771, USA. RI Cooper, John/D-4709-2012 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 1133 EP 1136 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00303 ER PT J AU Milliken, B Leske, RA Wiedenbeck, ME AF Milliken, B Leske, RA Wiedenbeck, ME GP INT UNION PURE & APPL PHYS TI Silicon detector studies with an interferometric thickness mapper SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB A laser-interferometer system has been developed to precisely map the thickness variations of large-area silicon detectors. We describe the design and operation of the apparatus and the data processing carried out to derive thickness maps. We compare the results with a map made using accelerator beams of energetic heavy ions. RP Milliken, B (reprint author), JET PROPULS LAB,PASADENA,CA 91125, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 1283 EP 1286 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00343 ER PT B AU Cooper, JF King, JH Mathews, GJ McGuire, RE Papitashvili, NE Parthasarathy, R Towheed, SS AF Cooper, JF King, JH Mathews, GJ McGuire, RE Papitashvili, NE Parthasarathy, R Towheed, SS GP INT UNION PURE & APPL PHYS TI Internet access to NASA's OMNI and COHO data bases for interplanetary missions SO 24TH INTERNATIONAL COSMIC RAY CONFERENCE, VOL 4: SH SESSIONS - CONTRIBUTED PAPERS LA English DT Proceedings Paper CT 24th International Cosmic Ray Conference (XXIV ICRC) CY AUG 28-SEP 08, 1995 CL ROME, ITALY SP Minist Univ Ric Sci, Ist Nazl Fis Nucl, Consiglio Nazl Ric, Univ Sapienza, Roma, Univ Roma 3, Accad Nazl Lincei, Int Union Pure & Appl Phys, Int Ctr Theoret Phys, Commiss European Communities, DG XII, ICSC, World Lab, Comune Roma, Prov Roma, Banca Roma, PolHiTech, CAEN AB Internet access to interplanetary spacecraft measurements of magnetic fields, solar wind plasma, and energetic particles has long been supported by the OMNI data base at NSSDC. In 1991 the COHO data base brought anonymous FTP access to NSSDC's deep space heliospheric data sets. New OMNIWeb, COHOWeb, and other WWW services are discussed. RP Cooper, JF (reprint author), NASA,GODDARD SPACE FLIGHT CTR,NATL SPACE SCI DATA CTR,GREENBELT,MD 20771, USA. RI Cooper, John/D-4709-2012 NR 0 TC 0 Z9 0 U1 0 U2 2 PU ARGALIA EDITORE DELLE ARTI GRAFICHE EDITORIALI SRL PI URBINO PA 61029 URBINO, ITALY PY 1995 BP 1295 EP 1298 PG 4 WC Astronomy & Astrophysics; Physics, Nuclear SC Astronomy & Astrophysics; Physics GA BG94E UT WOS:A1995BG94E00346 ER PT B AU Curreri, PA Kaukler, WF AF Curreri, PA Kaukler, WF BE Schiffman, RA TI Real-time x-ray transmission microscopy of solidifying Al-In alloys SO 7TH INTERNATIONAL SYMPOSIUM ON EXPERIMENTAL METHODS FOR MICROGRAVITY MATERIALS SCIENCE LA English DT Proceedings Paper CT 7th International Symposium on Experimental Methods for Microgravity Materials Science, at the 124th TMS Annual Meeting CY FEB 12-16, 1995 CL LAS VEGAS, NV SP Minerals Met & Mat Soc, NASA Micrograv Sci, Code UG, ASM MSD Thermodyn & Phase Equilibria Comm C1 NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,HUNTSVILLE,AL 35812. OI Kaukler, William/0000-0002-7758-269X NR 0 TC 1 Z9 1 U1 0 U2 1 PU MINERALS, METALS & MATERIALS SOC PI WARRENDALE PA 420 COMMONWEALTH DR, WARRENDALE, PA 15086 BN 0-87339-311-2 PY 1995 BP 93 EP 101 PG 9 WC Materials Science, Multidisciplinary SC Materials Science GA BG04S UT WOS:A1995BG04S00015 ER PT J AU CHATTERJEE, S GILBERT Jr SCHREIBER, R TENG, SH AF CHATTERJEE, S GILBERT, JR SCHREIBER, R TENG, SH TI OPTIMAL EVALUATION OF ARRAY EXPRESSIONS ON MASSIVELY-PARALLEL MACHINES SO ACM TRANSACTIONS ON PROGRAMMING LANGUAGES AND SYSTEMS LA English DT Article DE ALGORITHMS; LANGUAGES; THEORY; ARRAY ALIGNMENT; COMPACT DYNAMIC PROGRAMMING; DATA PARALLEL PROGRAMMING; DISTRIBUTED MEMORY PARALLEL PROCESSORS; FIXED TOPOLOGY STEINER TREE; FORTRAN 90 ID TREES; PROGRAMS; NETWORKS AB We investigate the problem of evaluating Fortran 90-style array expressions on massively parallel distributed-memory machines. On such a machine, an elementwise operation can be performed in constant time for arrays whose corresponding elements are in the same processor. If the arrays are not aligned in this manner, the cost:of aligning them is part of the cost of evaluating the expression tree. The choice of where to perform the operation then affects this cost. We describe the communication cost of the parallel machine theoretically as a metric space; we model the alignment problem as that of finding a minimum-cost embedding of the expression tree into this space. We present algorithms based on dynamic programming that solve the embedding problem optimally for several communication cost metrics: multidimensional grids and rings, hypercubes, fat-trees, and the discrete metric. We also extend out approach to handle operations that change the shape of the arrays. C1 XEROX CORP, PALO ALTO RES CTR, PALO ALTO, CA 94304 USA. NASA, AMES RES CTR, RIACS, MOFFETT FIELD, CA 94035 USA. UNIV MINNESOTA, DEPT COMP SCI, MINNEAPOLIS, MN 55455 USA. RP CHATTERJEE, S (reprint author), UNIV N CAROLINA, DEPT COMP SCI, CAMPUS BOX 3175, SITTERSON HALL, CHAPEL HILL, NC 27599 USA. NR 40 TC 10 Z9 10 U1 0 U2 0 PU ASSOC COMPUTING MACHINERY PI NEW YORK PA 2 PENN PLAZA, STE 701, NEW YORK, NY 10121-0701 USA SN 0164-0925 J9 ACM T PROGR LANG SYS JI ACM Trans. Program. Lang. Syst. PD JAN PY 1995 VL 17 IS 1 BP 123 EP 156 DI 10.1145/200994.201004 PG 34 WC Computer Science, Software Engineering SC Computer Science GA QY685 UT WOS:A1995QY68500008 ER PT J AU CZERNY, B LOSKA, Z SZCZERBA, R CUKIERSKA, J MADEJSKI, G AF CZERNY, B LOSKA, Z SZCZERBA, R CUKIERSKA, J MADEJSKI, G TI NONSTANDARD EXTINCTION BY CIRCUMNUCLEAR DUST IN ACTIVE GALACTIC NUCLEI SO ACTA ASTRONOMICA LA English DT Article DE GALAXIES, INDIVIDUAL, NGC 6814; GALAXIES, ACTIVE; GALAXIES, SEYFERT; ACCRETION, ACCRETION DISKS; DUST, EXTINCTION ID X-RAY SPECTRA; SEYFERT-GALAXIES; ENERGY-DISTRIBUTIONS; INFRARED-SPECTRA; LINE REGION; QUASARS; ULTRAVIOLET; STELLAR; SPECTROPHOTOMETRY; VARIABILITY AB Observational data imply that Active Galactic Nuclei are likely to have a substantial amount of dust within some 0.1-100 pc. This dust modifies the observed spectrum of the nucleus by reprocessing a significant fraction of its intrinsic bolometric luminosity. The details of the emerging spectrum in the infrared and in the ultraviolet are dependent on the composition of such dust. It has been argued that the comparison of such models with the IR data indicates strong depletion of silicates (Czerny, Loska and Szczerba 1991, Laor and Draine 1993). In this paper we discuss several theoretical extinction curves. We show that the empirical extinction curve for the Small Magellanic Cloud corresponds well to extinction by dust dominated by amorphous carbon grains. We study the extinction by dust in X-ray band and suggest that in some sources this extinction can be mistaken for an absorption by neutral gas with cosmic abundances and an accompanying soft X-ray excess below 0.4 keV. Finally, we show that an application of a pure carbon dust model to the well-studied Seyfert galaxy NGC 6814 reveals a particularly simple form of the underlying starlight-subtracted continuum, where the spectrum (in F-v) is slightly rising with frequency. Although our determination of the intrinsic spectrum is not necessarily unique, it clearly shows the importance of further studies of the circumnuclear dust. C1 UNIV CALGARY,DEPT PHYS & ASTRON,CALGARY,AB T2N 1N4,CANADA. NICHOLAS COPERNICUS ASTRON CTR,PL-87100 TORUN,POLAND. NASA,GODDARD & UNIV SPACE RES ASSOC,LHEA,GREENBELT,MD 20771. RP CZERNY, B (reprint author), NICHOLAS COPERNICUS ASTRON CTR,BARTYCKA 18,PL-00716 WARSAW,POLAND. RI Czerny, Bozena/A-2363-2015 OI Czerny, Bozena/0000-0001-5848-4333 NR 65 TC 13 Z9 13 U1 0 U2 0 PU COPERNICUS FOUNDATION POLISH ASTRONOMY PI WARSAW PA AL UJAZDOWSKIE 4, 00-478 WARSAW, POLAND SN 0001-5237 J9 ACTA ASTRONOM JI Acta Astron. PY 1995 VL 45 IS 3 BP 623 EP 640 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA TA568 UT WOS:A1995TA56800002 ER PT J AU BLACK, FO PALOSKI, WH DOXEYGASWAY, DD RESCHKE, MF AF BLACK, FO PALOSKI, WH DOXEYGASWAY, DD RESCHKE, MF TI VESTIBULAR PLASTICITY FOLLOWING ORBITAL SPACEFLIGHT - RECOVERY FROM POSTFLIGHT POSTURAL INSTABILITY SO ACTA OTO-LARYNGOLOGICA LA English DT Article; Proceedings Paper CT 18th Barany-Society Meeting on Vestibular and Equilibrium Research - Basic and Clinical Implications CY JUN 06-08, 1994 CL UPPSALA, SWEDEN SP Barany Soc DE OTOLITH CONTROL OF POSTURE; VESTIBULAR COMPENSATION; SENSORY INTERACTION AND POSTURE CONTROL; COMPUTERIZED DYNAMIC POSTUROGRAPHY; MICROGRAVITY INDUCED MAL DE DEBARQUEMENT; SPACE ADAPTATION SYNDROME; SPACE MOTION SICKNESS ID HUMAN INNER-EAR; SPACELAB-1 MISSION; OCULAR REFLEX; WEIGHTLESSNESS; MICROGRAVITY AB Results of previous studies suggested that the vestibular mediated postural instability observed in astronauts upon return to earth from orbital spaceflight may be exacerbated by an increased weighting of visual inputs for spatial orientation and control of movement. This study was performed to better understand the roles of visual and somatosensory contributions to recovery of normal sensori-motor postural control in returning astronauts. Preflight and postnight, 23 astronaut volunteers were presented randomly with three trials of six sensory organization test (SOT) conditions in the EquiTest system test battery. Sagittal plane center-of-gravity (COG) excursions computed from ground reaction forces were significantly higher on landing day than preflight for those test conditions presenting sway-referenced visual and/or somatosensory orientation cues. The ratio of summed peak-to-peak COG sway amplitudes on the two sway-referenced vision tests (SOTs 3 + 6) compared to the two eyes closed tests (SOTs 2 + 5) was increased on landing day, indicating an increased reliance on visual orientation cues for postural control. The ratio of peak-to-peak COG excursions on sway-referenced surfaces (SOTs 4, 5 & 6) to an earth fixed support surfaces (SOTs 1, 2 & 3) increased even more after landing suggesting primary reliance on somatosensory orientation cues for recovery of postflight postural stability. Readaptation to sway-referenced support surfaces took longer than readaptation to sway-referenced vision. The increased reliance on visual and somatosensory inputs disappeared in all astronauts 4-8 days following return to earth. C1 LEGACY PORTLAND HOSP,RS DOW NEUROL SCI INST,PORTLAND,OR 97210. NASA,LYNDON B JOHNSON SPACE CTR,SPACE BIOMED RES INST,HOUSTON,TX 77058. KRUG LIFE SCI,HOUSTON,TX 77058. NR 16 TC 22 Z9 22 U1 0 U2 1 PU SCANDINAVIAN UNIVERSITY PRESS PI OSLO PA PO BOX 2959 TOYEN, JOURNAL DIVISION CUSTOMER SERVICE, N-0608 OSLO, NORWAY SN 0001-6489 J9 ACTA OTO-LARYNGOL JI Acta Oto-Laryngol. PY 1995 SU 520 BP 450 EP 454 PN 2 PG 5 WC Otorhinolaryngology SC Otorhinolaryngology GA TK017 UT WOS:A1995TK01700060 ER PT B AU Neeck, SP Scolese, CJ Bordi, F AF Neeck, SP Scolese, CJ Bordi, F BE Fujisada, H Sweeting, MN TI EOS-AM1: Project update SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 2 EP 15 DI 10.1117/12.228555 PG 14 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00001 ER PT B AU Nichols, DA Schwaller, M Pniel, M Geller, G AF Nichols, DA Schwaller, M Pniel, M Geller, G BE Fujisada, H Sweeting, MN TI EOSDIS support for the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. OI Geller, Gary/0000-0002-4490-6002 NR 0 TC 1 Z9 1 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 51 EP 61 DI 10.1117/12.228592 PG 11 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00005 ER PT B AU Smith, GL Lee, RB Barkstrom, BR Cooper, JE Kopia, LP Lawrence, RW AF Smith, GL Lee, RB Barkstrom, BR Cooper, JE Kopia, LP Lawrence, RW BE Fujisada, H Sweeting, MN TI Design and calibration features of the Clouds and the Earth's Radiant Energy System (CERES) instrument SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23681. NR 0 TC 0 Z9 0 U1 0 U2 2 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 62 EP 71 DI 10.1117/12.228599 PG 10 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00006 ER PT B AU Bruegge, C Duval, V Chrien, N Korechoff, R AF Bruegge, C Duval, V Chrien, N Korechoff, R BE Fujisada, H Sweeting, MN TI MISR instrument development and test status SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 1 Z9 1 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 92 EP 103 DI 10.1117/12.228610 PG 12 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00009 ER PT B AU Korechoff, RP Diner, DJ Preston, DJ Bruegge, CJ AF Korechoff, RP Diner, DJ Preston, DJ Bruegge, CJ BE Fujisada, H Sweeting, MN TI Spectroradiometer focal plane design considerations: Lessons learned from MISR camera SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 2 Z9 2 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 104 EP 116 DI 10.1117/12.228556 PG 13 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00010 ER PT B AU Liu, WT AF Liu, WT BE Fujisada, H Sweeting, MN TI Application of spaceborne scatterometer to study typhoon, tropical hydrologic balance, and El Nino SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 1 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 228 EP 234 DI 10.1117/12.228568 PG 7 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00021 ER PT B AU Krueger, AJ Jaross, G Hartmann, U AF Krueger, AJ Jaross, G Hartmann, U BE Fujisada, H Sweeting, MN TI Design of the ADEOS/TOMS instrument for ozone trend assessment SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NR 0 TC 2 Z9 2 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 235 EP 244 DI 10.1117/12.228569 PG 10 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00022 ER PT B AU Johnson, WTK Im, E Borgarelli, L Faustini, EZ AF Johnson, WTK Im, E Borgarelli, L Faustini, EZ BE Fujisada, H Sweeting, MN TI Cassini radar: Instrument description and performance status SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 CALTECH,JET PROP LAB,RADAR SCI & ENGN SECT,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 312 EP 322 DI 10.1117/12.228577 PG 11 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00030 ER PT B AU Aumann, HH Miller, C AF Aumann, HH Miller, C BE Fujisada, H Sweeting, MN TI Atmospheric Infrared Sounder (AIRS) on the earth observing system SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev DE EOS; AIRS; infrared; sounder; multi-aperture spectrometer; echelle grating; HgCdTe detector; Stirling cycle cryocooler C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 16 Z9 16 U1 2 U2 2 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 332 EP 343 DI 10.1117/12.228579 PG 12 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00032 ER PT B AU Flower, DA Waters, JW Froidevaux, L Jarnot, RF Lau, GK Pickett, HM Read, WG Siegel, PH AF Flower, DA Waters, JW Froidevaux, L Jarnot, RF Lau, GK Pickett, HM Read, WG Siegel, PH BE Fujisada, H Sweeting, MN TI The Microwave Limb Sounder on EOS-CHEM for atmospheric chemistry and global change investigations SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 344 EP 346 DI 10.1117/12.228580 PG 3 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00033 ER PT B AU Short, N Coronado, PL Stetina, F Mahoney, RL Shaffer, EH Wichmann, K AF Short, N Coronado, PL Stetina, F Mahoney, RL Shaffer, EH Wichmann, K BE Fujisada, H Sweeting, MN TI The development of a regional environmental system for the support of mission to planet earth SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 NASA,GODDARD SPACE FLIGHT CTR,INFORMAT SCI & TECHNOL BRANCH,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 356 EP 367 PG 12 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00035 ER PT B AU Samadi, S Masuoka, EJ AF Samadi, S Masuoka, EJ BE Fujisada, H Sweeting, MN TI A computing system to support software development, testing and product quality assurance for an Earth Observing System instrument - A case study SO ADVANCED AND NEXT-GENERATION SATELLITES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced and Next-Generation Satellites CY SEP 25-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrument Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 NASA,GODDARD SPACE FLIGHT CTR,TERR PHYS LAB,COMP SYST OFF,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1947-8 J9 P SOC PHOTO-OPT INS PY 1995 VL 2583 BP 380 EP 389 DI 10.1117/12.228584 PG 10 WC Engineering, Aerospace; Remote Sensing; Optics SC Engineering; Remote Sensing; Optics GA BE78U UT WOS:A1995BE78U00037 ER PT B AU LE, DK AF LE, DK BE Luk, FT TI Multiscale system identification and estimation SO ADVANCED SIGNAL PROCESSING ALGORITHMS SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Advanced Signal Processing Algorithms CY JUL 10-12, 1995 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE WAVELETS; MULTISCALE FORMULATION OF LINEAR DYNAMICS; STOCHASTIC PROCESSES; SYSTEM IDENTIFICATION; FILTERING; CONTROL DESIGN C1 NASA,LEWIS RES CTR,CONTROL SYST BRANCH,CLEVELAND,OH 44135. NR 0 TC 2 Z9 2 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1922-2 J9 P SOC PHOTO-OPT INS PY 1995 VL 2563 BP 470 EP 481 DI 10.1117/12.211423 PG 12 WC Computer Science, Software Engineering; Engineering, Electrical & Electronic; Remote Sensing; Physics, Applied SC Computer Science; Engineering; Remote Sensing; Physics GA BD49N UT WOS:A1995BD49N00040 ER PT J AU DesMarais, DJ AF DesMarais, DJ TI The biogeochemistry of hypersaline microbial mats SO ADVANCES IN MICROBIAL ECOLOGY, VOL 14 SE ADVANCES IN MICROBIAL ECOLOGY LA English DT Review ID CYANOBACTERIAL MATS; CARBON; SULFUR; COMMUNITIES; OXYGEN RP DesMarais, DJ (reprint author), NASA,AMES RES CTR,MOFFETT FIELD,CA 94035, USA. NR 39 TC 84 Z9 86 U1 2 U2 13 PU PLENUM PRESS DIV PLENUM PUBLISHING CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 SN 0147-4863 J9 ADV MICROB ECOL PY 1995 VL 14 BP 251 EP 274 PG 24 WC Agronomy; Ecology; Marine & Freshwater Biology; Microbiology SC Agriculture; Environmental Sciences & Ecology; Marine & Freshwater Biology; Microbiology GA BE58J UT WOS:A1995BE58J00006 PM 11539110 ER PT B AU Goedjen, JG Brindley, WJ Miller, RA AF Goedjen, JG Brindley, WJ Miller, RA BE Berndt, CC Sampath, S TI Sintering of plasma-sprayed sol gel zirconia-yttria as a function of silica content SO ADVANCES IN THERMAL SPRAY SCIENCE AND TECHNOLOGY LA English DT Proceedings Paper CT 8th National Thermal Spray Conference on Advances in Thermal Spray Science and Technology CY SEP 11-15, 1995 CL HOUSTON, TX SP ASM Int, Thermal Spray Soc, Amer Welding Soc, Deut Verband Schweisstech e V, High Temperature Soc Japan, Int Thermal Spray Assoc, Japanese Thermal Spraying Soc C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. NR 0 TC 7 Z9 7 U1 0 U2 1 PU ASM INTERNATIONAL PI MATERIALS PARK PA 9503 KINSMAN RD, MATERIALS PARK, OH 44073 BN 0-87170-541-9 PY 1995 BP 73 EP 77 PG 5 WC Materials Science, Coatings & Films SC Materials Science GA BF78B UT WOS:A1995BF78B00013 ER PT B AU Lacis, AA Mishchenko, MI AF Lacis, AA Mishchenko, MI BE Charlson, RJ Heintzenberg, J TI Climate forcing, climate sensitivity, and climate response: A radiative modeling perspective on atmospheric aerosols SO AEROSOL FORCING OF CLIMATE SE DAHLEM WORKSHOP REPORTS : ENVIRONMENTAL SCIENCES RESEARCH REPORT LA English DT Proceedings Paper CT Dahlem Workshop on Aerosol Forcing of Climate CY APR 24-29, 1994 CL BERLIN, GERMANY SP Senat Stadt Berlin, Freie Univ Berlin C1 NASA,GODDARD INST SPACE STUDIES,NEW YORK,NY 10025. RI Mishchenko, Michael/D-4426-2012 NR 0 TC 105 Z9 106 U1 0 U2 8 PU JOHN WILEY & SONS LTD PI CHICHESTER PA BAFFINS LANE, CHICHESTER, WEST SUSSEX, ENGLAND PO19 1UD BN 0-471-95693-7 J9 DAHL WS ENV PY 1995 VL 17 BP 11 EP 42 PG 32 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA BG41E UT WOS:A1995BG41E00002 ER PT B AU Toon, OB AF Toon, OB BE Charlson, RJ Heintzenberg, J TI Modeling the relationships between aerosol properties and the direct and indirect effects of aerosols on climate SO AEROSOL FORCING OF CLIMATE SE DAHLEM WORKSHOP REPORTS : ENVIRONMENTAL SCIENCES RESEARCH REPORT LA English DT Proceedings Paper CT Dahlem Workshop on Aerosol Forcing of Climate CY APR 24-29, 1994 CL BERLIN, GERMANY SP Senat Stadt Berlin, Freie Univ Berlin C1 NASA,AMES RES CTR,EARTH SYST SCI DIV,MOFFETT FIELD,CA 94035. NR 0 TC 7 Z9 7 U1 0 U2 0 PU JOHN WILEY & SONS LTD PI CHICHESTER PA BAFFINS LANE, CHICHESTER, WEST SUSSEX, ENGLAND PO19 1UD BN 0-471-95693-7 J9 DAHL WS ENV PY 1995 VL 17 BP 197 EP 213 PG 17 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA BG41E UT WOS:A1995BG41E00011 ER PT B AU King, MD Tsay, SC Platnick, S AF King, MD Tsay, SC Platnick, S BE Charlson, RJ Heintzenberg, J TI In situ observations of the indirect effects of aerosols on clouds SO AEROSOL FORCING OF CLIMATE SE DAHLEM WORKSHOP REPORTS : ENVIRONMENTAL SCIENCES RESEARCH REPORT LA English DT Proceedings Paper CT Dahlem Workshop on Aerosol Forcing of Climate CY APR 24-29, 1994 CL BERLIN, GERMANY SP Senat Stadt Berlin, Freie Univ Berlin C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RI Tsay, Si-Chee/J-1147-2014; Platnick, Steven/J-9982-2014; King, Michael/C-7153-2011 OI Platnick, Steven/0000-0003-3964-3567; King, Michael/0000-0003-2645-7298 NR 0 TC 4 Z9 5 U1 0 U2 0 PU JOHN WILEY & SONS LTD PI CHICHESTER PA BAFFINS LANE, CHICHESTER, WEST SUSSEX, ENGLAND PO19 1UD BN 0-471-95693-7 J9 DAHL WS ENV PY 1995 VL 17 BP 227 EP 248 PG 22 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA BG41E UT WOS:A1995BG41E00013 ER PT B AU Kaufman, YJ AF Kaufman, YJ BE Charlson, RJ Heintzenberg, J TI Remote sensing of direct and indirect aerosol forcing SO AEROSOL FORCING OF CLIMATE SE DAHLEM WORKSHOP REPORTS : ENVIRONMENTAL SCIENCES RESEARCH REPORT LA English DT Proceedings Paper CT Dahlem Workshop on Aerosol Forcing of Climate CY APR 24-29, 1994 CL BERLIN, GERMANY SP Senat Stadt Berlin, Freie Univ Berlin C1 NASA,GODDARD SPACE FLIGHT CTR,LAB ATMOSPHERES 913,GREENBELT,MD 20771. NR 0 TC 22 Z9 22 U1 0 U2 1 PU JOHN WILEY & SONS LTD PI CHICHESTER PA BAFFINS LANE, CHICHESTER, WEST SUSSEX, ENGLAND PO19 1UD BN 0-471-95693-7 J9 DAHL WS ENV PY 1995 VL 17 BP 297 EP 332 PG 36 WC Environmental Sciences; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Geology; Meteorology & Atmospheric Sciences GA BG41E UT WOS:A1995BG41E00016 ER PT J AU TUBIELLO, FN ROSENZWEIG, C VOLK, T AF TUBIELLO, FN ROSENZWEIG, C VOLK, T TI INTERACTIONS OF CO2, TEMPERATURE AND MANAGEMENT-PRACTICES - SIMULATIONS WITH A MODIFIED VERSION OF CERES-WHEAT SO AGRICULTURAL SYSTEMS LA English DT Article ID CARBON-DIOXIDE; PLANT-GROWTH; LEAF-AREA; YIELD; CROP; PHOTOSYNTHESIS; PRODUCTIVITY; ENRICHMENT; CLIMATE AB A new growth subroutine was developed for CERES-Wheat, a computer model of wheat (Triticum aestivum) growth and development. The new subroutine simulates canopy photosynthetic response to CO2 concentrations and light levels, and includes the effects of temperature on canopy light-use effciency. Its performance was compared to the original CERES-Wheat V-2.10 in 30 different cases. Biomass and yield predictions of the two models were well correlated (correlation coefficient r > 0.95). As an application, summer growth of spring wheat was simulated at one site. Modeled crop responses to higher mean temperatures, different amounts of minimum and maximum warming, and doubled CO2 concentrations were compared to observations. The importance of irrigation and nitrogen fertilization in modulating the wheat crop climatic responses were also analyzed. Specifically, in agreement with observations, rainfed crops were found to be more sensitive to CO2 increases than irrigated ones. On the other hand, low nitrogen applications depressed the ability of the wheat crop to respond positively to CO2 increases. In general, the positive effects of high CO2 grain yield were found to be almost completely counterbalanced by the negative effects of high temperatures. Depending on how temperature minima and maxima were increased, yield changes averaged across management practices ranged from -4% to 8%. C1 NYU,DEPT EARTH SYST SCI,NEW YORK,NY 10003. RP TUBIELLO, FN (reprint author), COLUMBIA UNIV,GODDARD INST SPACE STUDIES,2880 BROADWAY,NEW YORK,NY 10025, USA. NR 36 TC 23 Z9 23 U1 2 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, OXON, ENGLAND OX5 1GB SN 0308-521X J9 AGR SYST JI Agric. Syst. PY 1995 VL 49 IS 2 BP 135 EP 152 DI 10.1016/0308-521X(94)00044-R PG 18 WC Agriculture, Multidisciplinary SC Agriculture GA RJ118 UT WOS:A1995RJ11800003 PM 11540251 ER PT J AU WU, SF MAESTRELLO, L AF WU, SF MAESTRELLO, L TI RESPONSES OF FINITE BAFFLED PLATE TO TURBULENT-FLOW EXCITATIONS SO AIAA JOURNAL LA English DT Article ID BOUNDARY-LAYER; SURFACE AB Formulations for estimating dynamic and acoustic responses of a finite baffled plate subject to turbulent boundary-layer excitations are presented. In deriving the formulations, the effects of structural nonlinearities induced by in-plane forces and shearing forces due to stretching of plate bending motion are considered. The excitation force due to turbulent flow is expressed in terms of a sum of two components. One component corresponds to a fluctuating pressure field due to acoustic radiation, which is determined analytically for both supersonic and subsonic flows. The other component corresponds to a fluctuating pressure field due to a turbulent boundary layer, which is determined experimentally. The cross-power spectra of the plate flexural displacement and the radiated acoustic pressure are shown to be directly related to that of the turbulent boundary layer In addition to the plate dynamic and acoustic responses, a stability analysis is given using the basic existence-uniqueness theorem. In particular, stable conditions for a linearized system are obtained via the Routh algorithm. It is shown that temporal instability can be induced by the added stiffness due to acoustic radiation in the presence of mean flow. The effect of the added stiffness increases quadratically with the mean now speed. C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23681. RP WU, SF (reprint author), WAYNE STATE UNIV,DEPT MECH ENGN,DETROIT,MI 48202, USA. NR 32 TC 33 Z9 33 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0001-1452 J9 AIAA J JI AIAA J. PD JAN PY 1995 VL 33 IS 1 BP 13 EP 19 DI 10.2514/3.12326 PG 7 WC Engineering, Aerospace SC Engineering GA QE786 UT WOS:A1995QE78600002 ER PT J AU DAVIS, SS AF DAVIS, SS TI AEROACOUSTIC MODEL FOR WEAK SHOCK-WAVES BASED ON BURGERS-EQUATION SO AIAA JOURNAL LA English DT Article AB The adiabatic form of the Euler equations are cast in a form emphasizing its signal propagation properties and solved using an approximate eigen-function analysis. Second-order rarefaction waves appear as direct eigenfunction solutions. The underlying scalar equation describing nonlinear shock wave evolution is rederived as a first-order Burgers equation. The characteristic sonic boom N waves are predicted using an implicit aeroacoustic-based finite-difference algorithm with numerical damping designed to suppress spurious oscillations at shock-wave discontinuities. The evolution of these sonic-boom-type signals to the mid- and far field are computed directly with the numerical method. RP DAVIS, SS (reprint author), NASA,AMES RES CTR,FLUID MECH LAB BRANCH,MOFFETT FIELD,CA 94035, USA. NR 15 TC 1 Z9 1 U1 1 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0001-1452 J9 AIAA J JI AIAA J. PD JAN PY 1995 VL 33 IS 1 BP 27 EP 32 DI 10.2514/3.12328 PG 6 WC Engineering, Aerospace SC Engineering GA QE786 UT WOS:A1995QE78600004 ER PT J AU SONDAK, DL PLETCHER, RH AF SONDAK, DL PLETCHER, RH TI APPLICATION OF WALL FUNCTIONS TO GENERALIZED NONORTHOGONAL CURVILINEAR COORDINATE SYSTEMS SO AIAA JOURNAL LA English DT Article ID TURBULENCE MODELS; BOUNDARY-LAYER; SHEAR LAYERS; NEAR-WALL; FLOWS; PREDICTION; CHANNEL AB A method has been developed for the application of wall functions to generalized curvilinear coordinate systems with nonorthogonal grids. Two test cases have been computed using this method with the k-epsilon turbulence model: now over a flat plate at 0-deg angle of attack using a nonorthogonal grid at the wall and now over a prolate hemispheroid with a hemispherical nose cap at 0-deg angle of attack. All results are compared with experimental data. In addition, the hemispheroid results are compared with computations using the Baldwin-Lomax algebraic turbulence model and the Chien low-Reynolds-number k-epsilon turbulence model. C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. IOWA STATE UNIV SCI & TECHNOL,DEPT MECH ENGN,AMES,IA 50011. NR 36 TC 12 Z9 15 U1 0 U2 1 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0001-1452 J9 AIAA J JI AIAA J. PD JAN PY 1995 VL 33 IS 1 BP 33 EP 41 DI 10.2514/3.12329 PG 9 WC Engineering, Aerospace SC Engineering GA QE786 UT WOS:A1995QE78600005 ER PT J AU SLATER, JW LIOU, MS HINDMAN, RG AF SLATER, JW LIOU, MS HINDMAN, RG TI APPROACH FOR DYNAMIC GRIDS SO AIAA JOURNAL LA English DT Article ID FLOW AB An approach is presented for the generation of two-dimensional, structured, dynamic grids utilizing grid speeds computed from the time differentiation of a set of grid equations. In application for the computation of unsteady, inviscid hows, it is shown that the approach is more efficient and accurate than an approach in which the grid speeds are computed using a finite difference of the grid with respect to time. C1 IOWA STATE UNIV SCI & TECHNOL,DEPT AEROSP ENGN & ENGN MECH,AMES,IA 50011. RP SLATER, JW (reprint author), NASA,LEWIS RES CTR,DIV INTERNAL FLUID MECH,COMPUTAT FLUID DYNAM BRANCH,MS 5-1,2100 BROOKPK RD,CLEVELAND,OH 44135, USA. NR 8 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 0001-1452 J9 AIAA J JI AIAA J. PD JAN PY 1995 VL 33 IS 1 BP 63 EP 68 DI 10.2514/3.12333 PG 6 WC Engineering, Aerospace SC Engineering GA QE786 UT WOS:A1995QE78600009 ER PT J AU WEYGANDT, JH MEHTA, RD AF WEYGANDT, JH MEHTA, RD TI EFFECTS OF STREAMWISE VORTICITY INJECTION ON A PLANE TURBULENT WAKE SO AIAA JOURNAL LA English DT Article ID MIXING LAYER; TRANSITION AB Past now visualization investigations of plane wakes originating from laminar initial boundary layers have shown the presence of streamwise vortical structures riding among the spanwise (von Karman) vortices. Quantitative measurements of the mean streamwise vorticity were recently obtained which shed more light on their formation and subsequent evolution. Measurements made in the same wake with both initial boundary layers turbulent, however, showed that spatially stationary streamwise structures did not exist in this case, thus resulting in a distinctly different mean three-dimensional structure and streamwise evolution. In the present study, the effects of injecting streamwise vorticity on the structure and development of a wake originating from turbulent boundary layers are investigated. A corrugated extension attached to the splitter plate trailing edge produced a relatively strong array of counter-rotating pairs of streamwise vorticity which were injected into the turbulent wake. This resulted in large spanwise variations in the wake mean properties and Reynolds stress distributions. Although the mean streamwise vorticity decreased with downstream distance, the spanwise variations were found to persist into the far-field region (X/Theta > 500) of the wake. In the near-held region (X/Theta < 500),the wake growth was increased, and the velocity defect was reduced, both because of increased entrainment due to the injected vorticity. However, in the far-field region, the forced wake growth rate and peak Reynolds stresses were reduced significantly with respect to the undisturbed wake. This result is attributed to the effect of the relatively strong streamwise vorticity in making the spanwise structures more three dimensional and, hence, less efficient at entraining surrounding fluid. C1 STANFORD UNIV,JOINT INST AERONAUT & ASTRONAUT,DEPT AERONAUT & ASTRONAUT,STANFORD,CA 94305. STANFORD UNIV,NASA,AMES RES CTR,JOINT INST AERONAUT & ACOUST,DEPT AERONAUT & ASTR,MOFFETT FIELD,CA 94035. STANFORD UNIV,NASA,AMES RES CTR,FLUID MECH LAB,MOFFETT FIELD,CA 94035. NR 20 TC 1 Z9 1 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0001-1452 J9 AIAA J JI AIAA J. PD JAN PY 1995 VL 33 IS 1 BP 86 EP 93 DI 10.2514/3.12336 PG 8 WC Engineering, Aerospace SC Engineering GA QE786 UT WOS:A1995QE78600012 ER PT J AU STAGG, AK CLINE, DD CAREY, GF SHADID, JN AF STAGG, AK CLINE, DD CAREY, GF SHADID, JN TI PARALLEL, SCALABLE PARABOLIZED NAVIER-STOKES SOLVER FOR LARGE-SCALE SIMULATIONS SO AIAA JOURNAL LA English DT Article ID EQUATIONS AB A massively parallel formulation for the solution of the parabolized Navier-Stokes equations has been developed for multiple instruction, multiple data (MIMD) computers. All functionality of the serial version of the code has been preserved in the parallel implementation, including grid generation, linear system solvers, and shock fitting. The computational domain is automatically decomposed and load balanced on individual processing elements. Performance timings are carried out for various MIMD architectures. Numerical tests indicate high parallel efficiency, with fixed solution time as the computational work is scaled with the number of processors. C1 UNIV TEXAS,HIGH PERFORMANCE COMP FACIL,AUSTIN,TX 78758. UNIV TEXAS,COLL ENGN,AUSTIN,TX 78758. SANDIA NATL LABS,TECH STAFF,ALBUQUERQUE,NM 87185. RP STAGG, AK (reprint author), CRAY RES INC,JET PROP LABS,PASADENA,CA 91109, USA. NR 13 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 0001-1452 J9 AIAA J JI AIAA J. PD JAN PY 1995 VL 33 IS 1 BP 102 EP 108 DI 10.2514/3.12338 PG 7 WC Engineering, Aerospace SC Engineering GA QE786 UT WOS:A1995QE78600014 ER PT J AU REHFIELD, LW ZISCHKA, PJ CHANG, S FENTRESS, ML AMBUR, DR AF REHFIELD, LW ZISCHKA, PJ CHANG, S FENTRESS, ML AMBUR, DR TI EXPERIMENTAL EVALUATION OF A BOX BEAM SPECIFICALLY TAILORED FOR CHORDWISE DEFORMATION SO AIAA JOURNAL LA English DT Article AB This paper describes an experimental methodology based upon the use of a flexible sling support and load application system that has been created and utilized to evaluate a box beam that incorporates an elastic tailoring technology. The design technique used here for elastically tailoring the composite box beam structure is to produce exaggerated chordwise camber deformation of substantial magnitude to be of practical use in the new composite aircraft wings. The traditional methods such as a four-point bend test to apply constant bending moment with rigid fixtures inhibit the desired chordwise deformation from occurring, hence the need for the new test method. The experimental results for global camber and spanwise bending compliances correlate well with theoretical predictions based on a beamlike model. C1 NASA,LANGLEY RES CTR,AIRCRAFT STURCT BRANCH,HAMPTON,VA 23692. RP REHFIELD, LW (reprint author), UNIV CALIF DAVIS,DEPT MECH AERONAUT & MAT ENGN,DAVIS,CA 95616, USA. NR 6 TC 0 Z9 0 U1 0 U2 0 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091 SN 0001-1452 J9 AIAA J JI AIAA J. PD JAN PY 1995 VL 33 IS 1 BP 116 EP 119 DI 10.2514/3.12340 PG 4 WC Engineering, Aerospace SC Engineering GA QE786 UT WOS:A1995QE78600016 ER PT J AU ABID, R GATSKI, TB MORRISON, JH AF ABID, R GATSKI, TB MORRISON, JH TI ASSESSMENT OF PRESSURE-STRAIN MODELS IN PREDICTING COMPRESSIBLE, TURBULENT RAMP FLOWS SO AIAA JOURNAL LA English DT Note C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23681. ANALYT SERV & MAT INC,HAMPTON,VA 23666. RP ABID, R (reprint author), HIGH TECHNOL CORP,28 RES DR,HAMPTON,VA 23666, USA. NR 14 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 0001-1452 J9 AIAA J JI AIAA J. PD JAN PY 1995 VL 33 IS 1 BP 156 EP 159 DI 10.2514/3.12347 PG 4 WC Engineering, Aerospace SC Engineering GA QE786 UT WOS:A1995QE78600023 ER PT B AU BARKER, BC AF BARKER, BC BE Otto, RG Lenz, J TI Wake vortex systems research SO AIR TRAFFIC CONTROL TECHNOLOGIES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Air Traffic Control Technologies CY APR 18-19, 1995 CL ORLANDO, FL SP Soc Photo Opt Instrumentat Engineers C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23665. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1817-X J9 P SOC PHOTO-OPT INS PY 1995 VL 2464 BP 50 EP 62 DI 10.1117/12.211477 PG 13 WC Instruments & Instrumentation; Remote Sensing; Optics SC Instruments & Instrumentation; Remote Sensing; Optics GA BD35H UT WOS:A1995BD35H00005 ER PT B AU BOGUE, R BAGLEY, H SOREIDE, D BOWDLE, D AF BOGUE, R BAGLEY, H SOREIDE, D BOWDLE, D BE Otto, RG Lenz, J TI A coherent lidar solution for the HSCT supersonic engine inlet unstart problem SO AIR TRAFFIC CONTROL TECHNOLOGIES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Air Traffic Control Technologies CY APR 18-19, 1995 CL ORLANDO, FL SP Soc Photo Opt Instrumentat Engineers DE COHERENT LIDAR; SUPERSONIC ENGINE INLET UNSTART; HIGH SPEED CIVIL TRANSPORT; ATMOSPHERIC TURBULENCE; GUST; ACLAIM; STRATOSPHERE BACKSCATTER; TROPOSPHERE BACKSCATTER; EYE-SAFE LASER; SR-71 C1 NASA,DRYDEN FLIGHT RES CTR,EDWARDS AFB,CA 93523. NR 0 TC 1 Z9 1 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1817-X J9 P SOC PHOTO-OPT INS PY 1995 VL 2464 BP 79 EP 93 DI 10.1117/12.211479 PG 15 WC Instruments & Instrumentation; Remote Sensing; Optics SC Instruments & Instrumentation; Remote Sensing; Optics GA BD35H UT WOS:A1995BD35H00007 ER PT B AU Tielens, AGGM AF Tielens, AGGM BE Haas, MR Davidson, JA Erickson, EF TI The interstellar medium SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,DIV SPACE SCI,MOFFETT FIELD,CA 94035. NR 0 TC 9 Z9 9 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 3 EP 22 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00001 ER PT B AU Allamandola, LJ Sandford, SA Hudgins, DM Witteborn, FC AF Allamandola, LJ Sandford, SA Hudgins, DM Witteborn, FC BE Haas, MR Davidson, JA Erickson, EF TI Airborne and laboratory studies of interstellar PAHs SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 15 Z9 15 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 23 EP 32 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00002 ER PT B AU Bregman, J Harker, D Rank, D Temi, P AF Bregman, J Harker, D Rank, D Temi, P BE Haas, MR Davidson, JA Erickson, EF TI Spectral imaging of the Orion Bar at 6.2 and 7.8 microns SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 63 EP 66 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00008 ER PT B AU Jenniskens, P Blake, DF AF Jenniskens, P Blake, DF BE Haas, MR Davidson, JA Erickson, EF TI Physical and chemical evolution of reduced organic matter in the ISM SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 71 EP 72 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00010 ER PT B AU Simpson, JP Bregman, JD Dinerstein, HL Lester, DF Rank, DM Witteborn, FC Wooden, DH AF Simpson, JP Bregman, JD Dinerstein, HL Lester, DF Rank, DM Witteborn, FC Wooden, DH BE Haas, MR Davidson, JA Erickson, EF TI Argon and neon in galactic nebulae SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 105 EP 110 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00018 ER PT B AU Rubin, RH Simpson, JP Erickson, EF Haas, MR Lord, SD Colgan, SWJ AF Rubin, RH Simpson, JP Erickson, EF Haas, MR Lord, SD Colgan, SWJ BE Haas, MR Davidson, JA Erickson, EF TI Density determination from far-infrared lines SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. RI Colgan, Sean/M-4742-2014 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 115 EP 118 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00020 ER PT B AU Werner, MW Eisenhardt, PRM AF Werner, MW Eisenhardt, PRM BE Haas, MR Davidson, JA Erickson, EF TI Infrared studies of galaxies from space SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 169 EP 176 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00025 ER PT B AU Tsai, JC Mathews, WG AF Tsai, JC Mathews, WG BE Haas, MR Davidson, JA Erickson, EF TI Interstellar grains in elliptical galaxies SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 177 EP 180 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00026 ER PT B AU Madden, SC Geis, N Townes, CH Genzel, R Herrmann, F Poglitsch, A Stacey, GJ AF Madden, SC Geis, N Townes, CH Genzel, R Herrmann, F Poglitsch, A Stacey, GJ BE Haas, MR Davidson, JA Erickson, EF TI Extragalactic diffuse [CII] emission SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 7 Z9 7 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 181 EP 184 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00027 ER PT B AU Davidson, JA Schleuning, D Dotson, JL Dowell, CD Hildebrand, RH AF Davidson, JA Schleuning, D Dotson, JL Dowell, CD Hildebrand, RH BE Haas, MR Davidson, JA Erickson, EF TI The magnetic field structure in high-mass star formation regions SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,SETI INST,MOFFETT FIELD,CA 94035. NR 0 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 225 EP 234 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00035 ER PT B AU Hollenbach, D Ceccarelli, C Neufeld, DA Tielens, AGGM AF Hollenbach, D Ceccarelli, C Neufeld, DA Tielens, AGGM BE Haas, MR Davidson, JA Erickson, EF TI Infrared spectra of protostellar collapse SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 243 EP 250 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00037 ER PT B AU Salama, F Allamandola, LJ Sandford, SA Bregman, JD Witteborn, FC Cruikshank, DP AF Salama, F Allamandola, LJ Sandford, SA Bregman, JD Witteborn, FC Cruikshank, DP BE Haas, MR Davidson, JA Erickson, EF TI Detection of a new strong band near 3590 cm(-1) (2.79 mu m) in the spectrum of Io SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 337 EP 340 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00050 ER PT B AU Bell, JF Bregman, JD Rank, DM Temi, P Roush, TL Hawke, BR Lucey, PG Pollack, JB AF Bell, JF Bregman, JD Rank, DM Temi, P Roush, TL Hawke, BR Lucey, PG Pollack, JB BE Haas, MR Davidson, JA Erickson, EF TI Mid-infrared (5.0-7.0 mu m) imaging spectroscopy of the moon from the KAO SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,DIV SPACE SCI,THEORET STUDIES BRANCH,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 341 EP 344 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00051 ER PT B AU Roush, T Pollack, J Witteborn, F Bregman, J Bell, J Sitton, B AF Roush, T Pollack, J Witteborn, F Bregman, J Bell, J Sitton, B BE Haas, MR Davidson, JA Erickson, EF TI Thermal infrared spectroscopic observations of Mars from the Kuiper Airborne Observatory (KAO): Constraints on past climates and weathering products SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,DIV SPACE SCI,THEORET STUDIES BRANCH,SAN FRANCISCO UNIV,DEPT GEOSCI,MOFFETT FIELD,CA 94035. NR 0 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 345 EP 348 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00052 ER PT B AU Haas, MR Glassgold, AE Tielens, AGGM AF Haas, MR Glassgold, AE Tielens, AGGM BE Haas, MR Davidson, JA Erickson, EF TI Fine structure line emission from supergiants SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 397 EP 404 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00059 ER PT B AU Wooden, DH AF Wooden, DH BE Haas, MR Davidson, JA Erickson, EF TI KAO observations of SN1987A SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 405 EP 412 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00060 ER PT B AU Goebel, JH Bregman, JD Witteborn, FC AF Goebel, JH Bregman, JD Witteborn, FC BE Haas, MR Davidson, JA Erickson, EF TI A 7 mu m dust emission feature in oxygen-rich circumstellar shells SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,DIV SPACE SCI,TECHNOL DEV BRANCH,MOFFETT FIELD,CA 94035. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 419 EP 423 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00062 ER PT B AU Sloan, GC Price, SD LittleMarenin, IR LeVan, PD AF Sloan, GC Price, SD LittleMarenin, IR LeVan, PD BE Haas, MR Davidson, JA Erickson, EF TI Silicate and related dust emission in stars on the asymptotic giant branch SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 425 EP 428 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00063 ER PT B AU Justtanont, K Tielens, AGGM Skinner, CJ Haas, MR AF Justtanont, K Tielens, AGGM Skinner, CJ Haas, MR BE Haas, MR Davidson, JA Erickson, EF TI High rotational CO lines in post-AGB stars and PNe SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 429 EP 432 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00064 ER PT B AU Erickson, EF Colgan, SWJ Simpson, JP Rubin, RH Haas, MR Morris, M Cotera, AS Allen, DA Burton, MG AF Erickson, EF Colgan, SWJ Simpson, JP Rubin, RH Haas, MR Morris, M Cotera, AS Allen, DA Burton, MG BE Haas, MR Davidson, JA Erickson, EF TI KAO and AAT observations of the galactic center filaments SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. RI Colgan, Sean/M-4742-2014 NR 0 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 489 EP 498 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00072 ER PT B AU Telesco, CM DAvidson, JA Werner, MW AF Telesco, CM DAvidson, JA Werner, MW BE Haas, MR Davidson, JA Erickson, EF TI High angular resolution 30 mu m observations of the galactic center SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Meeting Abstract CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB,ES-63,HUNTSVILLE,AL 35812. NR 0 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 503 EP 503 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00074 ER PT B AU Colgan, SWJ Erickson, EF Simpson, JP Haas, MR Morris, M AF Colgan, SWJ Erickson, EF Simpson, JP Haas, MR Morris, M BE Haas, MR Davidson, JA Erickson, EF TI Excitation of the ''arched'' filaments near the Galactic Center SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,SETI INST,MOFFETT FIELD,CA 94035. RI Colgan, Sean/M-4742-2014 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 507 EP 510 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00076 ER PT B AU Dunham, EW AF Dunham, EW BE Haas, MR Davidson, JA Erickson, EF TI Optical instrumentation for airborne astronomy SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,DIV SPACE SCI,MOFFETT FIELD,CA 94035. NR 0 TC 5 Z9 5 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 517 EP 522 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00078 ER PT B AU Erickson, EF Haas, MR Colgan, SWJ Simpson, JP Rubin, RH AF Erickson, EF Haas, MR Colgan, SWJ Simpson, JP Rubin, RH BE Haas, MR Davidson, JA Erickson, EF TI The cryogenic grating spectrometer SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. RI Colgan, Sean/M-4742-2014 NR 0 TC 9 Z9 9 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 523 EP 530 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00079 ER PT B AU Haas, MR Erickson, EF Colgan, SWJ Baltz, JA Lynch, DH AF Haas, MR Erickson, EF Colgan, SWJ Baltz, JA Lynch, DH BE Haas, MR Davidson, JA Erickson, EF TI Design considerations for a large Airborne Infrared Echelle Spectrometer (AIRES) SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. RI Colgan, Sean/M-4742-2014 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 531 EP 534 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00080 ER PT B AU Witteborn, FC Cohen, M Bregman, JD Heere, KR Greene, TP Wooden, DH AF Witteborn, FC Cohen, M Bregman, JD Heere, KR Greene, TP Wooden, DH BE Haas, MR Davidson, JA Erickson, EF TI HIFOGS: Its design, operation and calibration SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 17 Z9 17 U1 0 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 573 EP 578 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00091 ER PT B AU Baltz, JA Erickson, EF AF Baltz, JA Erickson, EF BE Haas, MR Davidson, JA Erickson, EF TI A synchronous motor chopper for laboratory testing of detector systems in infrared astronomy SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,SETI INST,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 579 EP 582 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00092 ER PT B AU Bregman, J Harker, D Rank, D Temi, P AF Bregman, J Harker, D Rank, D Temi, P BE Haas, MR Davidson, JA Erickson, EF TI Mid-infrared array camera on the KAO SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 583 EP 586 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00093 ER PT B AU Whiting, WA Mathias, EC AF Whiting, WA Mathias, EC BE Haas, MR Davidson, JA Erickson, EF TI From the KAO archives: Photographs and video from the first 20 years SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Meeting Abstract CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 609 EP 609 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00096 ER PT B AU Caroff, LJ AF Caroff, LJ BE Haas, MR Davidson, JA Erickson, EF TI Panel discussion: The future of IR astronomy SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA HEADQUARTERS,DIV ASTROPHYS,WASHINGTON,DC 20546. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 647 EP 658 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00104 ER PT B AU Roellig, TL AF Roellig, TL BE Haas, MR Davidson, JA Erickson, EF TI The Infrared Telescope in Space (IRTS) mission SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 665 EP 668 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00106 ER PT B AU Dunham, EW AF Dunham, EW BE Haas, MR Davidson, JA Erickson, EF TI KAO mission summary SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 679 EP 680 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00109 ER PT B AU Davidson, JA AF Davidson, JA BE Haas, MR Davidson, JA Erickson, EF TI COPE mission summary SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 683 EP 684 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00111 ER PT B AU Roellig, TL AF Roellig, TL BE Haas, MR Davidson, JA Erickson, EF TI IRTS mission summary SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 687 EP 688 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00113 ER PT B AU Schember, H AF Schember, H BE Haas, MR Davidson, JA Erickson, EF TI WIRE mission summary SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 695 EP 696 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00117 ER PT B AU Erickson, EF AF Erickson, EF BE Haas, MR Davidson, JA Erickson, EF TI SOFIA mission summary SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 697 EP 698 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00118 ER PT B AU Werner, MW AF Werner, MW BE Haas, MR Davidson, JA Erickson, EF TI IRIS mission summary SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 699 EP 700 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00119 ER PT B AU Werner, MW AF Werner, MW BE Haas, MR Davidson, JA Erickson, EF TI SIRTF mission summary SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 701 EP 702 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00120 ER PT B AU Erickson, EF Davidson, JA AF Erickson, EF Davidson, JA BE Haas, MR Davidson, JA Erickson, EF TI SOFIA: The future of airborne astronomy SO AIRBORNE ASTRONOMY SYMPOSIUM ON THE GALACTIC ECOSYSTEM: FROM GAS TO STARS TO DUST SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Airborne Astronomy Symposium on the Galactic Ecosystem - From Gas to Stars to Dust CY JUL 05-08, 1994 CL NASA AMES RES CTR, MOFFETT FIELD, CA SP NASA, SETI Inst, Contraves Inc, Pittsburg, E Syst, Greenville, Hughes Aircraft Co, El Segundo, Sterling Software, Palo Alto HO NASA AMES RES CTR C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 10 Z9 10 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-92-9 J9 ASTR SOC P PY 1995 VL 73 BP 707 EP 732 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33X UT WOS:A1995BE33X00123 ER PT B AU MADSEN, SN AF MADSEN, SN BE Giglio, DA TI On absolute phase determination techniques in SAR interferometry SO ALGORITHMS FOR SYNTHETIC APERTURE RADAR IMAGERY II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Algorithms for Synthetic Aperture Radar Imagery II CY APR 19-21, 1995 CL ORLANDO, FL SP Soc Photo Opt Instrumentat Engineers DE SAR INTERFEROMETRY; SYNTHETIC APERTURE RADAR (SAR); ABSOLUTE PHASE; SPLIT-SPECTRUM ALGORITHM; RESIDUAL DELAY ESTIMATION ALGORITHM C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 19 Z9 20 U1 0 U2 2 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1840-4 J9 P SOC PHOTO-OPT INS PY 1995 VL 2487 BP 393 EP 401 DI 10.1117/12.210860 PG 9 WC Instruments & Instrumentation; Remote Sensing; Optics SC Instruments & Instrumentation; Remote Sensing; Optics GA BD35K UT WOS:A1995BD35K00033 ER PT J AU BISHOP, PA LEE, SMC MCBRINE, JJ SINCONOLFI, SF GREENISEN, MC AF BISHOP, PA LEE, SMC MCBRINE, JJ SINCONOLFI, SF GREENISEN, MC TI VALIDATION AND EVALUATION OF A LIGHTWEIGHT PORTABLE DEVICE FOR MEASURING VO2 SO AMERICAN INDUSTRIAL HYGIENE ASSOCIATION JOURNAL LA English DT Article ID OXYGEN-CONSUMPTION; SYSTEM AB The accuracy and utility of a portable, lightweight (1.3 kg total) battery-powered telemetry system (PMS) for measuring the oxygen uptake (VO2) of humans was evaluated. Ventilation measurements agreed closely with a mechanical calibrator and a reference system (REF) (R2 = 0.99-1.0). Measures of VO2 (78 total observations, 13 subjects) were compared in humans between the PMS and a mass-spectrometer based REF over a broad range of VO2s and for 30 min at a constant work rate. Agreement between systems was maximized by: VO2REF (L/min) = 0.94VO2PMS(raw) -0.06 R2 = 0.97; S(yx) = 0.148. Cross-validation on 26 data points yielded an R2 of 0.97 and a S(yx) of 0.11 L/min. Drift in VO2 measures was acceptable in relation to time and across the range of VO2s. With the above equation, the PMS VO2s were sufficiently accurate for many research and monitoring applications. The PMS was also highly portable, mechanically reliable, comfortable for the subjects even for prolonged use, and potentially useful in many industrial situations. C1 UNIV ALABAMA,UNIVERSITY,AL 35486. NASA,LYNDON B JOHNSON SPACE CTR,EXERCISE PHYSIOL LAB,HOUSTON,TX 77058. KRUG LIFE SCI,HOUSTON,TX. NR 9 TC 1 Z9 1 U1 0 U2 0 PU AMER INDUSTRIAL HYGIENE ASSOC PI FAIRFAX PA 2700 PROSPERITY AVE #250, FAIRFAX, VA 22031-4307 SN 0002-8894 J9 AM IND HYG ASSOC J JI Am. Ind. Hyg. Assoc. J. PD JAN PY 1995 VL 56 IS 1 BP 50 EP 54 PG 5 WC Environmental Sciences; Public, Environmental & Occupational Health SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health GA QC620 UT WOS:A1995QC62000009 ER PT J AU SEVER, TL AF SEVER, TL TI REMOTE-SENSING SO AMERICAN JOURNAL OF ARCHAEOLOGY LA English DT Article RP SEVER, TL (reprint author), NASA,EARTH SCI PROGRAM OFF,JA-20,JOHN C STENNIS SPACE CTR,BAY ST LOUIS,MS 39529, USA. NR 8 TC 2 Z9 2 U1 0 U2 0 PU ARCHAEOLOGICAL INST PI NEW YORK PA 135 WILLIAM ST, NEW YORK, NY 10038-3805 SN 0002-9114 J9 AM J ARCHAEOL JI Am. J. Archaeol. PD JAN PY 1995 VL 99 IS 1 BP 83 EP 84 PG 2 WC Archaeology SC Archaeology GA QH140 UT WOS:A1995QH14000005 ER PT B AU Ellis, SR Bucher, UJ Menges, BM AF Ellis, SR Bucher, UJ Menges, BM BE Sheridan, TB TI The relationship of binocular convergence and errors in judged distance to virtual objects SO ANALYSIS, DESIGN AND EVALUATION OF MAN-MACHINE SYSTEMS 1995, VOLS 1 AND 2 LA English DT Proceedings Paper CT 6th IFAC/IFIP/IFORS/IEA Symposium on Analysis, Design and Evaluation of Man-Machine Systems CY JUN 27-29, 1995 CL MIT, CAMBRIDGE, MA SP Int Federat Automat Control, Tech Comm Syst Engn, Int Federat Automat Control, Tech Comm Social Effects Automat, Amer Automat Control Council, Int Federat Informat Proc, Int Federat Operat Res Soc, Int Ergon Assoc HO MIT DE see-through display; virtual objects; stereo vision; computer-aided work; binocular convergence C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD, ENGLAND OX5 1GB BN 0-08-042370-1 PY 1995 BP 253 EP 257 PG 5 WC Automation & Control Systems; Computer Science, Cybernetics; Ergonomics SC Automation & Control Systems; Computer Science; Engineering GA BF64X UT WOS:A1995BF64X00039 ER PT B AU Corker, KM Pisanich, GM AF Corker, KM Pisanich, GM BE Sheridan, TB TI Analysis and modeling of flight crew performance in automated air traffic management systems SO ANALYSIS, DESIGN AND EVALUATION OF MAN-MACHINE SYSTEMS 1995, VOLS 1 AND 2 LA English DT Proceedings Paper CT 6th IFAC/IFIP/IFORS/IEA Symposium on Analysis, Design and Evaluation of Man-Machine Systems CY JUN 27-29, 1995 CL MIT, CAMBRIDGE, MA SP Int Federat Automat Control, Tech Comm Syst Engn, Int Federat Automat Control, Tech Comm Social Effects Automat, Amer Automat Control Council, Int Federat Informat Proc, Int Federat Operat Res Soc, Int Ergon Assoc HO MIT DE air traffic control; aircraft operations; modelling; computer simulation C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD, ENGLAND OX5 1GB BN 0-08-042370-1 PY 1995 BP 547 EP 552 PG 6 WC Automation & Control Systems; Computer Science, Cybernetics; Ergonomics SC Automation & Control Systems; Computer Science; Engineering GA BF64X UT WOS:A1995BF64X00087 ER PT J AU HORBURY, T BALOGH, A FORSYTH, RJ SMITH, EJ AF HORBURY, T BALOGH, A FORSYTH, RJ SMITH, EJ TI ULYSSES MAGNETIC-FIELD OBSERVATIONS OF FLUCTUATIONS WITHIN POLAR CORONAL FLOWS SO ANNALES GEOPHYSICAE-ATMOSPHERES HYDROSPHERES AND SPACE SCIENCES LA English DT Letter ID SOLAR-WIND; TURBULENCE; EVOLUTION AB The Ulysses spacecraft has gathered data from within flows from the Sun's southern polar coronal hole, the first in situ measurement of this region. We present a brief analysis of the heliospheric magnetic field data from this region, using a fractal method. As is the case near the ecliptic, estimated spectral exponents are near 5/3 on spacecraft scales of seconds to minutes. On longer time scales, however, there appears to be a significantly different population in polar flows, which is similar to that found by the Hellos spacecraft in fast solar wind flows at 0.3 AU. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. RP HORBURY, T (reprint author), UNIV LONDON IMPERIAL COLL SCI & TECHNOL,BLACKETT LAB,LONDON SW7 2BZ,ENGLAND. NR 16 TC 20 Z9 21 U1 0 U2 0 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0992-7689 J9 ANN GEOPHYS JI Ann. Geophys.-Atmos. Hydrospheres Space Sci. PD JAN PY 1995 VL 13 IS 1 BP 105 EP 107 PG 3 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA QD945 UT WOS:A1995QD94500012 ER PT B AU ZWALLY, HJ GIOVINETTO, MB AF ZWALLY, HJ GIOVINETTO, MB BE Rothrock, DA TI Accumulation in Antarctica and Greenland derived from passive-microwave data: A comparison with contoured compilations SO ANNALS OF GLACIOLOGY, VOL 21, 1995: PROCEEDINGS OF THE INTERNATIONAL SYMPOSIUM ON THE ROLE OF THE CRYOSPHERE IN GLOBAL CHANGE LA English DT Proceedings Paper CT 1994 International Symposium on the Role of the Cryosphere in Global Change CY AUG 07-12, 1994 CL OHIO STATE UNIV, BYRD POLAR RES CTR, COLUMBUS, OH SP Int Glaciol Soc, Byrd Polar Res Ctr, Amer Meteorol Soc, Amer Geophys Union HO OHIO STATE UNIV, BYRD POLAR RES CTR C1 GODDARD SPACE FLIGHT CTR,OCEANS & ICE BRANCH,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 1 PU INT GLACIOLOGICAL SOC PI CAMBRIDGE PA LENSFIELD RD, CAMBRIDGE, ENGLAND CB2 1ER BN 0-946417-15-6 PY 1995 BP 123 EP 130 PG 8 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA BD94D UT WOS:A1995BD94D00020 ER PT B AU THOMAS, R KRABILL, W FREDERICK, E JEZEK, K AF THOMAS, R KRABILL, W FREDERICK, E JEZEK, K BE Rothrock, DA TI Thickening of Jakobshavns Isbrae, West Greenland, measured by borne laser altimetry SO ANNALS OF GLACIOLOGY, VOL 21, 1995: PROCEEDINGS OF THE INTERNATIONAL SYMPOSIUM ON THE ROLE OF THE CRYOSPHERE IN GLOBAL CHANGE LA English DT Proceedings Paper CT 1994 International Symposium on the Role of the Cryosphere in Global Change CY AUG 07-12, 1994 CL OHIO STATE UNIV, BYRD POLAR RES CTR, COLUMBUS, OH SP Int Glaciol Soc, Byrd Polar Res Ctr, Amer Meteorol Soc, Amer Geophys Union HO OHIO STATE UNIV, BYRD POLAR RES CTR C1 NASA,WASHINGTON,DC 20546. NR 0 TC 0 Z9 0 U1 0 U2 1 PU INT GLACIOLOGICAL SOC PI CAMBRIDGE PA LENSFIELD RD, CAMBRIDGE, ENGLAND CB2 1ER BN 0-946417-15-6 PY 1995 BP 259 EP 262 PG 4 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA BD94D UT WOS:A1995BD94D00041 ER PT B AU HALL, DK WILLIAMS, RS SIGURDSSON, O AF HALL, DK WILLIAMS, RS SIGURDSSON, O BE Rothrock, DA TI Glaciological observations of Bruarjokull, Iceland, using synthetic aperture radar and thematic mapper satellite data SO ANNALS OF GLACIOLOGY, VOL 21, 1995: PROCEEDINGS OF THE INTERNATIONAL SYMPOSIUM ON THE ROLE OF THE CRYOSPHERE IN GLOBAL CHANGE LA English DT Proceedings Paper CT 1994 International Symposium on the Role of the Cryosphere in Global Change CY AUG 07-12, 1994 CL OHIO STATE UNIV, BYRD POLAR RES CTR, COLUMBUS, OH SP Int Glaciol Soc, Byrd Polar Res Ctr, Amer Meteorol Soc, Amer Geophys Union HO OHIO STATE UNIV, BYRD POLAR RES CTR C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RI Hall, Dorothy/D-5562-2012 NR 0 TC 0 Z9 0 U1 0 U2 0 PU INT GLACIOLOGICAL SOC PI CAMBRIDGE PA LENSFIELD RD, CAMBRIDGE, ENGLAND CB2 1ER BN 0-946417-15-6 PY 1995 BP 271 EP 276 PG 6 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA BD94D UT WOS:A1995BD94D00043 ER PT B AU PARKINSON, CL AF PARKINSON, CL BE Rothrock, DA TI Recent sea-ice advances in Baffin Bay Davis Strait and retreats in the Bellingshausen Sea SO ANNALS OF GLACIOLOGY, VOL 21, 1995: PROCEEDINGS OF THE INTERNATIONAL SYMPOSIUM ON THE ROLE OF THE CRYOSPHERE IN GLOBAL CHANGE LA English DT Proceedings Paper CT 1994 International Symposium on the Role of the Cryosphere in Global Change CY AUG 07-12, 1994 CL OHIO STATE UNIV, BYRD POLAR RES CTR, COLUMBUS, OH SP Int Glaciol Soc, Byrd Polar Res Ctr, Amer Meteorol Soc, Amer Geophys Union HO OHIO STATE UNIV, BYRD POLAR RES CTR C1 NASA,GODDARD SPACE FLIGHT CTR,OCEANS & ICE BRANCH,GREENBELT,MD 20771. RI Parkinson, Claire/E-1747-2012 OI Parkinson, Claire/0000-0001-6730-4197 NR 0 TC 0 Z9 0 U1 1 U2 1 PU INT GLACIOLOGICAL SOC PI CAMBRIDGE PA LENSFIELD RD, CAMBRIDGE, ENGLAND CB2 1ER BN 0-946417-15-6 PY 1995 BP 348 EP 352 PG 5 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA BD94D UT WOS:A1995BD94D00055 ER PT B AU LISTON, GE HALL, DK AF LISTON, GE HALL, DK BE Rothrock, DA TI Sensitivity of lake freeze-up and break-up to climate change: A physically based modeling study SO ANNALS OF GLACIOLOGY, VOL 21, 1995: PROCEEDINGS OF THE INTERNATIONAL SYMPOSIUM ON THE ROLE OF THE CRYOSPHERE IN GLOBAL CHANGE LA English DT Proceedings Paper CT 1994 International Symposium on the Role of the Cryosphere in Global Change CY AUG 07-12, 1994 CL OHIO STATE UNIV, BYRD POLAR RES CTR, COLUMBUS, OH SP Int Glaciol Soc, Byrd Polar Res Ctr, Amer Meteorol Soc, Amer Geophys Union HO OHIO STATE UNIV, BYRD POLAR RES CTR C1 NASA,GODDARD SPACE FLIGHT CTR,HYDROL SCI BRANCH,GREENBELT,MD 20771. RI Hall, Dorothy/D-5562-2012 NR 0 TC 0 Z9 0 U1 0 U2 0 PU INT GLACIOLOGICAL SOC PI CAMBRIDGE PA LENSFIELD RD, CAMBRIDGE, ENGLAND CB2 1ER BN 0-946417-15-6 PY 1995 BP 387 EP 393 PG 7 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA BD94D UT WOS:A1995BD94D00061 ER PT S AU LISK, RC AF LISK, RC GP IEEE TI THE ROLE OF THE R&M DISCIPLINES IN THE NEW NASA SO ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM - 1995 PROCEEDINGS SE PROCEEDINGS : ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM LA English DT Proceedings Paper CT 1995 Annual Reliability and Maintainability Symposium CY JAN 16-19, 1995 CL WASHINGTON, DC SP IEEE DE SYSTEMS ENGINEERING; CONCURRENT ENGINEERING; COST EFFECTIVENESS; ASSURANCE TECHNOLOGIES C1 NASA,WASHINGTON,DC 20546. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 SN 0149-144X BN 0-7803-2470-6 J9 P A REL MAI PY 1995 BP 112 EP 117 DI 10.1109/RAMS.1995.513232 PG 6 WC Engineering, Industrial; Engineering, Manufacturing SC Engineering GA BC87S UT WOS:A1995BC87S00019 ER PT S AU EVANS, J LALL, P BAUERNSCHUB, R AF EVANS, J LALL, P BAUERNSCHUB, R GP IEEE TI A FRAMEWORK FOR RELIABILITY MODELING OF ELECTRONICS SO ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM - 1995 PROCEEDINGS SE PROCEEDINGS : ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM LA English DT Proceedings Paper CT 1995 Annual Reliability and Maintainability Symposium CY JAN 16-19, 1995 CL WASHINGTON, DC SP IEEE DE PHYSICS-OF-FAILURE; ELECTRONIC PACKAGING; FAILURE MECHANISMS; ACCELERATED TESTING; SCREENING; DERATING; MULTICHIP MODULES C1 NASA,WASHINGTON,DC 20546. NR 0 TC 5 Z9 5 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 SN 0149-144X BN 0-7803-2470-6 J9 P A REL MAI PY 1995 BP 144 EP 151 DI 10.1109/RAMS.1995.513238 PG 8 WC Engineering, Industrial; Engineering, Manufacturing SC Engineering GA BC87S UT WOS:A1995BC87S00025 ER PT S AU JENKINS, JP MIZELL, D LOFTIN, RB SATAVA, RM HARTT, HN AF JENKINS, JP MIZELL, D LOFTIN, RB SATAVA, RM HARTT, HN GP IEEE TI PANEL - VIRTUAL REALITY APPLICATIONS - TECHNOLOGY FOR ASSURANCE SO ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM - 1995 PROCEEDINGS SE PROCEEDINGS : ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM LA English DT Proceedings Paper CT 1995 Annual Reliability and Maintainability Symposium CY JAN 16-19, 1995 CL WASHINGTON, DC SP IEEE DE VIRTUAL ENVIRONMENT; TELEPRESENCE; INTERACTIVE SYSTEM; HIGH PERFORMANCE COMPUTING AND COMMUNICATION (HPCC) C1 NASA,WASHINGTON,DC 20546. NR 0 TC 1 Z9 1 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 SN 0149-144X BN 0-7803-2470-6 J9 P A REL MAI PY 1995 BP 188 EP 192 PG 5 WC Engineering, Industrial; Engineering, Manufacturing SC Engineering GA BC87S UT WOS:A1995BC87S00032 ER PT S AU HULET, MW CARROLL, CW AF HULET, MW CARROLL, CW GP IEEE TI AVOIDING SAFETY-MANAGEMENT ERRORS IN THE NEXT GENERATION SO ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM - 1995 PROCEEDINGS SE PROCEEDINGS : ANNUAL RELIABILITY AND MAINTAINABILITY SYMPOSIUM LA English DT Proceedings Paper CT 1995 Annual Reliability and Maintainability Symposium CY JAN 16-19, 1995 CL WASHINGTON, DC SP IEEE DE SAFETY; MANAGEMENT; HUMAN ERROR C1 NASA,AMES PRES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 SN 0149-144X BN 0-7803-2470-6 J9 P A REL MAI PY 1995 BP 496 EP 501 DI 10.1109/RAMS.1995.513290 PG 6 WC Engineering, Industrial; Engineering, Manufacturing SC Engineering GA BC87S UT WOS:A1995BC87S00078 ER PT J AU GOLDSTEIN, ML ROBERTS, DA MATTHAEUS, WH AF GOLDSTEIN, ML ROBERTS, DA MATTHAEUS, WH TI MAGNETOHYDRODYNAMIC TURBULENCE IN THE SOLAR-WIND SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS LA English DT Article DE INTERPLANETARY MEDIUM; ALFVENIC FLUCTUATIONS; SHEAR INSTABILITIES; NONLINEAR INTERACTIONS ID INTERPLANETARY ALFVENIC FLUCTUATIONS; INHOMOGENEOUS MHD TURBULENCE; INTER-PLANETARY SPACE; LOW MACH NUMBER; MAGNETIC-FIELD; DENSITY-FLUCTUATIONS; POWER SPECTRUM; INCOMPRESSIBLE FLUIDS; STREAM STRUCTURE; CROSS-HELICITY AB The fluctuations in magnetic field and plasma velocity in the solar wind possess many features expected of fully developed magnetohydrodynamic turbulence. Understanding this nonlinear system is complicated by the dynamical effects of velocity shear between fast and slow solar wind streams, by the spherical expansion of the solar wind, and by its compressibility. Direct spacecraft observations from 0.3 to over 20 AU, radio scintillation observations of plasmas near the Sun, numerical simulations, and various models provide complementary methods that have shown convincingly that the fluctuations in the wind parameters undergo significant dynamical evolution independent of whatever turbulence might exist in the solar photosphere and corona. This rich area of study allows one to test theories of turbulence against direct observation, and to use observations to guide and motivate development of turbulence theories. The solar wind thus provides an excellent laboratory for studying many fundamental questions about turbulent plasmas. C1 UNIV DELAWARE, BARTOL RES INST, NEWARK, DE 19716 USA. RP GOLDSTEIN, ML (reprint author), NASA, GODDARD SPACE FLIGHT CTR, CODE 692, GREENBELT, MD 20771 USA. RI Roberts, Dana/D-4625-2012; Goldstein, Melvyn/B-1724-2008 NR 185 TC 382 Z9 385 U1 6 U2 20 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 1995 VL 33 BP 283 EP 325 DI 10.1146/annurev.aa.33.090195.001435 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RX082 UT WOS:A1995RX08200010 ER PT J AU WEISSMAN, PR AF WEISSMAN, PR TI THE KUIPER BELT SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS LA English DT Article DE SHORT-PERIOD COMETS; LONG-PERIOD COMETS; PLANETESIMALS; OUTER SOLAR SYSTEM ID SHORT-PERIOD COMETS; OUTER SOLAR-SYSTEM; CHAOTIC MOTION; TAURUS-AURIGA; BETA-PICTORIS; ORIGIN; DISK; CLOUD; NEPTUNE; STATE AB The Kuiper belt is a ring of icy planetesimals, i.e. comets, beyond the orbit of Neptune, a remnant of the formation of the solar system. These volatile-rich bodies never accreted into a planet because of the decreasing surface density of the solar nebula accretion disk and the increasingly long orbital periods at large heliocentric distances. The inner region of the Kuiper belt, between 34 and 45 AU, is dynamically active with an estimated population of similar to 6 x 10(9) objects, and it is likely the source of the Jupiter-family short-period comets. The dynamically inactive region beyond 45 AU may extend out to 10(3) AU or more and may contain up to several times 10(13) objects with a total mass of several hundred Earth masses. Observational searches have so far discovered 18 objects in the Kuiper belt, ranging in diameter from similar to 90 to 360 km. IRAS dust disks around nearby stars are likely similar, comet belt structures. RP WEISSMAN, PR (reprint author), CALTECH, JET PROP LAB, DIV EARTH & SPACE SCI, PASADENA, CA 91109 USA. NR 94 TC 41 Z9 41 U1 0 U2 0 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 1995 VL 33 BP 327 EP 357 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RX082 UT WOS:A1995RX08200011 ER PT J AU FISHMAN, GJ MEEGAN, CA AF FISHMAN, GJ MEEGAN, CA TI GAMMA-RAY BURSTS SO ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICS LA English DT Article DE GAMMA-RAY SOURCES; X-RAY; NEUTRON STARS; COSMOLOGY ID GALACTIC HALO; OPTICAL COUNTERPARTS; SPATIAL-DISTRIBUTION; GRAVITATIONAL-WAVES; BLACK-HOLES; V/VMAX TEST; MODELS; STATISTICS; FIREBALLS; TRANSIENT AB The present status of gamma-ray burst research is reviewed, with an emphasis on recent observations of their temporal, spectral, and global distribution properties. The observed sky distribution of weak gamma-ray bursts constrains the allowable geometrical models to sources in either a giant spherical galactic halo or to sources at cosmological distances. Observations of time dilation consistent with the latter have been reported. Extensive searches for a counterpart to gamma-ray bursts in other wavelength regions have thus far proved negative. In spite of the abundance of new observations of gamma-ray bursts, their energy source and emission mechanism remain highly speculative. New, rapid counterpart search efforts and several new space-borne experiments may provide the needed observations to make progress in the field. RP FISHMAN, GJ (reprint author), NASA, GEORGE C MARSHALL SPACE FLIGHT CTR, SPACE SCI LAB, HUNTSVILLE, AL 35812 USA. NR 274 TC 419 Z9 427 U1 0 U2 5 PU ANNUAL REVIEWS PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 USA SN 0066-4146 J9 ANNU REV ASTRON ASTR JI Annu. Rev. Astron. Astrophys. PY 1995 VL 33 BP 415 EP 458 DI 10.1146/annurev.aa.33.090195.002215 PG 44 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA RX082 UT WOS:A1995RX08200014 ER PT J AU ERICKSON, GE AF ERICKSON, GE TI HIGH ANGLE-OF-ATTACK AERODYNAMICS SO ANNUAL REVIEW OF FLUID MECHANICS LA English DT Review DE VORTEX FLOWS; SEPARATED FLOWS; ATTACHED FLOWS; SHOCK WAVES; WIND TUNNELS; FLIGHT TESTING; COMPUTATIONAL FLUID DYNAMICS RP ERICKSON, GE (reprint author), NASA,LANGLEY RES CTR,HAMPTON,VA 23681, USA. NR 105 TC 11 Z9 14 U1 0 U2 10 PU ANNUAL REVIEWS INC PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 SN 0066-4189 J9 ANNU REV FLUID MECH JI Annu. Rev. Fluid Mech. PY 1995 VL 27 BP 45 EP 88 DI 10.1146/annurev.fl.27.010195.000401 PG 44 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA QC817 UT WOS:A1995QC81700004 ER PT J AU SQUIRE, VA DUGAN, JP WADHAMS, P ROTTIER, PJ LIU, AK AF SQUIRE, VA DUGAN, JP WADHAMS, P ROTTIER, PJ LIU, AK TI OF OCEAN WAVES AND SEA-ICE SO ANNUAL REVIEW OF FLUID MECHANICS LA English DT Review DE MARGINAL ICE ZONE; CONTINUOUS SEA ICE; BIPOLAR; MODELING; FIELD EXPERIMENTS ID SYNTHETIC APERTURE RADAR; ARCTIC PACK ICE; SHORE FAST ICE; FLOE COLLISIONS; GRAVITY-WAVES; GREENLAND SEA; EDGE NOISE; ZONE; MODEL; ATTENUATION C1 ONR EUROPEAN OFF,LONDON NW1 5TH,ENGLAND. UNIV CAMBRIDGE,SCOTT POLAR RES INST,CAMBRIDGE CB2 1ER,ENGLAND. BAESEMA LTD,GLASGOW G2 8JE,LANARK,SCOTLAND. NASA,GODDARD SPACE FLIGHT CTR,OCEANS & ICE BRANCH,GREENBELT,MD 20771. RP SQUIRE, VA (reprint author), UNIV OTAGO,DEPT MATH & STAT,DUNEDIN,NEW ZEALAND. NR 139 TC 177 Z9 181 U1 2 U2 24 PU ANNUAL REVIEWS INC PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 SN 0066-4189 J9 ANNU REV FLUID MECH JI Annu. Rev. Fluid Mech. PY 1995 VL 27 BP 115 EP 168 PG 54 WC Mechanics; Physics, Fluids & Plasmas SC Mechanics; Physics GA QC817 UT WOS:A1995QC81700006 ER PT J AU MANCINELLI, RL AF MANCINELLI, RL TI THE REGULATION OF METHANE OXIDATION IN SOIL SO ANNUAL REVIEW OF MICROBIOLOGY LA English DT Review DE METHANOTROPHY; METHYLOTROPHY; SOIL; METHANOTROPH ECOLOGY ID METHYLOSINUS-TRICHOSPORIUM OB3B; METHYLOCOCCUS-CAPSULATUS-BATH; TEMPERATE FOREST SOILS; MONO-OXYGENASE; UTILIZING BACTERIA; NITROUS-OXIDE; METHYLOTROPHIC BACTERIA; METHANOTROPHIC BACTERIA; OXIDIZING ORGANISMS; MICROBIAL OXIDATION AB The atmospheric concentration of methane, a greenhouse gas, has more than doubled during the past 200 years. Consequently, identifying the factors influencing the flux of methane into the atmosphere is becoming increasingly important. Methanotrophs, microaerophilic organisms widespread in aerobic soils and sediments, oxidize methane to derive energy and carbon for biomass. In so doing, they play an important role in mitigating the flux of methane into the atmosphere. Several physico-chemical factors influence rates of methane oxidation in soil, including soil diffusivity; water potential; and levels of oxygen, methane, ammonium, nitrate, nitrite, and copper. Most of these factors exert their influence through interactions with methane monooxygenase (MMO), the enzyme that catalyzes the reaction converting methane to methanol, the first step in methane oxidation. Although biological factors such as competition and predation undoubtedly play a role in regulating the methanotroph population in soils, and thereby limit the amount of methane consumed by methanotrophs, the significance of these factors is unknown. Obtaining a better understanding of the ecology of methanotrophs will help elucidate the mechanisms that regulate soil methane oxidation. RP MANCINELLI, RL (reprint author), NASA,AMES RES CTR,MAIL STOP 239-12,MOFFETT FIELD,CA 94035, USA. RI Mancinelli, Rocco/L-8971-2016 NR 218 TC 111 Z9 118 U1 6 U2 39 PU ANNUAL REVIEWS INC PI PALO ALTO PA 4139 EL CAMINO WAY, PO BOX 10139, PALO ALTO, CA 94303-0139 SN 0066-4227 J9 ANNU REV MICROBIOL JI Annu. Rev. Microbiol. PY 1995 VL 49 BP 581 EP 605 PG 25 WC Microbiology SC Microbiology GA TB319 UT WOS:A1995TB31900021 PM 8561473 ER PT B AU SAID, MA THOMAS, V AF SAID, MA THOMAS, V GP SOC PLAST ENGINEERS TI Thin film discriminator criteria for polyethylene scientific balloons SO ANTEC 95 - THE PLASTICS CHALLENGER: A REVOLUTION IN EDUCATION, CONFERENCE PROCEEDINGS, VOLS I-III: VOL I: PROCESSING; VOL II: MATERIALS; VOL III: SPECIAL AREAS LA English DT Proceedings Paper CT 53rd Annual Technical Conference of the Society-of-Plastics-Engineers - The Plastics Challenge: A Revolution in Education CY MAY 07-11, 1995 CL BOSTON, MA SP Soc Plast Engineers C1 NASA,GODDARD SPACE FLIGHT CTR,WALLOPS FLIGHT FACIL,WALLOPS ISL,VA 23337. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SOC PLASTICS ENGINEERS PI BROOKFIELD CENTER PA 14 FAIRFIELD DR, BROOKFIELD CENTER, CT 06805 BN 1-56676-319-3 PY 1995 BP 2419 EP 2423 PG 5 WC Engineering, Chemical; Polymer Science SC Engineering; Polymer Science GA BD81E UT WOS:A1995BD81E00426 ER PT S AU RANDOLPH, JE AF RANDOLPH, JE BE Wenzel, KP Sarris, ET TI NASA SOLAR PROBE MISSION AND SYSTEM CONCEPTS SO ANTICIPATING A SOLAR PROBE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT D1 2 Meeting of COSPAR Scientific Commission D on Anticipating a Solar Probe, at the 30th COSPAR Scientific Assembly CY JUL 11-21, 1994 CL HAMBURG, GERMANY SP Comm Space Res AB Major evolutionary steps have occurred recently and will be reviewed in the design of the Solar Probe mission resulting in a new lightweight and low cost concept that will. change the earlier perceptions of this scientifically exciting mission. NASA program guidelines emphasize low lifecycle-costs which include the launch vehicle and mission operations costs. The new Solar Probe concept reflects these guidelines and is consistent with a realistic life-cycle cost of less than four hundred million dollars for a dual spacecraft mission. This has been possible with the inheritance of high technology systems that have been developed for other missions during the past decade. In addition, a proposed scientific instrument payload with significantly reduced mass was accommodated on the smaller spacecraft. New mission design concepts have optimized the encounter (perihelion) trajectory conditions allowing a new parabolic shield concept. The perihelion radius is specified at four solar radii to capture as many of the scientific objectives consistent with the thermal environmental constraints, The trajectory with these perihelion conditions relies on Jupiter to provide the energy change necessary to achieve the final orbit. With the new low mass concept for the Solar Probe, a small launch vehicle such as a Delta can provide the required launch energy. System design concepts consistent with these mission requirements and small and low cost system elements will be discussed in the context of three case studies describing the evolution of the spacecraft and mission design concepts and their accommodation of scientific experiments over the past two decades. Details of some of the principal technology elements of the spacecraft will also be presented. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. RP RANDOLPH, JE (reprint author), NASA,DIV SPACE PHYS,CODE SS,WASHINGTON,DC 20546, USA. NR 31 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0273-1177 BN 0-08-042643-3 J9 ADV SPACE RES PY 1995 VL 17 IS 3 BP 3 EP 12 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA BD47J UT WOS:A1995BD47J00001 ER PT S AU MCNUTT, RL REYNOLDS, EL MCADAMS, JV BOKULIC, RS BHATNAGAR, V WILLIAMS, BD WILLEY, CE MYERS, R GEFERT, LP AF MCNUTT, RL REYNOLDS, EL MCADAMS, JV BOKULIC, RS BHATNAGAR, V WILLIAMS, BD WILLEY, CE MYERS, R GEFERT, LP BE Wenzel, KP Sarris, ET TI MISSION TO THE SUN - THE SOLAR PIONEER SO ANTICIPATING A SOLAR PROBE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT D1 2 Meeting of COSPAR Scientific Commission D on Anticipating a Solar Probe, at the 30th COSPAR Scientific Assembly CY JUL 11-21, 1994 CL HAMBURG, GERMANY SP Comm Space Res AB The Solar Pioneer is a mission concept developed by the Johns Hopkins University Applied Physics Laboratory (JHU/APL) to do exploratory science in the inner heliosphere and outer solar corona. The concept is derived from the Near Earth Asteroid Rendezvous (NEAR) spacecraft now being built by JHU/APL for NASA and draws upon that design to the maximum extent possible. The primary purpose, to conduct an exploratory in situ basic science investigation, has been focused to emphasize in situ particles and fields measurements of the outer solar corona and inner solar wind region. The purpose of the Solar Pioneer is to deliver a payload of scientific instruments to approximately 4 solar radii. The basic characteristics of the JHU/APL baseline concept provide for delivery of 30 to 50 kg of scientific payload to 4 R(S) while maintaining a high data rate. Life-cycle cost control is obtained by: (1) focusing on prime science objectives, (2) applying advanced technology where it makes sense, and (3) capitalizing on developed subsystems derived from the NEAR spacecraft. By implementing a focused strategy from science goals through all stages of program management, such a mission can be carried out for less than one quarter of previous Solar Probe mission cost estimates. C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. RP MCNUTT, RL (reprint author), JOHNS HOPKINS UNIV,APPL PHYS LAB,LAUREL,MD 20723, USA. RI McNutt, Ralph/E-8006-2010 OI McNutt, Ralph/0000-0002-4722-9166 NR 21 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0273-1177 BN 0-08-042643-3 J9 ADV SPACE RES PY 1995 VL 17 IS 3 BP 21 EP 30 PG 10 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA BD47J UT WOS:A1995BD47J00003 ER PT S AU FELDMAN, W GOLDSTEIN, B TSURUTANI, B AF FELDMAN, W GOLDSTEIN, B TSURUTANI, B BE Wenzel, KP Sarris, ET TI SCIENTIFIC OBJECTIVES OF A SOLAR PROBE MISSION SO ANTICIPATING A SOLAR PROBE SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT D1 2 Meeting of COSPAR Scientific Commission D on Anticipating a Solar Probe, at the 30th COSPAR Scientific Assembly CY JUL 11-21, 1994 CL HAMBURG, GERMANY SP Comm Space Res ID WIND AB Solar Probe is a mission of exploration and discovery in a region near the Sun that has never previously been directly investigated. Major advances and surprises in our understanding of the planets resulted from the first planetary exploratory missions; Solar Probe should similarly revolutionize our understanding of the corona and the solar wind. The first in situ measurements of coronal particles and fields will provide definitive discriminators amongst many currently proposed models of processes that shape the structure and dynamics of the outer corona and solar wind. In addition, observation of the development of turbulence, nonlinear wave processes, plasma heating, and particle acceleration in the corona will advance our understanding of these areas of plasma physics in a new regime neither duplicated by Earth-based laboratories nor by previous space exploration. It will also fill the last gap between our knowledge of the terrestrial response to the solar output as well as provide insight for interpreting observations of general stellar envelopes. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. RP FELDMAN, W (reprint author), LOS ALAMOS NATL LAB,LOS ALAMOS,NM 87545, USA. NR 18 TC 0 Z9 0 U1 0 U2 0 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0273-1177 BN 0-08-042643-3 J9 ADV SPACE RES PY 1995 VL 17 IS 3 BP 41 EP 47 PG 7 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA BD47J UT WOS:A1995BD47J00005 ER PT B AU RAY, B GERBER, SS PATTERSON, RL MYERS, IT AF RAY, B GERBER, SS PATTERSON, RL MYERS, IT GP IEEE TI Low-temperature operation of a buck DC/DC converter SO APEC '95 - TENTH ANNUAL APPLIED POWER ELECTRONICS CONFERENCE AND EXPOSITION, CONFERENCE PROCEEDINGS 1995, VOLS 1 AND 2 LA English DT Proceedings Paper CT 10th Annual Applied Power Electronics Conference and Exposition (APEC 95) CY MAR 05-09, 1995 CL DALLAS, TX SP IEEE, Power Electr Soc, IEEE, Ind Applicat Soc, Power Sources Manufacturers Assoc C1 NASA,NRC,CLEVELAND,OH 44135. NR 0 TC 0 Z9 0 U1 0 U2 0 PU I E E E PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 BN 0-7803-2482-X J9 APPL POWER ELECT CO PY 1995 BP 941 EP 946 PG 6 WC Engineering, Electrical & Electronic SC Engineering GA BD23R UT WOS:A1995BD23R00133 ER PT B AU Watson, MD Abushagur, M Ashley, PR JohnsonCole, H AF Watson, MD Abushagur, M Ashley, PR JohnsonCole, H BE Jannson, T TI Polymer waveguide output coupler SO APPLICATION AND THEORY OF PERIODIC STRUCTURES SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Application and Theory of Periodic Structures CY JUL 10-12, 1995 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE diffraction grating; integrated optics; non-planar coupling; optical interconnection; polymer; waveguide C1 NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,DATA ACQUISIT & DISTRIBUT BRANCH,HUNTSVILLE,AL 35812. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1891-9 J9 P SOC PHOTO-OPT INS PY 1995 VL 2532 BP 131 EP 140 DI 10.1117/12.221219 PG 4 WC Optics SC Optics GA BE29E UT WOS:A1995BE29E00013 ER PT B AU LYON, RG DORBAND, JE HOLLIS, JM AF LYON, RG DORBAND, JE HOLLIS, JM BE Tescher, AG TI Characterization of a maximum entropy image reconstruction algorithm SO APPLICATIONS OF DIGITAL IMAGE PROCESSING XVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT 1995 Symposium on Applications of Digital Image Processing XVIII CY JUL 12-14, 1995 CL SAN DIEGO, CA SP Soc Photo Opt Instrumentat Engineers DE IMAGE ENHANCEMENT; IMAGE RESTORATION; MAXIMUM ENTROPY; HUBBLE SPACE TELESCOPE; POINT SPREAD FUNCTION C1 NASA,GODDARD SPACE FLIGHT CTR,CTR EXCELLENCE SPACE DATA & INFORMAT SCI,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1923-0 J9 P SOC PHOTO-OPT INS PY 1995 VL 2564 BP 126 EP 135 DI 10.1117/12.217392 PG 10 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods; Optics SC Computer Science; Optics GA BD96W UT WOS:A1995BD96W00013 ER PT B AU BARNES, WL SALOMONSON, VV AF BARNES, WL SALOMONSON, VV BE Lampropoulos, GA Chrostowski, J Measures, RM TI Design and projected performance of MODIS - A moderate-resolution imaging spectroradiometer for the Earth Observing System (EOS) SO APPLICATIONS OF PHOTONIC TECHNOLOGY LA English DT Proceedings Paper CT International Conference on Applications of Photonic Technology, Sensing, Signal Processing, and Communications CY JUN 21-23, 1994 CL TORONTO, CANADA C1 NASA,GODDARD SPACE FLIGHT CTR,HYDROSPHER PROCESSES LAB,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU PLENUM PRESS DIV PLENUM PUBLISHING CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 BN 0-306-45011-9 PY 1995 BP 171 EP 178 PG 8 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Optics; Physics, Applied; Telecommunications SC Engineering; Instruments & Instrumentation; Optics; Physics; Telecommunications GA BE11H UT WOS:A1995BE11H00034 ER PT B AU CHENG, LJ AF CHENG, LJ BE Lampropoulos, GA Chrostowski, J Measures, RM TI A polarimetric hyperspectral imaging sensor SO APPLICATIONS OF PHOTONIC TECHNOLOGY LA English DT Proceedings Paper CT International Conference on Applications of Photonic Technology, Sensing, Signal Processing, and Communications CY JUN 21-23, 1994 CL TORONTO, CANADA C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. NR 0 TC 1 Z9 1 U1 0 U2 0 PU PLENUM PRESS DIV PLENUM PUBLISHING CORP PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 BN 0-306-45011-9 PY 1995 BP 183 EP 189 PG 7 WC Engineering, Electrical & Electronic; Instruments & Instrumentation; Optics; Physics, Applied; Telecommunications SC Engineering; Instruments & Instrumentation; Optics; Physics; Telecommunications GA BE11H UT WOS:A1995BE11H00036 ER PT B AU WALLER, MJ AF WALLER, MJ BE Mcdonald, N Johnston, N Fuller, R TI WORK GROUP MULTITASKING IN AVIATION SO APPLICATIONS OF PSYCHOLOGY TO THE AVIATION SYSTEM - PROCEEDINGS OF THE 21ST CONFERENCE OF THE EUROPEAN ASSOCIATION FOR AVIATION PSYCHOLOGY (EAAP), VOL 1 LA English DT Proceedings Paper CT 21st Conference of the European-Association-for-Aviation-Psychology CY 1994 CL IRELAND SP EUROPEAN ASSOC AVIAT PSYCHOL RP WALLER, MJ (reprint author), UNIV TEXAS,NASA,FAA AEROSP CREW RES PROJECT,DALLAS,TX 75230, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AVEBURY PI ALDERSHOT PA GOWER HOUSE, CROFT RD, ALDERSHOT, HANTS, ENGLAND GU11 3HR BN 0-291-39818-9 PY 1995 BP 256 EP 261 PG 6 WC Psychology, Applied SC Psychology GA BC63P UT WOS:A1995BC63P00039 ER PT B AU MOSIER, KL SKITKA, LJ AF MOSIER, KL SKITKA, LJ BE Mcdonald, N Johnston, N Fuller, R TI AUTOMATION AND ACCOUNTABILITY SO APPLICATIONS OF PSYCHOLOGY TO THE AVIATION SYSTEM - PROCEEDINGS OF THE 21ST CONFERENCE OF THE EUROPEAN ASSOCIATION FOR AVIATION PSYCHOLOGY (EAAP), VOL 1 LA English DT Proceedings Paper CT 21st Conference of the European-Association-for-Aviation-Psychology CY 1994 CL IRELAND SP EUROPEAN ASSOC AVIAT PSYCHOL RP MOSIER, KL (reprint author), NASA,AMES RES CTR,MOFFETT FIELD,CA 94035, USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AVEBURY PI ALDERSHOT PA GOWER HOUSE, CROFT RD, ALDERSHOT, HANTS, ENGLAND GU11 3HR BN 0-291-39818-9 PY 1995 BP 275 EP 280 PG 6 WC Psychology, Applied SC Psychology GA BC63P UT WOS:A1995BC63P00043 ER PT B AU JACOBSON, NS AF JACOBSON, NS BE Nash, P Sundman, B TI Carbothermal reduction of silica in high temperature materials SO APPLICATIONS OF THERMODYNAMICS IN THE SYNTHESIS AND PROCESSING OF MATERIALS LA English DT Proceedings Paper CT Symposium on Applications of Thermodynamics in the Synthesis and Processing of Materials, at Materials Week 94 CY OCT 02-06, 1994 CL ROSEMONT, IL SP ASM Int, Thermodynam & Phase Equilibria Comm, Minerals Met & Mat Soc, Mat Design & Mfg Div C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. NR 0 TC 0 Z9 0 U1 1 U2 2 PU MINERALS, METALS & MATERIALS SOC PI WARRENDALE PA 420 COMMONWEALTH DR, WARRENDALE, PA 15086 BN 0-87339-291-4 PY 1995 BP 19 EP 27 PG 9 WC Thermodynamics; Materials Science, Multidisciplinary SC Thermodynamics; Materials Science GA BD50W UT WOS:A1995BD50W00002 ER PT B AU JACOBSON, NS AF JACOBSON, NS BE Nash, P Sundman, B TI Double Knudsen cell system for alloy activity measurements by mass spectrometry SO APPLICATIONS OF THERMODYNAMICS IN THE SYNTHESIS AND PROCESSING OF MATERIALS LA English DT Proceedings Paper CT Symposium on Applications of Thermodynamics in the Synthesis and Processing of Materials, at Materials Week 94 CY OCT 02-06, 1994 CL ROSEMONT, IL SP ASM Int, Thermodynam & Phase Equilibria Comm, Minerals Met & Mat Soc, Mat Design & Mfg Div C1 NASA,LEWIS RES CTR,CLEVELAND,OH 44135. NR 0 TC 6 Z9 6 U1 0 U2 0 PU MINERALS, METALS & MATERIALS SOC PI WARRENDALE PA 420 COMMONWEALTH DR, WARRENDALE, PA 15086 BN 0-87339-291-4 PY 1995 BP 319 EP 329 PG 11 WC Thermodynamics; Materials Science, Multidisciplinary SC Thermodynamics; Materials Science GA BD50W UT WOS:A1995BD50W00024 ER PT J AU ERICKSON, JD GRIMM, KA PENDLETON, TW HOWARD, LE GOODE, RA HAWKINS, MS BLOSS, D SEABORN, JA HESS, CW WALKER, D PHINNEY, DE NORSWORTHY, RS ANDERSON, G CHIEN, CH HEWGILL, L LITTLEFIELD, M GAUDIANO, F AF ERICKSON, JD GRIMM, KA PENDLETON, TW HOWARD, LE GOODE, RA HAWKINS, MS BLOSS, D SEABORN, JA HESS, CW WALKER, D PHINNEY, DE NORSWORTHY, RS ANDERSON, G CHIEN, CH HEWGILL, L LITTLEFIELD, M GAUDIANO, F TI AN INTELLIGENT SPACE ROBOT FOR CREW HELP AND CREW AND EQUIPMENT RETRIEVAL SO APPLIED INTELLIGENCE LA English DT Article DE REAL TIME; VISION; MANIPULATORS; MOBILITY; REACTING; PLANNING; GRASPING AB This paper describes the development status of a prototype supervised intelligent robot for space application for purposes of (1) helping the crew of a spacecraft such as the Space Station with various tasks such as holding objects and retrieving/replacing tools and other objects from/into storage, and for purposes of (2) retrieving detached objects, such as equipment or crew, that have become separated from their spacecraft. In addition to this set of tasks in this low Earth orbiting spacecraft environment, it is argued that certain aspects of the technology can be viewed as generic in approach, thereby offering insight into intelligent robots for other tasks and environments. Some candidate requirements for the space applications are presented which will be refined by the results of the prototype development and evaluation testing. Our development approach is described, including space simulation environments used in developmental testing. Candidate software architectures and their key technical issues which enable real work in real environments to be accomplished safely and robustly are addressed. Results of computer simulations of retrieving detached objects, including the situated reasoning/reaction plan approach used, are presented, as well as the results of an air bearing floor simulation of retrieving detached objects. Also described are characterization results on the usable reduced gravity environment in an aircraft flying parabolas (to simulate weightlessness) and results on hardware performance there. These results show it is feasible to use that environment for evaluative testing of dexterous grasping based on real-time vision of freely rotating and translating objects. C1 GHG INC,HOUSTON,TX. LOCKHEED ENGN & SCI CO,HOUSTON,TX 77058. RP ERICKSON, JD (reprint author), NASA,LYNDON B JOHNSON SPACE CTR,DIV AUTOMAT & ROBOT,ER,HOUSTON,TX 77058, USA. NR 87 TC 0 Z9 1 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0924-669X J9 APPL INTELL JI Appl. Intell. PD JAN PY 1995 VL 5 IS 1 BP 7 EP 39 DI 10.1007/BF00872781 PG 33 WC Computer Science, Artificial Intelligence SC Computer Science GA QH939 UT WOS:A1995QH93900002 ER PT J AU HE, QB YEH, P AF HE, QB YEH, P TI PHOTOREFRACTIVE MUTUALLY PUMPED PHASE-CONJUGATION WITH PARTIALLY COHERENT BEAMS SO APPLIED PHYSICS B-LASERS AND OPTICS LA English DT Article ID INCOHERENT BEAMS; MIRROR; BATIO3 AB We investigate the mutually pumped phase-conjugation process in photorefractive media with partially coherent pump beams. We consider the effects of transmission, reflection, and 2k-reflection gratings as well as the depletion of both pump beams. The theoretical results can be employed to qualitatively explain the experimental observations. C1 UNIV CALIF SANTA BARBARA,DEPT ELECT & COMP ENGN,SANTA BARBARA,CA 93106. ROCKWELL INT CORP,CTR SCI,ANAHEIM,CA 92803. RP HE, QB (reprint author), JET PROP LAB,MS 303-310,4800 OAK GROVE DR,PASADENA,CA 91109, USA. RI Yeh, Pochi/A-2109-2010 NR 17 TC 13 Z9 15 U1 0 U2 0 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0946-2171 J9 APPL PHYS B-LASERS O JI Appl. Phys. B-Lasers Opt. PD JAN PY 1995 VL 60 IS 1 BP 47 EP 50 DI 10.1007/BF01082072 PG 4 WC Optics; Physics, Applied SC Optics; Physics GA PZ096 UT WOS:A1995PZ09600008 ER PT J AU FLETCHER, DG AF FLETCHER, DG TI 2-PHOTON EXCITATION OF ATOMIC OXYGEN USING A RAMAN-SHIFTED ARF-EXCIMER LASER SO APPLIED PHYSICS B-LASERS AND OPTICS LA English DT Article ID INDUCED FLUORESCENCE; COMBUSTION DIAGNOSTICS; TEMPERATURE; FLAMES; O-2; NM; SPECTROSCOPY; ABSORPTION; EMISSION; RANGE AB A novel method for exciting the two-photon 2p3 3p 3P <-- 2p4 3P atomic oxygen transition is reported. The transition energy is provided by the combined photon energies of the second and third Stokes orders of a deuterium-filled Raman shifter pumped by an ArF-excimer laser. The ArF-excimer-pumped Raman shifter performance is characterized and the approach is demonstrated in an atomic oxygen population created by molecular oxygen absorption and predissociation in room air. RP FLETCHER, DG (reprint author), NASA,AMES RES CTR,MODELING & EXPTL VALIDAT BRANCH,MS 229-1,MOFFETT FIELD,CA 94035, USA. NR 24 TC 2 Z9 2 U1 0 U2 2 PU SPRINGER VERLAG PI NEW YORK PA 175 FIFTH AVE, NEW YORK, NY 10010 SN 0946-2171 J9 APPL PHYS B-LASERS O JI Appl. Phys. B-Lasers Opt. PD JAN PY 1995 VL 60 IS 1 BP 61 EP 65 DI 10.1007/BF01082074 PG 5 WC Optics; Physics, Applied SC Optics; Physics GA PZ096 UT WOS:A1995PZ09600010 ER PT B AU Noever, D Baskaran, S AF Noever, D Baskaran, S BE Pearson, DW Steele, NC Albrecht, RF TI Dominant takeover regimes for genetic algorithms SO ARTIFICIAL NEURAL NETS AND GENETIC ALGORITHMS LA English DT Proceedings Paper CT International Conference on Artificial Neural Nets and Genetic Algorithms CY 1995 CL ALES, FRANCE C1 NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,BIOPHYS BRANCH,HUNTSVILLE,AL 35812. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG PI VIENNA PA MOLKERBASTEI 5, POSTFACH 367, A-1011 VIENNA, AUSTRIA BN 3-211-82692-0 PY 1995 BP 223 EP 226 PG 4 WC Computer Science, Artificial Intelligence SC Computer Science GA BE73Z UT WOS:A1995BE73Z00058 ER PT S AU Pan, XP Kulkarni, S Shao, M Colavita, MM AF Pan, XP Kulkarni, S Shao, M Colavita, MM BE Hog, E Seidelmann, PK TI Narrow-angle and wide-angle astrometry via long baseline optical/infrared interferometers SO ASTRONOMICAL AND ASTROPHYSICAL OBJECTIVES OF SUB-MILLIARCSECOND OPTICAL ASTROMETRY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 166th Symposium of the International-Astronomical-Union on Astronomical and Astrophysical Objectives of Sub-Milliarcsecond Optical Astrometry CY AUG 15-19, 1994 CL THE HAGUE, NETHERLANDS SP Int Astron Union ID III STELLAR INTERFEROMETER; ORBIT AB Long baseline optical/infrared interferometers, such as the Mark III Stellar Interferometer(1) on Mt. Wilson and the ASEPS-0 Testbed Interferometer(2) on Palomar Mountain, California, have good capabilities for narrow-angle and wide-angle astrometry with very high precision. Using the Mark III Interferometer many spectroscopic binaries became ''visual'' for the first time. The measurement accuracy of angular separation is 0.2 mas, the smallest separation measured between two components is 2 mas, the maximum magnitude difference is 4 mag, and the smallest semimajor axis is 4 mas. Such high angular resolution and dynamic range have been used to determine stellar masses with precision of 2% and differential stellar luminosities to better than 0.05 mag for separations of less than 0.''2. For some binary stars, not only have the systems been resolved, but also the diameter of the primary component has been determined, yielding direct measurements of stellar effective temperature with high accuracy. For parallax determination, the precision is 1 mas or better and is unaffected by interstellar extinction. For wide-angle astrometry with the Mark III interferometer, the observation results yielded average formal 1 sigma errors for FK5 stars of about 10 mas. Presently a new infrared interferometer, the ASEPS-0 Testbed Interferometer on Palomar Mountain is under construction, and is being optimized to perform high accuracy narrow-angle astrometry using long baseline observations at 2.2 mu m, with phase referencing for increased sensitivity. The goal is to demonstrate differential astrometric accuracies of 0.06-0.1 mas(3) in order to allow for detection of extra-solar planets in the near future. C1 CALTECH, JET PROP LAB, PASADENA, CA 91109 USA. RP Pan, XP (reprint author), CALTECH, PASADENA, CA 91125 USA. NR 10 TC 1 Z9 1 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-3442-6 J9 IAU SYMP PY 1995 IS 166 BP 13 EP 18 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE11F UT WOS:A1995BE11F00003 ER PT S AU Standish, EM AF Standish, EM BE Hog, E Seidelmann, PK TI The dynamical reference frame SO ASTRONOMICAL AND ASTROPHYSICAL OBJECTIVES OF SUB-MILLIARCSECOND OPTICAL ASTROMETRY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 166th Symposium of the International-Astronomical-Union on Astronomical and Astrophysical Objectives of Sub-Milliarcsecond Optical Astrometry CY AUG 15-19, 1994 CL THE HAGUE, NETHERLANDS SP Int Astron Union AB Planetary and lunar ephemerides continue to improve in accuracy as they continue to be adjusted to newer and more accurate observational data. An additional improvement will be that of the orientation of the ephemerides; in the future, the ephemerides produced at JPL will be based upon the reference frame of the radio source catalogues. Recent planetary observations have been made directly with respect to the radio reference frame, and these observations have shown a satisfying degree of absolute accuracy and internal consistency; they enable the automatic orientation of the ephemerides onto the radio reference system during the ephemeris adjustment process. RP Standish, EM (reprint author), CALTECH, JET PROP LAB, 301-150, PASADENA, CA 91109 USA. NR 12 TC 0 Z9 0 U1 3 U2 3 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-3442-6 J9 IAU SYMP PY 1995 IS 166 BP 109 EP 116 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE11F UT WOS:A1995BE11F00018 ER PT S AU Lestrade, JF Jones, DL Preston, RA Phillips, RB Kovalevsky, J Froeschle, M Mignard, F AF Lestrade, JF Jones, DL Preston, RA Phillips, RB Kovalevsky, J Froeschle, M Mignard, F BE Hog, E Seidelmann, PK TI VLBI astrometry of radio-emitting stars SO ASTRONOMICAL AND ASTROPHYSICAL OBJECTIVES OF SUB-MILLIARCSECOND OPTICAL ASTROMETRY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 166th Symposium of the International-Astronomical-Union on Astronomical and Astrophysical Objectives of Sub-Milliarcsecond Optical Astrometry CY AUG 15-19, 1994 CL THE HAGUE, NETHERLANDS SP Int Astron Union ID ALGOL AB High-accuracy astrometric VLBI observations of 7 radio stars are presented with applications to the connection between the Hipparcos and VLBI extragalactic reference frames, to the identification of the radio emitting region in the ternary system Algol and the detectability of Jupitersize planet orbiting the radio star sigma(2) CrB. C1 CALTECH,JET PROP LAB,PASADENA,CA 91109. MIT,HAYSTACK OBSERV,WESTFORD,MA 01886. CTR ETUD & RECH GEODYNAM & ASTRON,F-06130 GRASSE,FRANCE. RP Lestrade, JF (reprint author), OBSERV PARIS,CNRS,URA 1757,ARPEGES,F-92195 MEUDON,FRANCE. NR 10 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-3442-6 J9 IAU SYMP PY 1995 IS 166 BP 119 EP 126 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE11F UT WOS:A1995BE11F00019 ER PT S AU Kaspi, VM AF Kaspi, VM BE Hog, E Seidelmann, PK TI High-precision timing of millisecond pulsars and precision astrometry SO ASTRONOMICAL AND ASTROPHYSICAL OBJECTIVES OF SUB-MILLIARCSECOND OPTICAL ASTROMETRY SE IAU SYMPOSIA LA English DT Article; Proceedings Paper CT 166th Symposium of the International-Astronomical-Union on Astronomical and Astrophysical Objectives of Sub-Milliarcsecond Optical Astrometry CY AUG 15-19, 1994 CL THE HAGUE, NETHERLANDS SP Int Astron Union ID BRIGHT AB We present the technique of long-term, high-precision timing of millisecond pulsars as applied to precision astrometry. We provide a tutorial on pulsars and pulsar timing, as well as up-to-date results of long-term timing observations of two millisecond pulsars, PSRs B1855+09 and B1937+21. We consider the feasibility of tying the extragalactic and optical reference frames to that defined by solar system objects, and we conclude that precision astrometry from millisecond pulsar timing has a bright future. RP Kaspi, VM (reprint author), CALTECH,JET PROP LAB,IPAC,770 SO WILSON AVE,PASADENA,CA 91125, USA. NR 11 TC 0 Z9 2 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0074-1809 BN 0-7923-3442-6 J9 IAU SYMP PY 1995 IS 166 BP 163 EP 171 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE11F UT WOS:A1995BE11F00025 ER PT B AU Riegler, G AF Riegler, G BE Shaw, RA Payne, HE Hayes, JJE TI The view from NASA headquarters: Trends and changes in mission operations and data analysis programs SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS IV SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Annual Conference on Astronomical Data Analysis Software and Systems (ADASS IV) CY SEP 25-28, 1994 CL BALTIMORE, MD SP Space Telescope Sci Inst, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Natl Radio Astron Observ, NASA, Natl Res Council Canada, Natl Sci Fdn, Hughes STX, Sun Microsyst Inc, Resource One, Sybase Inc, Silicon Graph Inc, Open Concepts Inc, Res Syst Inc, Digital Equipment Corp C1 NASA HEADQUARTERS,DIV ASTROPHYS,WASHINGTON,DC 20546. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-96-1 J9 ASTR SOC P PY 1995 VL 77 BP 8 EP 11 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Y UT WOS:A1995BE33Y00002 ER PT B AU Richmond, A Duesterhaus, M Yom, S Schlegel, E Smale, A White, NE AF Richmond, A Duesterhaus, M Yom, S Schlegel, E Smale, A White, NE BE Shaw, RA Payne, HE Hayes, JJE TI Design of a remote proposal submission system SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS IV SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Annual Conference on Astronomical Data Analysis Software and Systems (ADASS IV) CY SEP 25-28, 1994 CL BALTIMORE, MD SP Space Telescope Sci Inst, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Natl Radio Astron Observ, NASA, Natl Res Council Canada, Natl Sci Fdn, Hughes STX, Sun Microsyst Inc, Resource One, Sybase Inc, Silicon Graph Inc, Open Concepts Inc, Res Syst Inc, Digital Equipment Corp C1 NASA,GODDARD SPACE FLIGHT CTR,HUGHES STX,GREENBELT,MD 20771. RI White, Nicholas/B-6428-2012 OI White, Nicholas/0000-0003-3853-3462 NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-96-1 J9 ASTR SOC P PY 1995 VL 77 BP 62 EP 64 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Y UT WOS:A1995BE33Y00014 ER PT B AU Jordan, JM CresitelloDittmar, M Allen, JS AF Jordan, JM CresitelloDittmar, M Allen, JS BE Shaw, RA Payne, HE Hayes, JJE TI Exploring interactive archive data presentation at the COSSC SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS IV SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Annual Conference on Astronomical Data Analysis Software and Systems (ADASS IV) CY SEP 25-28, 1994 CL BALTIMORE, MD SP Space Telescope Sci Inst, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Natl Radio Astron Observ, NASA, Natl Res Council Canada, Natl Sci Fdn, Hughes STX, Sun Microsyst Inc, Resource One, Sybase Inc, Silicon Graph Inc, Open Concepts Inc, Res Syst Inc, Digital Equipment Corp C1 NASA,GODDARD SPACE FLIGHT CTR,HUGHES STX,COSSC,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-96-1 J9 ASTR SOC P PY 1995 VL 77 BP 176 EP 178 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Y UT WOS:A1995BE33Y00040 ER PT B AU Corcoran, MF Angelini, L George, I McGlynn, T Mukai, K Pence, W Rots, A AF Corcoran, MF Angelini, L George, I McGlynn, T Mukai, K Pence, W Rots, A BE Shaw, RA Payne, HE Hayes, JJE TI The OGIP FITS working group SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS IV SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Annual Conference on Astronomical Data Analysis Software and Systems (ADASS IV) CY SEP 25-28, 1994 CL BALTIMORE, MD SP Space Telescope Sci Inst, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Natl Radio Astron Observ, NASA, Natl Res Council Canada, Natl Sci Fdn, Hughes STX, Sun Microsyst Inc, Resource One, Sybase Inc, Silicon Graph Inc, Open Concepts Inc, Res Syst Inc, Digital Equipment Corp C1 NASA,GODDARD SPACE FLIGHT CTR,OFF GUEST INVESTIGATOR PROGRAMS,GREENBELT,MD 20771. NR 0 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-96-1 J9 ASTR SOC P PY 1995 VL 77 BP 219 EP 220 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Y UT WOS:A1995BE33Y00051 ER PT B AU Jennings, DG Pence, WD Folk, M AF Jennings, DG Pence, WD Folk, M BE Shaw, RA Payne, HE Hayes, JJE TI Convert: Bridging the scientific data format chasm SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS IV SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Annual Conference on Astronomical Data Analysis Software and Systems (ADASS IV) CY SEP 25-28, 1994 CL BALTIMORE, MD SP Space Telescope Sci Inst, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Natl Radio Astron Observ, NASA, Natl Res Council Canada, Natl Sci Fdn, Hughes STX, Sun Microsyst Inc, Resource One, Sybase Inc, Silicon Graph Inc, Open Concepts Inc, Res Syst Inc, Digital Equipment Corp C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NR 0 TC 4 Z9 4 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-96-1 J9 ASTR SOC P PY 1995 VL 77 BP 229 EP 232 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Y UT WOS:A1995BE33Y00054 ER PT B AU Pence, WD AF Pence, WD BE Shaw, RA Payne, HE Hayes, JJE TI FITSIO Subroutine Library update SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS IV SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Annual Conference on Astronomical Data Analysis Software and Systems (ADASS IV) CY SEP 25-28, 1994 CL BALTIMORE, MD SP Space Telescope Sci Inst, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Natl Radio Astron Observ, NASA, Natl Res Council Canada, Natl Sci Fdn, Hughes STX, Sun Microsyst Inc, Resource One, Sybase Inc, Silicon Graph Inc, Open Concepts Inc, Res Syst Inc, Digital Equipment Corp C1 NASA,GODDARD SPACE FLIGHT CTR,HEASARC,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-96-1 J9 ASTR SOC P PY 1995 VL 77 BP 245 EP 246 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Y UT WOS:A1995BE33Y00058 ER PT B AU Blackburn, JK AF Blackburn, JK BE Shaw, RA Payne, HE Hayes, JJE TI FTOOLS: A FITS data processing and analysis software package SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS IV SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Annual Conference on Astronomical Data Analysis Software and Systems (ADASS IV) CY SEP 25-28, 1994 CL BALTIMORE, MD SP Space Telescope Sci Inst, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Natl Radio Astron Observ, NASA, Natl Res Council Canada, Natl Sci Fdn, Hughes STX, Sun Microsyst Inc, Resource One, Sybase Inc, Silicon Graph Inc, Open Concepts Inc, Res Syst Inc, Digital Equipment Corp C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NR 0 TC 121 Z9 121 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-96-1 J9 ASTR SOC P PY 1995 VL 77 BP 367 EP 370 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Y UT WOS:A1995BE33Y00085 ER PT B AU Landsman, WB AF Landsman, WB BE Shaw, RA Payne, HE Hayes, JJE TI The IDL Astronomy User's Library SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS IV SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Annual Conference on Astronomical Data Analysis Software and Systems (ADASS IV) CY SEP 25-28, 1994 CL BALTIMORE, MD SP Space Telescope Sci Inst, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Natl Radio Astron Observ, NASA, Natl Res Council Canada, Natl Sci Fdn, Hughes STX, Sun Microsyst Inc, Resource One, Sybase Inc, Silicon Graph Inc, Open Concepts Inc, Res Syst Inc, Digital Equipment Corp C1 NASA,GODDARD SPACE FLIGHT CTR,HUGHES STX CO,GREENBELT,MD 20771. NR 0 TC 21 Z9 21 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-96-1 J9 ASTR SOC P PY 1995 VL 77 BP 437 EP 440 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Y UT WOS:A1995BE33Y00103 ER PT B AU Ake, TB AF Ake, TB BE Shaw, RA Payne, HE Hayes, JJE TI Calculating the position and velocity components of HST SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS IV SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Annual Conference on Astronomical Data Analysis Software and Systems (ADASS IV) CY SEP 25-28, 1994 CL BALTIMORE, MD SP Space Telescope Sci Inst, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Natl Radio Astron Observ, NASA, Natl Res Council Canada, Natl Sci Fdn, Hughes STX, Sun Microsyst Inc, Resource One, Sybase Inc, Silicon Graph Inc, Open Concepts Inc, Res Syst Inc, Digital Equipment Corp C1 COMP SCI CORP,GODDARD SPACE FLIGHT CTR,ASTRON PROGRAMS,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-96-1 J9 ASTR SOC P PY 1995 VL 77 BP 464 EP 467 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Y UT WOS:A1995BE33Y00108 ER PT B AU Barrett, P AF Barrett, P BE Shaw, RA Payne, HE Hayes, JJE TI Application of the linear quadtree to astronomical databases SO ASTRONOMICAL DATA ANALYSIS SOFTWARE AND SYSTEMS IV SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Annual Conference on Astronomical Data Analysis Software and Systems (ADASS IV) CY SEP 25-28, 1994 CL BALTIMORE, MD SP Space Telescope Sci Inst, Natl Opt Astron Observ, Smithsonian Astrophys Observ, Natl Radio Astron Observ, NASA, Natl Res Council Canada, Natl Sci Fdn, Hughes STX, Sun Microsyst Inc, Resource One, Sybase Inc, Silicon Graph Inc, Open Concepts Inc, Res Syst Inc, Digital Equipment Corp C1 NASA,GODDARD SPACE FLIGHT CTR,UNIV SPACE RES ASSOC,GREENBELT,MD 20771. NR 0 TC 3 Z9 3 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-96-1 J9 ASTR SOC P PY 1995 VL 77 BP 472 EP 475 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Y UT WOS:A1995BE33Y00110 ER PT J AU ULVESTAD, JS ANTONUCCI, RRJ GOODRICH, RW AF ULVESTAD, JS ANTONUCCI, RRJ GOODRICH, RW TI RADIO PROPERTIES OF NARROW-LINED SEYFERT-1 GALAXIES SO ASTRONOMICAL JOURNAL LA English DT Article ID ACTIVE GALACTIC NUCLEI; OPTICAL POSITIONS; LIMITED SAMPLE; SPECTROPOLARIMETRY; POLARIZATION; EMISSION; NGC-1068; SPECTRUM; NGC-4151 C1 UNIV CALIF SANTA BARBARA,DEPT PHYS,SANTA BARBARA,CA 93106. UNIV CALIF SANTA CRUZ,LICK OBSERV,SANTA CRUZ,CA 95064. RP ULVESTAD, JS (reprint author), JET PROP LAB,MAIL STOP 301-125J,PASADENA,CA 91109, USA. OI Ulvestad, James/0000-0002-9362-7237 NR 44 TC 67 Z9 69 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 JAN PY 1995 VL 109 IS 1 BP 81 EP 86 DI 10.1086/117258 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA PZ937 UT WOS:A1995PZ93700008 ER PT J AU CHARLOT, P SOVERS, OJ WILLIAMS, JG NEWHALL, XX AF CHARLOT, P SOVERS, OJ WILLIAMS, JG NEWHALL, XX TI PRECESSION AND NUTATION FROM JOINT ANALYSIS OF RADIO INTERFEROMETRIC AND LUNAR LASER RANGING OBSERVATIONS SO ASTRONOMICAL JOURNAL LA English DT Article ID INNER CORE DYNAMICS; FORCED NUTATIONS; RIGID-EARTH; NUMERICAL DETERMINATION; CONSTANTS; ROTATION; GEODESY; SYSTEM; MODEL; SOLAR C1 OBSERV PARIS,CENT BUR IERS,CNRS,URA 1125,F-75014 PARIS,FRANCE. JET PROP LAB,PASADENA,CA 91109. RP CHARLOT, P (reprint author), JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 36 TC 29 Z9 29 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 JAN PY 1995 VL 109 IS 1 BP 418 EP 427 DI 10.1086/117286 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA PZ937 UT WOS:A1995PZ93700036 ER PT J AU SAHAI, R LIECHTI, S AF SAHAI, R LIECHTI, S TI CIRCUMSTELLAR CO EMISSION IN S-STARS .1. MASS-LOSS WITH LITTLE OR NO DUST SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE STARS, MASS-LOSS; STARS, AGB AND POST-AGB; CIRCUMSTELLAR MATTER; STARS, LATE-TYPE; RADIO LINES, MOLECULAR LINE, PROFILES ID LOSS RATES; CARBON STARS; RED GIANTS; ENVELOPES; TECHNETIUM; EVOLUTION AB 47 S stars have been searched for circumstellar CO (J=1-0 and/or 2-1) emission, and 29 have been detected, including 4 which show no evidence of dust in their IRAS LRS spectra, and one with possibly no Tc (and therefore not an AGE star). Six stars show anomalous features in their profiles, showing the presence of more than one kinematic component in the expanding outflow. Two stars may have detached-shell envelopes. The expansion velocity distribution for S stars envelopes is different than that for C-rich stars, with the former having a slightly lower mean expansion velocity, and a significantly higher fraction of objects with very low expansion velocities (less than or similar to 5.5 km s(-1)). In most S stars, the mass-loss rates are > 2 x 10(-7) Mo yr(-1) and the gas-to-dust ratios are > 1000. Our detection of CO in S stars with little or no detectable dust implies substantial mass-loss in these objects. The expansion velocities and mass-loss rates of the relatively dust-free stars show a much steeper dependence on the the far-infrared excess (Delta IR(e)), as compared to the more dusty stars. This suggests that when the amount of dust becomes small, mass-loss may be partially driven by a different mechanism than radiation pressure on grains, which probably dominates in the dusty envelopes. C1 CHALMERS UNIV TECHNOL, S-41296 GOTHENBURG, SWEDEN. GOTHENBURG UNIV, S-41296 GOTHENBURG, SWEDEN. NATL ACAD SCI, NATL RES COUNCIL, WASHINGTON, DC 20418 USA. CTR ASTRON YEBES, E-19080 GUADALAJARA, SPAIN. RP SAHAI, R (reprint author), CALTECH, JET PROP LAB, MS169-506, 4800 OAK GROVE DR, PASADENA, CA 91109 USA. NR 24 TC 30 Z9 30 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 JAN PY 1995 VL 293 IS 1 BP 198 EP 207 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA PZ830 UT WOS:A1995PZ83000030 ER PT J AU ALLOIN, D SANTOSLLEO, M PETERSON, BM WAMSTEKER, W ALTIERI, B BRINKMANN, W CLAVEL, J CRENSHAW, DM GEORGE, IM GLASS, IS JOHNSON, WN KRISS, GA MALKAN, MA POLIDAN, RS REICHERT, GA RODRIGUEZPASCUAL, PM ROMANISHIN, W STARR, CH STIRPE, GM TAYLOR, M TURNER, TJ VEGA, H WINGE, C WOOD, DOS AF ALLOIN, D SANTOSLLEO, M PETERSON, BM WAMSTEKER, W ALTIERI, B BRINKMANN, W CLAVEL, J CRENSHAW, DM GEORGE, IM GLASS, IS JOHNSON, WN KRISS, GA MALKAN, MA POLIDAN, RS REICHERT, GA RODRIGUEZPASCUAL, PM ROMANISHIN, W STARR, CH STIRPE, GM TAYLOR, M TURNER, TJ VEGA, H WINGE, C WOOD, DOS TI A SNAPSHOT OF THE CONTINUOUS EMISSION OF THE ACTIVE GALACTIC NUCLEUS IN NGC-3783 FROM GAMMA-RAY TO RADIO WAVELENGTHS SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE GALAXIES, SEYFERT; GALAXIES, INDIVIDUAL, NGC 3783; GALAXIES, NUCLEI; RADIATION MECHANISMS, NONTHERMAL; RADIATION MECHANISMS, THERMAL; BLACK HOLE PHYSICS ID BROAD-LINE REGION; FAR-ULTRAVIOLET SPECTROPHOTOMETRY; SEYFERT-GALAXY NGC-3783; SPECTROMETER EXPERIMENT; OPTICAL WAVELENGTHS; DISK MODELS; FE-II; VARIABILITY; NGC-5548; SPECTRA AB With the aim of better understanding the physical processes that produce the continuous emission in active galactic nuclei (AGNs), a snapshot of the overall continuous energy distribution of NGC 3783, from gamma-ray to radio wavelengths, has been obtained within the framework of the World Astronomy Days. The data collected in this campaign are from GRO, ROSAT, Voyager 2, IUE, HST, ESO, CTIO, SAAO and the VLA. Great care has been taken in disentangling the genuine AGN continuous emission from other contributions: depending on the waveband, the latter might be (i) unrelated contaminating sources in cases where the instrument field of view is large, (ii) components within which the AGN is embedded, such as the stellar bulge population which accounts for a significant fraction of the optical continuum, and free-bound and FeII blends which contribute to the ultraviolet flux. After correction for these other contributions, the continuous emission of the isolated AGN appears to be rather flat (i.e., approximately equal energy per unit logarithmic frequency) from soft gamma-ray to infrared wavelengths. At high energies (0.1 MeV to 0.1 keV), the AGN continuum can be fitted by a power law F-upsilon proportional to upsilon(-alpha) with a spectral index alpha approximate to 1. At longer wavelengths, two excesses above this power law (''bumps'') appear: in the ultraviolet, the classical big blue bump, which can be interpreted as thermal emission from the accretion disc surrounding a massive black hole, and in the infrared a second bump which can be ascribed to thermal emission from dust in the vicinity of the AGN, heated by ultraviolet radiation from the central source. By fitting accretion-disc models to the observed AGN spectral energy distribution, we find values for the accretion disc innermost temperature, accretion rate, and black hole mass, with some differences that depend on whether or not we extrapolate the high-energy power law up to infrared wavelengths. A fit to the LR bump above the extended alpha = 1 power law suggests the presence of a dust component covering the region from a distance r approximate to 80 light days (hot grains at a temperature T approximate to 1500 K) to r approximate to 60 light years (cool grains at T approximate to 200 K). The total mass of dust is around 60 M(.). C1 OHIO STATE UNIV, DEPT ASTRON, COLUMBUS, OH 43210 USA. ESA, IUE OBSERV, E-28080 MADRID, SPAIN. EUROPEAN SPACE AGCY, ESTEC, ISO OBSERV, DIV ASTROPHYS, 2200 AG NOORDWIJK, NETHERLANDS. MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. NASA, GODDARD SPACE FLIGHT CTR, COMP SCI CORP, SCI PROGRAM, GREENBELT, MD 20771 USA. NASA, GODDARD SPACE FLIGHT CTR, HIGH ENERGY ASTROPHYS LAB, GREENBELT, MD 20771 USA. NASA, GODDARD SPACE FLIGHT CTR, UNIV SPACE RES ASSOC, GREENBELT, MD 20771 USA. S AFRICAN ASTRON OBSERV, CAPE TOWN 7935, SOUTH AFRICA. USN, RES LAB, EO HULBURT CTR SPACE RES, WASHINGTON, DC 20375 USA. JOHNS HOPKINS UNIV, DEPT PHYS & ASTRON, BALTIMORE, MD 21218 USA. UNIV CALIF LOS ANGELES, DEPT ASTRON, LOS ANGELES, CA 90024 USA. NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, GREENBELT, MD 20771 USA. UNIV OKLAHOMA, DEPT PHYS & ASTRON, NORMAN, OK 73019 USA. NASA, GODDARD SPACE FLIGHT CTR, CGRO SCI SUPPORT CTR, GREENBELT, MD 20771 USA. OSSERV ASTRON BOLOGNA, I-40126 BOLOGNA, ITALY. CATHOLIC UNIV AMER, WASHINGTON, DC 20064 USA. EUROPEAN SO OBSERV, SANTIAGO 19, CHILE. UNIV FED RIO GRANDE SUL, INST FIS, DEPT ASTRON, BR-91500 PORTO ALEGRE, RS, BRAZIL. NATL RADIO ASTRON OBSERV, SOCORRO, NM 87801 USA. RP ALLOIN, D (reprint author), OBSERV PARIS, CNRS, URA 173, F-92195 MEUDON, FRANCE. RI Johnson, Neil/G-3309-2014; Stirpe, Giovanna/O-9393-2015 OI Stirpe, Giovanna/0000-0002-3702-8731 NR 70 TC 33 Z9 33 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 JAN PY 1995 VL 293 IS 2 BP 293 EP 308 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QB723 UT WOS:A1995QB72300006 ER PT J AU BLOEMEN, H BENNETT, K BLOOM, JJ COLLMAR, W HERMSEN, W LICHTI, GG MORRIS, D SCHONFELDER, V STACY, JG STRONG, AW WINKLER, C AF BLOEMEN, H BENNETT, K BLOOM, JJ COLLMAR, W HERMSEN, W LICHTI, GG MORRIS, D SCHONFELDER, V STACY, JG STRONG, AW WINKLER, C TI NEW COMPTEL GAMMA-RAY SOURCE (GRO-J0516-609) NEAR PKS-0506-612/0522-611 - FIRST EVIDENCE FOR MEV BLAZARS SO ASTRONOMY & ASTROPHYSICS LA English DT Letter DE GAMMA RAYS, OBSERVATIONS; GALAXIES, ACTIVE; QUASARS, PKS 0506-612 AND PKS 0522-611 ID EMISSION AB We report evidence for a blazar-type AGN that is exceptionally bright at MeV energies. It is firmly detected by COMPTEL in the 1-10 MeV range, but we find only a weak similar to 3 sigma source in the EGRET archival data (>100 MeV), which is confirmed by the EGRET team. The source is now listed as one of the marginal detections in the latest EGRET catalogue, being the weakest source in the whole list. It is located about 10 degrees from the LMC at l approximate to 270 degrees, b approximate to: -35 degrees. Within the 99% error region of this new COMPTEL source (GRO J0516-609), two potential AGN counterparts can be identified. These are PKS 0506-612 and PKS 0522-611, separated by similar to 20, which are both compact, radio loud, flat-spectrum radio sources, like all AGNs detected at high-energy gamma-rays. The former is the preferred counterpart by the weak EGRET detection, which has a smaller error region. The source was in the COMPTEL field-of-view on three occasions during its Phase I sky survey, but it was detected only in the second and third observation. This suggests a flux increase by a factor of about two in the two-month period between the first and second viewing. Evidence for the weak EGRET source is also only found in the second and third observation. The radiated power per decade of energy (vF(v)) strongly peaks at similar to 3 MeV. If GRO J0516-609 is indeed a blazar, it can probably be ruled out that the MeV gamma-rays are mainly due to Comptonization of an external radiation field. ''MeV blazars'' like GRO J0516-609 may be responsible for the observed MeV bump in the cosmic background spectrum. C1 MAX PLANCK INST EXTRATERR PHYS, D-85740 GARCHING, GERMANY. UNIV NEW HAMPSHIRE, CTR SPACE SCI, DURHAM, NH 03824 USA. EUROPEAN SPACE TECHNOL CTR, EUROPEAN SPACE AGCY, DIV ASTROPHYS, 2200 AG NOORDWIJK, NETHERLANDS. LEIDEN OBSERV, 2300 RA LEIDEN, NETHERLANDS. NASA, GSFC, COMPTON OBSERV SCI SUPPORT CTR, GREENBELT, MD USA. RP BLOEMEN, H (reprint author), SRON, SORBONNELAAN 2, 3584 CA UTRECHT, NETHERLANDS. NR 23 TC 47 Z9 47 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 JAN PY 1995 VL 293 IS 1 BP L1 EP L4 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA PZ830 UT WOS:A1995PZ83000001 ER PT J AU GOTTWALD, M PARMAR, AN REYNOLDS, AP WHITE, NE PEACOCK, A TAYLOR, BG AF GOTTWALD, M PARMAR, AN REYNOLDS, AP WHITE, NE PEACOCK, A TAYLOR, BG TI THE EXOSAT GSPC IRON LINE CATALOG SO ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES LA English DT Article DE CATALOGS; X-RAYS ID X-RAY BINARIES; SCORPIUS X-1; K LINE; CIRCUMSTELLAR MATTER; TENMA OBSERVATIONS; EMISSION LINES; VELA X-1; SPECTRA; VARIABILITY; SATELLITE AB We report on the global properties of the Fe features seen in the 6 - 7 keV spectra of X-ray sources observed with the EXOSAT Gas Scintillation Proportional Counter (GSPC). Of a total of 431 spectra extracted from the EXOSAT archive, 205 required the addition of a Gaussian emission line to the continuum spectrum in order to obtain satisfactory fits. The majority of these sources are X-ray binaries. The best fit line properties are given for each of these spectra as well as being summarized by source class. For the 226 spectra which did not require the addition of an emission feature, upper limit equivalent widths for narrow and broad lines are presented. C1 ESTEC,ESA,DEPT SPACE SCI,DIV ASTROPHYS,2200 AG NOORDWIJK,NETHERLANDS. DEUTSCH FORSCHUNGSANSTALT LUFT & RAUMFAHRT,GERMAN REMOTE SENSING DATA CTR,D-82234 OBERPFAFFENHOFEN,GERMANY. NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. RI White, Nicholas/B-6428-2012 OI White, Nicholas/0000-0003-3853-3462 NR 53 TC 26 Z9 26 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 JAN PY 1995 VL 109 IS 1 BP 9 EP 28 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA342 UT WOS:A1995QA34200002 ER PT J AU CLARK, TA BOSWORTH, J VANDENBERG, N GORDON, D HIMWICH, E SHAFFER, D WITHNEY, A COREY, B NIEL, A TOMAS, C MATVEENKO, LI MUSIN, RK SHEVCHENKO, AV NESTEROV, NS STEPANOV, AV NIKITIN, PS IPATOV, AV MARDYSHKIN, VV IVANOV, DA YATSKIV, YS MEDVEDSKII, MM AF CLARK, TA BOSWORTH, J VANDENBERG, N GORDON, D HIMWICH, E SHAFFER, D WITHNEY, A COREY, B NIEL, A TOMAS, C MATVEENKO, LI MUSIN, RK SHEVCHENKO, AV NESTEROV, NS STEPANOV, AV NIKITIN, PS IPATOV, AV MARDYSHKIN, VV IVANOV, DA YATSKIV, YS MEDVEDSKII, MM TI PRECISION-MEASUREMENTS OF THE LOCATION OF THE VLBI STATION SIMEIZ SO ASTRONOMY LETTERS-A JOURNAL OF ASTRONOMY AND SPACE ASTROPHYSICS LA English DT Article C1 NEROC,HAYSTACK RADIO OBSERV,WESTFORD,MA 01886. RUSSIAN ACAD SCI,INST SPACE RES,MOSCOW 117810,RUSSIA. UKRAINIAN STATE COMM SCI & TECHNOL,CRIMEAN ASTROPHYS OBSERV,NAUCHNYI 334413,UKRAINE. INST APPL ASTRON,ST PETERSBURG,RUSSIA. UKRAINIAN ACAD SCI,MAIN ASTRON OBSERV,KIEV 252127,UKRAINE. RP CLARK, TA (reprint author), NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771, USA. NR 5 TC 1 Z9 1 U1 0 U2 1 PU AMER INST PHYSICS PI WOODBURY PA CIRCULATION FULFILLMENT DIV, 500 SUNNYSIDE BLVD, WOODBURY, NY 11797-2999 SN 1063-7737 J9 ASTRON LETT+ JI Astron. Lett.-J. Astron. Space Astrophys. PD JAN-FEB PY 1995 VL 21 IS 1 BP 116 EP 117 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QL590 UT WOS:A1995QL59000015 ER PT B AU Lanz, T AF Lanz, T BE Adelman, SJ Wiese, WL TI The atmospheres of chemically peculiar stars: A laboratory for atomic physics SO ASTROPHYSICAL APPLICATIONS OF POWERFUL NEW DATABASES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Joint Discussion Number 16 of the 22nd General Assembly of the IAU - Astrophysical Applications of Powerful New Databases CY AUG 22-23, 1994 CL THE HAGUE, NETHERLANDS SP Int Astron Union C1 NASA,GODDARD SPACE FLIGHT CTR,UNIV SPACE RES ASSOC,GREENBELT,MD 20771. NR 0 TC 2 Z9 2 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-97-X J9 ASTR SOC P PY 1995 VL 78 BP 423 EP 437 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Z UT WOS:A1995BE33Z00046 ER PT B AU Rubin, RH Kunze, D Yamamoto, T AF Rubin, RH Kunze, D Yamamoto, T BE Adelman, SJ Wiese, WL TI What nebular observations and photoionization models can tell us about atmospheres of hot stars SO ASTROPHYSICAL APPLICATIONS OF POWERFUL NEW DATABASES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Joint Discussion Number 16 of the 22nd General Assembly of the IAU - Astrophysical Applications of Powerful New Databases CY AUG 22-23, 1994 CL THE HAGUE, NETHERLANDS SP Int Astron Union C1 NASA,AMES RES CTR,MOFFETT FIELD,CA 94035. NR 0 TC 11 Z9 11 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 0-937707-97-X J9 ASTR SOC P PY 1995 VL 78 BP 479 EP 507 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BE33Z UT WOS:A1995BE33Z00053 ER PT J AU COURVOISIER, TJL BLECHA, A BOUCHET, P BRATSCHI, P CARINI, MT DONAHUE, M EDELSON, R FEIGELSON, ED FILIPPENKO, AV GLASS, IS HEIDT, J KOLLGAARD, RI MATHESON, T MILLER, HR NOBLE, JC SEKIGUCHI, K SMITH, PS URRAY, CM WAGNER, SJ AF COURVOISIER, TJL BLECHA, A BOUCHET, P BRATSCHI, P CARINI, MT DONAHUE, M EDELSON, R FEIGELSON, ED FILIPPENKO, AV GLASS, IS HEIDT, J KOLLGAARD, RI MATHESON, T MILLER, HR NOBLE, JC SEKIGUCHI, K SMITH, PS URRAY, CM WAGNER, SJ TI MULTIWAVELENGTH MONITORING OF THE BL LACERTAE OBJECT PKS 2155-304 .3. GROUND-BASED OBSERVATIONS IN 1991 NOVEMBER SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL LAC OBJECTS, INDIVIDUAL (PKS 2155-304); GALAXIES, PHOTOMETRY; POLARIZATION; ULTRAVIOLET, GALAXIES; X-RAYS, GALAXIES ID ABSOLUTE CALIBRATION; OPTICAL VARIABILITY; UBVRI PHOTOMETRY; POLARIMETRY; PKS-2155-304; SPECTRUM; SYSTEM; FIELDS; MODELS; STARS AB We present ground-based observations of the BL Lac object PKS 2155-304 during 1991 November. These data were obtained as part of a large international campaign of observations spanning the electro-magnetic spectrum from the radio waves to the X-rays. The data presented here include radio, and UBVRI fluxes, as well as optical polarimetry. The U to I data show the same behavior in all bands and that only upper limits to any lag can be deduced from the cross-correlation of the light curves. The spectral slope in the U-I domain remained constant on all epochs but 2. There is no correlation between changes in the spectral slope and large variations in the total or polarized flux. The radio flux variations did not follow the same pattern of variability as the optical and infrared fluxes. The polarized flux varied by a larger factor than the total flux. The variations of the polarized flux are poorly correlated with those of the total flux in the optical (and hence UV domain; see the accompanying paper by Edelson et al.) nor with those of the soft X-rays. We conclude that the variability of PKS 2155-304 in the optical and near-infrared spectral domains are easier to understand in the context of a variable geometry or bulk Lorentz factor than of variable electron acceleration and cooling rates. C1 EUROPEAN SO OBSERV,SANTIAGO 19,CHILE. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. UNIV IOWA,DEPT PHYS & ASTRON,IOWA CITY,IA 52242. PENN STATE UNIV,DEPT ASTRON & ASTROPHYS,UNIVERSITY PK,PA 16802. UNIV CALIF BERKELEY,DEPT ASTRON,BERKELEY,CA 94720. LANDESSTERNWARTE HEIDELBERG KONIGSTUHL,D-69117 HEIDELBERG,GERMANY. GEORGIA STATE UNIV,DEPT PHYS,ATLANTA,GA 30303. UNIV ARIZONA,STEWARD OBSERV,TUCSON,AZ 85721. NASA,GODDARD SPACE FLIGHT CTR,COMP SCI CORP,GREENBELT,MD 20771. S AFRICA ASTRON OBSERV,OBSER 7935,SOUTH AFRICA. RP COURVOISIER, TJL (reprint author), GENEVA OBSERV,CH-1290 SAUVERNY,SWITZERLAND. RI Donahue, Megan/B-5361-2012 NR 33 TC 35 Z9 35 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 JAN 1 PY 1995 VL 438 IS 1 BP 108 EP 119 DI 10.1086/175058 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA055 UT WOS:A1995QA05500010 ER PT J AU EDELSON, R KROLIK, J MADEJSKI, G MARASCHI, L PIKE, G URRY, CM BRINKMANN, W COURVOISIER, TJL ELLITHORPE, J HORNE, K TREVES, A WAGNER, S WAMSTEKER, W WARWICK, R ALLER, HD ALLER, MF ASHLEY, M BLECHA, A BOUCHET, P BRATSCHI, P BREGMAN, JN CARINI, M CELOTTI, A DONAHUE, M FEIGELSON, E FILIPPENKO, AV FINK, H GEORGE, I GLASS, I HEIDT, J HEWITT, J HUGHES, P KOLLGAARD, R KONDO, Y KORATKAR, A LEIGHLY, K MARSCHER, A MARTIN, PG MATHESON, T MILLER, HR KNOBLE, JC OBRIEN, P PIAN, E REICHERT, G SAKEN, JM SHULL, JM SITKO, M SMITH, PS SUN, WH TAGLIAFERRI, G AF EDELSON, R KROLIK, J MADEJSKI, G MARASCHI, L PIKE, G URRY, CM BRINKMANN, W COURVOISIER, TJL ELLITHORPE, J HORNE, K TREVES, A WAGNER, S WAMSTEKER, W WARWICK, R ALLER, HD ALLER, MF ASHLEY, M BLECHA, A BOUCHET, P BRATSCHI, P BREGMAN, JN CARINI, M CELOTTI, A DONAHUE, M FEIGELSON, E FILIPPENKO, AV FINK, H GEORGE, I GLASS, I HEIDT, J HEWITT, J HUGHES, P KOLLGAARD, R KONDO, Y KORATKAR, A LEIGHLY, K MARSCHER, A MARTIN, PG MATHESON, T MILLER, HR KNOBLE, JC OBRIEN, P PIAN, E REICHERT, G SAKEN, JM SHULL, JM SITKO, M SMITH, PS SUN, WH TAGLIAFERRI, G TI MULTIWAVELENGTH MONITORING OF THE BL LACERTAE OBJECT PKS 2155-304 .4. MULTIWAVELENGTH ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL LACERTAE OBJECT, INDIVIDUAL (PKS 2155-304); GALAXIES, ACTIVE; INFRARED, GALAXIES; RADIO CONTINUUM, GALAXIES; ULTRAVIOLET, GALAXIES; X-RAYS, GALAXIES ID ACTIVE GALACTIC NUCLEI; X-RAY VARIABILITY; ULTRAVIOLET VARIABILITY; RELATIVISTIC JETS; POWER SPECTRUM; LAC OBJECTS; PKS-2155-304; RADIO; EMISSION; MODELS AB Simultaneous X-ray, ultraviolet, optical, infrared, and radio monitoring data were used to test and constrain models of continuum emission from the BL Lacertae object PKS 2155-304. Intensively sampled ultraviolet and soft X-ray light curves showed a clear temporal correlation, with the X-rays leading the ultraviolet by 2-3 hr. This lag was found to be significantly different from zero after an exhaustive comparison of four different techniques for measuring temporal correlations. Variations in the ultraviolet through optical wave bands were also all strongly correlated, with no measurable lag down to limiting timescales of less-than-or-similar-to 1-2 hr. This strong correlation extends to the near-infrared, but the less intensive sampling precludes measurement of any lag beyond an upper limit of less-than-or-similar-to 1 day. These lags and limits of the order of hours are much shorter than the most rapid observed single-band variations. Because of the very sparse radio sampling, it was not possible to measure quantitatively the correlation and lag with shorter wavelengths, but the data do suggest that the radio may lag the optical/ultraviolet by approximately 1 week, with longer delays and weaker variations to longer radio wavelengths. The epoch-folding Q2 statistic was used to test for periodicity, and no evidence for strict or quasi-periodicity was found in any of the light curves. Because they lead the lower frequencies, the soft X-rays (less-than-or-similar-to 1 keV) cannot arise from synchrotron self-Compton scattering. These results also rule out the accretion disk model, which predicts a measurable lag between ultraviolet/optical wavelength bands and a correlation between hardness and brightness, neither of which were seen. They are consistent with the entire radio through X-ray continuum arising from direct synchrotron emission from a relativistic jet. However, the tapered jet model, in which the X-ray emission is prochrotron emission from a relativistic jet. However, the tapered jet model, in which the X-ray emission is produced closer in, has problems explaining the magnitude of the ultraviolet/X-ray lag, because the X-ray-emitting electrons have very short lifetimes (t1/2 much-less-than 1 s). The result that the lag is much smaller than the variability timescale suggests instead that the radiation may be produced in a flattened region such as a shock front. C1 UNIV IOWA,DEPT PHYS & ASTRON,IOWA CITY,IA 52242. JOHNS HOPKINS UNIV,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. UNIV MILAN,DEPT PHYS,I-20133 MILAN,ITALY. SPACE TELESCOPE SCI INST,BALTIMORE,MD 21218. MAX PLANCK INST EXTRATERR PHYS,GIESSENBACHSTR,W-8046 GARCHING,GERMANY. OBSERVE GENEVE,CH-1290 SAUVERNY,SWITZERLAND. MIT,DEPT PHYS,CAMBRIDGE,MA 02139. STERREKUNDIG INST UTRECHT,3508 TA UTRECHT,NETHERLANDS. SISSA,INT SCH ADV STUDIES,TRIESTE,ITALY. LANDESSTERNWARTE HEIDELBERG KONIGSTUHL,D-69117 HEIDELBERG,GERMANY. ESA,IUE OBSERV,E-28080 MADRID,SPAIN. UNIV LEICESTER,DEPT PHYS,LEICESTER LE1 7RH,ENGLAND. UNIV MICHIGAN,DEPT ASTRON,ANN ARBOR,MI 48109. UNIV NEW S WALES,DEPT ASTRON,KENSINGTON,NSW 2033,AUSTRALIA. RP EDELSON, R (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,CODE 666,GREENBELT,MD 20771, USA. RI Donahue, Megan/B-5361-2012; Urry, Claudia/G-7381-2011 OI Urry, Claudia/0000-0002-0745-9792 NR 54 TC 82 Z9 84 U1 1 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 JAN 1 PY 1995 VL 438 IS 1 BP 120 EP 134 DI 10.1086/175059 PN 1 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA055 UT WOS:A1995QA05500011 ER PT J AU HILL, JK CHENG, KP BOHLIN, RC CORNETT, RH HINTZEN, PMN OCONNELL, RW ROBERTS, MS SMITH, AM SMITH, EP STECHER, TP AF HILL, JK CHENG, KP BOHLIN, RC CORNETT, RH HINTZEN, PMN OCONNELL, RW ROBERTS, MS SMITH, AM SMITH, EP STECHER, TP TI ULTRAVIOLET IMAGING TELESCOPE AND OPTICAL EMISSION-LINE OBSERVATIONS OF H-II REGIONS IN M81 SO ASTROPHYSICAL JOURNAL LA English DT Article DE DUST, EXTINCTION; GALAXIES, INDIVIDUAL (M81); GALAXIES, STELLAR CONTENT; H-II REGIONS; ULTRAVIOLET, GALAXIES ID ROCKET ULTRAVIOLET; STAR FORMATION; NEARBY GALAXIES; EXTINCTION; IMAGES; DUST AB Images of the type Sab spiral galaxy M81 were obtained in far-UV and near-UV bands by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Spacelab mission of 1990 December. Magnitudes in the two UV bands are determined for 52 H II regions from the catalog of Petit, Sivan, & Karachentsev (1988). Fluxes of the Halpha and Hbeta emission lines are determined from CCD images. Extinctions for the brightest H II regions are determined from observed Balmer decrements. Fainter H II regions are assigned the average of published radio-Halpha extinctions for several bright H II regions. The radiative transfer models of Witt, Thronson, & Capuano (1992) are shown to predict a relationship between Balmer Decrement and Halpha extinction consistent with observed line and radio fluxes for the brightest 7 H II regions and are used to estimate the UV extinction. Ratios of Lyman continuum flux (computed from the extinction corrected Halpha flux) to the extinction corrected far-UV flux are compared with ratios predicted by model spectra computed for IMF slope equal to -1.0 and stellar masses ranging from 5 to 120 M(.). Ages and masses are estimated by comparing the Halpha and far-UV fluxes and their ratio with the models. The total of the estimated stellar masses for the 52 H II regions is 1.4 x 10(5) M(.). The star-formation rate inferred for M81 from the observed UV and Halpha fluxes is low for a spiral galaxy at approximately 0.13 M(.) yr-1, but consistent with the low star-formation rates obtained by Kennicutt (1983) and Caldwell et al. (1991) for early-type spirals. C1 SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. UNIV VIRGINIA, CHARLOTTESVILLE, VA 22903 USA. NATL RADIO ASTRON OBSERV, CHARLOTTESVILLE, VA 22903 USA. NASA, GODDARD SPACE FLIGHT CTR, ASTRON & SOLAR PHYS LAB, GREENBELT, MD 20771 USA. CALIF STATE UNIV LONG BEACH, DEPT PHYS & ASTRON, LONG BEACH, CA 90840 USA. RP HILL, JK (reprint author), HUGHES STX, 4400 FORBES BLVD, LANHAM, MD 20706 USA. NR 25 TC 24 Z9 24 U1 0 U2 1 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 JAN 1 PY 1995 VL 438 IS 1 BP 181 EP 187 DI 10.1086/175063 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA055 UT WOS:A1995QA05500015 ER PT J AU HANNER, MS BROOKE, TY TOKUNAGA, AT AF HANNER, MS BROOKE, TY TOKUNAGA, AT TI 10-MICRON SPECTROSCOPY OF YOUNG STARS IN THE RHO-OPHIUCHI CLOUD SO ASTROPHYSICAL JOURNAL LA English DT Article DE CIRCUMSTELLAR MATTER; INFRARED, STARS; ISM, INDIVIDUAL (RHO-OPHIUCHI); STARS, PRE-MAIN-SEQUENCE ID INFRARED-EMISSION BANDS; DARK CLOUD; OPTICAL-PROPERTIES; IRAS OBSERVATIONS; SILICATES; DUST; EXTINCTION; FEATURES; GRAINS; SPECTROPHOTOMETRY AB Spectra in the 10 mum region were obtained of 14 young stars associated with the central core of the rho Oph dark cloud complex. Silicate dust emission and absorption features can be fairly well reproduced with simple models using the emissivity of the silicates in the Orion Trapezium region, believed to be typical of molecular cloud dust. A spectrum of the Trapezium star theta1 Ori D was obtained to define the emissivity more precisely. The emissivity of silicate dust around the late-type giant mu Cep does not improve the fits to the absorption features and provides a poorer match to the emission features. None of the sources display a strong 11.2 mum peak like that seen in comet Halley and attributed to crystalline olivine. A broad weak feature near 11.2 mum, possibly related to the comet feature, may be present in the emission spectrum of the Herbig Ae star HD 150193. Absorption features toward two of the objects are narrower than would be expected from Trapezium-like silicates, suggesting differences in the composition of the silicates. The relation between the silicate extinction band depth and H2O ice band depths is determined for the deeply embedded objects. One late-type object, Elias 14, clearly shows the 11.25 mum aromatic hydrocarbon emission feature, possibly excited by the nearby B star, HD 147889, though the latter does not exhibit the feature. C1 UNIV HAWAII, INST ASTRON, HONOLULU, HI 96822 USA. RP HANNER, MS (reprint author), JET PROP LAB, MS 183-601, 4800 OAK GROVE DR, PASADENA, CA 91109 USA. NR 41 TC 53 Z9 53 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 JAN 1 PY 1995 VL 438 IS 1 BP 250 EP 258 DI 10.1086/175069 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA055 UT WOS:A1995QA05500021 ER PT J AU HOLLIS, JM JEWELL, PR LOVAS, FJ AF HOLLIS, JM JEWELL, PR LOVAS, FJ TI CONFIRMATION OF INTERSTELLAR METHYLENE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM, INDIVIDUAL (ORION-KL); ISM, MOLECULES; LINE, IDENTIFICATION ID WAVELENGTH SPECTRAL-LINES; GAS-PHASE CHEMISTRY; ORION NEBULA; CH2; CALIBRATION; CLOUDS; FREQUENCIES; STATE; MIXER; X3B1 AB Four spectral emission features of the N(KK) = 4(04)-3(13) rotational transition of methylene (CH2) have been detected at signal levels 5-7 sigma above noise toward the hot core of the Orion-KL nebula and the molecular cloud in proximity to the continuum source W51 M. Specifically, in both sources we have resolved the F = 6-5, 5-4, and 4-3 hyperfine transitions of the J = 5-4 fine-structure levels and detected the blended hyperfine structure of the J = 4-3 fine structure levels. At the J = 3-2 fine-structure levels, we have observed new transitions of NS, a known interstellar molecule, which severely contaminates the search for CH2 hyperfine transitions. These new sensitive observations finally confirm the existence of interstellar CH2 which was tentatively reported by us some years ago. C1 NATL READIO ASTRON OBSERV,TUCSON,AZ 85721. NIST,DIV MOLEC PHYS,GAITHERSBURG,MD 20899. RP HOLLIS, JM (reprint author), NASA,GODDARD SPACE FLIGHT CTR,DIV SPACE DATA COMP,CODE 930,GREENBELT,MD 20771, USA. NR 22 TC 31 Z9 31 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 JAN 1 PY 1995 VL 438 IS 1 BP 259 EP 264 DI 10.1086/175070 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA055 UT WOS:A1995QA05500022 ER PT J AU BALIUNAS, SL DONAHUE, RA SOON, WH HORNE, JH FRAZER, J WOODARDEKLUND, L BRADFORD, M RAO, LM WILSON, OC ZHANG, Q BENNETT, W BRIGGS, J CARROLL, SM DUNCAN, DK FIGUEROA, D LANNING, HH MISCH, A MUELLER, J NOYES, RW POPPE, D PORTER, AC ROBINSON, CR RUSSELL, J SHELTON, JC SOYUMER, T VAUGHAN, AH WHITNEY, JH AF BALIUNAS, SL DONAHUE, RA SOON, WH HORNE, JH FRAZER, J WOODARDEKLUND, L BRADFORD, M RAO, LM WILSON, OC ZHANG, Q BENNETT, W BRIGGS, J CARROLL, SM DUNCAN, DK FIGUEROA, D LANNING, HH MISCH, A MUELLER, J NOYES, RW POPPE, D PORTER, AC ROBINSON, CR RUSSELL, J SHELTON, JC SOYUMER, T VAUGHAN, AH WHITNEY, JH TI CHROMOSPHERIC VARIATIONS IN MAIN-SEQUENCE STARS .2. SO ASTROPHYSICAL JOURNAL LA English DT Review DE STARS ACTIVITY; STARS CHROMOSPHERES; STARS LATE-TYPE; STARS ROTATION ID CA-II H; EMISSION-LINE FLUXES; SOLAR-TYPE STARS; K-EMISSION; COOL STARS; MAGNETIC-STRUCTURE; STELLAR ROTATION; TIME VARIATIONS; BINARY STARS; CYCLE AB The fluxes in passbands 0.1 nm wide and centered on the Ca II H and K emission cores have been monitored in 111 stars of spectral type F2-M2 on or near the main sequence in a continuation of an observing program started by O. C. Wilson. Most of the measurements began in 1966, with observations scheduled monthly until 1980, when observations were scheduled several times per week. The records, with a long-term precision of about 1.5%, display fluctuations that can be identified with variations on timescales similar to the 11 yr cycle of solar activity as well as axial rotation, and the growth and decay of emitting regions. We present the records of chromospheric emission and general conclusions about variations in surface magnetic activity on timescales greater than 1 yr but less than a few decades. The results for stars of spectral type G0-K5 V indicate a pattern of change in rotation and chromospheric activity on an evolutionary timescale, in which (1) young stars exhibit high average levels of activity, rapid rotation rates, no Maunder minimum phase and rarely display a smooth, cyclic variation; (2) stars of intermediate age (approximately 1-2 Gyr for 1 M.) have moderate levels of activity and rotation rates, and occasional smooth cycles; and (3) stars as old as the Sun and older have slower rotation rates, lower activity levels, and smooth cycles with occasional Maunder minimum-phases. C1 TENNESSEE STATE UNIV, CTR EXCELLENCE INFORMAT SYST, NASHVILLE, TN 37203 USA. HOOVER INST WAR REVOLUT & PEACE, STANFORD, CA 94305 USA. YALE UNIV, DEPT PHYS, NEW HAVEN, CT 06520 USA. MT WILSON OBSERV, MT WILSON, CA 91023 USA. UNIV CALIF LOS ANGELES, DEPT ASTRON, LOS ANGELES, CA 90024 USA. UNIV WISCONSIN, DEPT ASTRON, MADISON, WI 53706 USA. YERKES OBSERV, WILLIAMS BAY, WI 53191 USA. MIT, CTR THEORET PHYS, NUCL SCI LAB, CAMBRIDGE, MA 02139 USA. MIT, DEPT PHYS, CAMBRIDGE, MA 02139 USA. UNIV CHICAGO, DEPT ASTRON & ASTROPHYS, CHICAGO, IL 60637 USA. ADLER PLANETARIUM, CHICAGO, IL 60637 USA. COMP SCI CORP, SPACE TELESCOPE SCI INST, BALTIMORE, MD 21218 USA. LICK OBSERV, SANTA CRUZ, CA 95064 USA. PALOMAR OBSERV, PALOMAR MT, CA 92060 USA. NATL OPT ASTRON OBSERV, TUCSON, AZ 85726 USA. PENN STATE UNIV, DEPT ASTRON & ASTROPHYS, UNIVERSITY PK, PA 16802 USA. JET PROP LAB, OFF SPACE SCI & INSTRUMENTAT, PASADENA, CA 91109 USA. UNIV VIRGINIA, DEPT ASTRON, UNIV STN, CHARLOTTESVILLE, VA 22903 USA. RP BALIUNAS, SL (reprint author), HARVARD SMITHSONIAN CTR ASTROPHYS, 60 GARDEN ST, CAMBRIDGE, MA 02138 USA. NR 104 TC 602 Z9 604 U1 1 U2 5 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 JAN 1 PY 1995 VL 438 IS 1 BP 269 EP 287 DI 10.1086/175072 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA055 UT WOS:A1995QA05500024 ER PT J AU WHEATON, WA DUNKLEE, AL JACOBSON, AS LING, JC MAHONEY, WA RADOCINSKI, RG AF WHEATON, WA DUNKLEE, AL JACOBSON, AS LING, JC MAHONEY, WA RADOCINSKI, RG TI MULTIPARAMETER LINEAR LEAST-SQUARES FITTING TO POISSON DATA ONE COUNT AT A TIME SO ASTROPHYSICAL JOURNAL LA English DT Article DE GAMMA RAYS, GENERAL; NUMERICAL METHODS ID POSITRON-ANNIHILATION RADIATION; GAMMA-RAY SPECTROMETER; CYGNUS-X-1; GALAXIES AB A standard problem in gamma-ray astronomy data analysis is the decomposition of a set of observed counts, described by Poisson statistics, according to a given multicomponent linear model, with underlying physical count rates or fluxes which are to be estimated from the data. Despite its conceptual simplicity, the linear least-squares (LLSQ) method for solving this problem has generally been limited to situations in which the number n(i) of counts in each bin i is not too small, conventionally more than 5-30. It seems to be widely believed that the failure of the LLSQ method for small counts is due to the failure of the Poisson distribution to be even approximately normal for small numbers. The cause is more accurately the strong anticorrelation between the data and the weights w(i) in the weighted LLSQ method when square-rootn(i) instead of square-rootnBAR(i) is used to approximate the uncertainties, sigma(i), in the data, where nBAR(i) = E[n(i)], the expected value of n(i). We show in an appendix that, avoiding this approximation, the correct equations for the Poisson LLSQ (PLLSQ) problem are actually identical to those for the maximum likelihood estimate using the exact Poisson distribution. Since weighted linear least-squares involves a kind of weighted averaging, LLSQ estimators generally produce biased results when the data and their weights are correlated. We describe a class of weighted PLLSQ estimators which are linear functions of the observed counts. Such PLLSQ estimators are unbiased independent of nBAR(i), even when the average number of counts in an entire fit is much less than one. Their variance is a minimum when the weights are calculated from the true variances of the data, but in general these are not accurately known. Fortunately, the variance of the estimate is a very weak function of the weights near the optimum value, so for the PLLSQ problem it is easy in practice to find weights that are virtually ideal yet still completely unbiased. PLLSQ estimators which are linear in the data also allow fitting multiple data sets by the calculation of only a scalar product, without the need to repeat the accumulation and solution of the LLSQ equations. Owing also to the linearity of the estimates in the data, each count contributes to the answers independently of every other count, so that the results for small bins are independent of the particular choice of binning. This property makes possible PLLSQ methods which avoid binning the data altogether. Some alternatives to the approximation of the uncertainties in the data by the square root of the observed counts are discussed. We apply the method to solve a problem in high-resolution gamma-ray spectroscopy for the JPL High-Resolution Gamma-Ray Spectrometer flown on HEAO 3. Systematic error in subtracting the strong, highly variable background encountered in the low-energy gamma-ray region can be significantly reduced by closely pairing source and background data in short segments. Significant results can be built up by weighted averaging of the net fluxes obtained from the subtraction of many individual source/background pairs. Extension of the approach to complex situations, with multiple cosmic sources and realistic background parameterizations, requires a means of efficiently fitting to data from single scans in the narrow (almost-equal-to 1.2 keV, for HEAO 3) energy channels of a Ge spectrometer, where the expected number of counts obtained per scan may be very low. Such an analysis system is discussed and compared to the method previously used. RP WHEATON, WA (reprint author), JET PROP LAB,MS 169-327,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 27 TC 28 Z9 28 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 JAN 1 PY 1995 VL 438 IS 1 BP 322 EP 340 DI 10.1086/175077 PN 1 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA055 UT WOS:A1995QA05500029 ER PT J AU DSILVA, S DUVALL, TL AF DSILVA, S DUVALL, TL TI TIME-DISTANCE HELIOSEISMOLOGY IN THE VICINITY OF SUNSPOTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE MHD; SUN, OSCILLATIONS; SUNSPOTS ID SOLAR CONVECTION ZONE; MAGNETIC-FLUX TUBES; P-MODES; ABSORPTION; OSCILLATIONS; EVOLUTION; REGIONS; SUN AB We use the ray description of acoustic-gravity modes to calculate time-distance diagrams for the quiet Sun and for regions in the vicinity of a sunspot with a monolithic flux-tube structure. Time-distance curves for the quiet Sun match the observations of Duvall et al. In the vicinity of a sunspot these quiet Sun curves split into a family of closely spaced curves. The structure of this bandlike feature is found to be sensitive to the sunspot model, and can be a diagnostic of the subsurface geometry of the sunspot flux tube. C1 NASA, GODDARD SPACE FLIGHT CTR, GSFC, ASTRON & SOLAR PHYS LAB, GREENBELT, MD 20771 USA. RP DSILVA, S (reprint author), NATL OPT ASTRON OBSERV, NATL SOLAR OBSERV, TUCSON, AZ 85726 USA. RI Duvall, Thomas/C-9998-2012 NR 39 TC 27 Z9 27 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 JAN 1 PY 1995 VL 438 IS 1 BP 454 EP 462 DI 10.1086/175089 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA055 UT WOS:A1995QA05500041 ER PT J AU PORTER, JG FONTENLA, JM SIMNETT, GM AF PORTER, JG FONTENLA, JM SIMNETT, GM TI SIMULTANEOUS ULTRAVIOLET AND X-RAY OBSERVATIONS OF SOLAR MICROFLARES SO ASTROPHYSICAL JOURNAL LA English DT Article DE SUN, FLARES; SUN, UV RADIATION; SUN, X-RAYS, GAMMA RAYS ID ACTIVE REGION; MAXIMUM MISSION; FLARES; BURSTS; EMISSION; OSO-8; BRIGHTENINGS; SPECTROMETER; UV AB We present a comparison of observations of a solar active region obtained with the Ultraviolet Spectrometer and Polarimeter (UVSP) and the Hard X-ray Imaging Spectrometer (HXIS) on board the Solar Maximum Mission (SMM). The data show many subflares and smaller events during a 9 hr period in which there were no major flares. This activity is associated with areas of complex, evolving magnetic fields. Events substantially smaller than subflares, identified in C IV 1548 angstrom emission (T = 10(5) K), are found to have impulsive counterparts in 3.5-5.5 keV X-ray emission characteristic of T approximately 10(7) K. These ''microflares'' are therefore true members of the flare family, reaching temperatures greater than that of the ambient solar corona. Plots of X-ray versus UV emission show that the emission from the smaller microflares is softer than that from the larger microflares and subflares. Distributions of solar flares with energy that are based on hard X-ray fluxes can be corrected using this X-ray/UV relationship. The corrected distributions suggest that microflares play a larger role in coronal heating than was indicated by analysis of the original distributions. C1 UNIV ALABAMA,CSPAR,HUNTSVILLE,AL 35899. UNIV BIRMINGHAM,DEPT PHYS & SPACE RES,BIRMINGHAM B15 2TT,W MIDLANDS,ENGLAND. RP PORTER, JG (reprint author), NASA,GEORGE C MARSHALL SPACE FLIGHT CTR,SPACE SCI LAB,ES 82,HUNTSVILLE,AL 35812, USA. NR 47 TC 50 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 JAN 1 PY 1995 VL 438 IS 1 BP 472 EP 479 DI 10.1086/175091 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA055 UT WOS:A1995QA05500043 ER PT J AU KEENAN, FP RAMSBOTTOM, CA BELL, KL BERRINGTON, KA HIBBERT, A FEIBELMAN, WA BLAIR, WP AF KEENAN, FP RAMSBOTTOM, CA BELL, KL BERRINGTON, KA HIBBERT, A FEIBELMAN, WA BLAIR, WP TI N-IV EMISSION-LINES IN THE ULTRAVIOLET-SPECTRA OF GASEOUS NEBULAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ATOMIC DATA; ATOMIC PROCESSES; ULTRAVIOLET, ISM ID PLANETARY-NEBULAE; OPACITY CALCULATIONS; IUE OBSERVATIONS; CYGNUS LOOP; ATOMIC DATA; STRENGTHS; ABUNDANCES; TELESCOPE; PLASMAS; HBV-475 AB Theoretical electron density sensitive emission-line ratios, determined using electron impact excitation rates calculated with the R-matrix code, are presented for R = I(2s2 1S-2s2p 3P2)/I(2s2 1S-2s2p 3P1) = I(1483 angstrom)/I(1486 angstrom) in N IV. These are found to be up to an order of magnitude different from those deduced by previous authors, principally due to the inclusion of excitation rates for transitions among the 2s2p 3P fine-structure levels. The observed values of R for several planetary nebulae, symbiotic stars and the Cygnus Loop supernova remnant, measured from spectra obtained with the International Ultraviolet Explorer (IUE) satellite and the Hopkins Ultraviolet Telescope (HUT), lead to electron densities which are in excellent agreement with those deduced from line ratios in other species. This provides observational support for the accuracy of the atomic data adopted in the present calculations. C1 QUEENS UNIV BELFAST,DEPT APPL MATH & THEORET PHYS,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. JOHNS HOPKINS UNIV,CTR ASTROPHYS SCI,DEPT PHYS & ASTRON,BALTIMORE,MD 21218. RP KEENAN, FP (reprint author), QUEENS UNIV BELFAST,DEPT PURE & APPL PHYS,BELFAST BT7 1NN,ANTRIM,NORTH IRELAND. NR 29 TC 19 Z9 19 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 1 PY 1995 VL 438 IS 1 BP 500 EP 503 DI 10.1086/175094 PN 1 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA055 UT WOS:A1995QA05500046 ER PT J AU RAMATY, R KOZLOVSKY, B LINGENFELTER, RE AF RAMATY, R KOZLOVSKY, B LINGENFELTER, RE TI GAMMA-RAY LINES FROM THE ORION COMPLEX SO ASTROPHYSICAL JOURNAL LA English DT Article DE ACCELERATION OF PARTICLES; GALAXY, ABUNDANCES; GAMMA RAYS, THEORY; NUCLEAR REACTIONS, NUCLEOSYNTHESIS, ABUNDANCES; STARS, WOLF-RAYET; SUPERNOVAE, GENERAL ID PARTICLE INTERACTIONS; MASSIVE STARS; AL-26 AB We show that the 4.44 and 6.13 MeV line emission observed with COMPTEL from Orion is consistent with gamma-ray spectra consisting of a mixture of narrow and broad lines or spectra containing only broad lines. We employed several accelerated particle compositions and showed that the current COMPTEL data in the 3-7 MeV region alone cannot distinguish between the various possibilities. However, the COMPTEL upper limits in the 1-3 MeV band favor a composition similar to that of the winds of Wolf-Rayet stars of spectral type WC. The power dissipated by the accelerated particles at Orion is about 4 x 10(38) ergs s(-1). These particles are not expected to produce significant amounts of Al-26. C1 TEL AVIV UNIV,SCH PHYS & ASTRON,IL-69978 TEL AVIV,ISRAEL. UNIV CALIF SAN DIEGO,CTR ASTROPHYS & SPACE SCI,LA JOLLA,CA 92093. RP RAMATY, R (reprint author), NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY PHYS LAB,GREENBELT,MD 20771, USA. NR 17 TC 50 Z9 50 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 JAN 1 PY 1995 VL 438 IS 1 BP L21 EP L24 DI 10.1086/187705 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QA057 UT WOS:A1995QA05700006 ER PT J AU MAGNANI, L CAILLAULT, JP BUCHALTER, A BEICHMAN, CA AF MAGNANI, L CAILLAULT, JP BUCHALTER, A BEICHMAN, CA TI A SEARCH FOR T-TAURI STARS IN HIGH-LATITUDE MOLECULAR CLOUDS .2. THE IRAS FAINT SOURCE SURVEY CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE CATALOGS; INFRARED, STARS; ISM, CLOUDS; STARS, PRE-MAIN-SEQUENCE; STARS, STATISTICS ID YOUNG STELLAR OBJECTS; POINT-SOURCE CATALOG; EMISSION-LINE STARS; GALACTIC LATITUDE; DARK CLOUD; CO SURVEY; AURIGA; GALAXIES; REGIONS; CIRRUS AB We present a catalog of infrared point sources from the IRAS Faint Source Survey at Galactic latitudes \b\greater than or equal to 30 degrees. The aim of this paper is to provide a list of possible star-forming sites at high Galactic latitudes in order to address the question of whether or not the translucent molecular clouds (which are most easily identified at high latitudes) are capable of star formation. The primary list of sources has 12, 25, 60, and 100 mu m fluxes within the range typical of pre-main-sequence or T Tauri stars. A secondary list has the same range of 12, 25, and 60 mu m fluxes, but only upper limits at 100 mu m. A total of 127 candidates from the first category and 65 candidates from the second category are identified and their positions and infrared spectral characteristics tabulated. Although the colors and fluxes of these sources are typical of T Tauri or pre-main-sequence stars and YSOs, extralactic sources and planetary nebulae sometimes have similar colors. These lists provide a starting point for optical spectroscopy or other techniques to positively identify these objects. We can determine an upper limit to the star forming efficiency of high-latitude molecular clouds assuming all the candidates in our sample are pre-main sequence stars of one solar mass. The upper limit of a few tenths of 1% is less than the star-forming efficiency of local dark cloud complexes such as the Taurus-Auriga or rho Ophiuchus clouds. C1 STANFORD UNIV,STANFORD,CA 94305. UNIV GEORGIA,SUMER NASA JOVE INTERN,ATHENS,GA 30602. CALTECH,JET PROP LAB,CTR INFRARED PROC & ANAL,PASADENA,CA 91125. RP MAGNANI, L (reprint author), UNIV GEORGIA,DEPT PHYS & ASTRON,ATHENS,GA 30602, USA. NR 65 TC 25 Z9 25 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 JAN PY 1995 VL 96 IS 1 BP 159 EP 173 DI 10.1086/192116 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA PZ339 UT WOS:A1995PZ33900006 ER PT J AU AYRES, TR FLEMING, TA SIMON, T HAISCH, BM BROWN, A LENZ, D WAMSTEKER, W DEMARTINO, D GONZALEZ, C BONNELL, J MASHESSE, JM ROSSO, C SCHMITT, JHMM TRUMPER, J VOGES, W PYE, J DEMPSEY, RC LINSKY, JL GUINAN, EF HARPER, GM JORDAN, C MONTESINOS, BM PAGANO, I RODONO, M AF AYRES, TR FLEMING, TA SIMON, T HAISCH, BM BROWN, A LENZ, D WAMSTEKER, W DEMARTINO, D GONZALEZ, C BONNELL, J MASHESSE, JM ROSSO, C SCHMITT, JHMM TRUMPER, J VOGES, W PYE, J DEMPSEY, RC LINSKY, JL GUINAN, EF HARPER, GM JORDAN, C MONTESINOS, BM PAGANO, I RODONO, M TI THE RIASS CORONATHON - JOINT X-RAY AND ULTRAVIOLET OBSERVATIONS OF NORMAL F-K STARS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE STARS, CORONAE; STARS, CHROMOSPHERE; STARS, LATE-TYPE; ULTRAVIOLET, STARS; X-RAYS, STARS ID ALL-SKY SURVEY; MAIN-SEQUENCE STARS; SOLAR-TYPE STARS; COOL STARS; CHROMOSPHERIC ACTIVITY; OUTER ATMOSPHERES; ROTATIONAL MODULATION; MAGNETIC-STRUCTURE; OXYGEN ABUNDANCES; STELLAR ACTIVITY AB Between 1990 August and 1991 January the ROSAT/IUE All Sky Survey (RIASS) coordinated pointings by the International Ultraviolet Explorer with the continuous X-ray/EUV mapping by the Rontgensatellit. The campaign provided an unprecedented multiwavelength view of a wide variety of cosmic sources. We report findings for F-K stars, a large proportion of the RIASS targets. Forty-eight of our 91 ''Coronathon'' candidates were observed by the IUE during the campaign. For stars missed by the IUE, we supplemented the ROSAT survey fluxes with archival UV spectra and/or follow-on observations. In addition to the coordinated work, we examined the UV emission histories of the Coronathon stars. Several of the dwarfs show evidence for long-term variations in their Mg II lambda 2802[h] emissions, and C IV lambda 1549 in a few cases. alpha Cen B (K0 V) and 0(2) Eri (K1 V) are noteworthy examples. Hertzsprung gap giants like 31 Com (G0 III) and the secondary of Capella (alpha Aur Ab: G0 III) are relatively constant in C IV and Mg II, at least over decade timescales. Similarly, G8-K0 ''Clump'' giants show only modest long-term changes in their ultraviolet emissions. On the other hand, several of the ''hybrid chromosphere'' G and K supergiants show dramatic variability in the wind absorption components of their Mg II h profiles. The closely related but more active G supergiants like beta Cam and beta Dra show smaller changes in their Mg II fluxes, and symmetric profile variations. Despite clear indications of secular variability, we find little support for the suspicion that previous broad statistical X-ray/UV studies of normal stars have been compromised by nonsimultaneous data sets. For well-studied stars, the temporal standard deviation rarely exceeds 20% in C IV, and 10% in Mg II h. We find no evidence that long-term cycles play any significant role in fostering the large dispersion in activity within any of the stellar classes. We correlated the X-ray and UV emissions, normalized to the stellar bolometric fluxes (e.g., R(x) drop fX/fbol). As found by Ayres, Marstad, & Linsky, MS stars of spectral types F-K obey a power-law relation between R(x) and R(h) with a slope of approximate to 3. Here, the dwarf stars follow a R(CIV) versus R(h), power law of slope approximate to 2, and a R(x) versus R(CIV) power law of slope approximate to 1.5. The F9-G2 ''solar-type'' MS stars have a significantly steeper slope in X-rays versus C IV than the cooler G8-K5 dwarfs. The populous Clump giants follow essentially the same behavior as the cooler MS stars, showing a nearly 1:1 correlation between X-rays and C IV. However, other key groups-some F dwarfs, the Hertzsprung gap giants, and virtually all of the supergiants-fall systematically to lower R(x) with respect to their R(CIV) and R(h) (as noted previously by Simon and Drake for the former two classes), and exhibit steeper power laws than the cooler stars. The MS and evolved stars detected in both X-rays and the WFC S1 and S2 filters show close to a 1:1 connection between their normalized coronal and EUV fluxes. Thus, the latter likely are dominated by T> 10(6) K emissions. There is no distortion in the X-ray/EUV diagram which would indicate that the ''X-ray deficiency'' of the F dwarfs or Hertzsprung gap giants is caused by local absorption at the source. All of the X-ray deficient stars follow a normal (i.e., MS) correlation between R(CIV) and R(h), suggesting that the X-ray deficit truly is a coronal anomaly. Many of the Clump giants, and G/K supergiants, show enhanced N V/C IV ratios, possibly associated with envelope enrichment of nitrogen at first dredge-up. C IV/C II ratios display a slight tilt toward larger values with increasing R(x) in the dwarf stars, but a nearly 1:1 relation in the Clump giants. The origin of the effect is uncertain. O I/Mg II ratios exhibit a systematic increase in the more luminous objects. The origin likely is Bowen fluorescence. The ''coronal proxy'' He II lambda 1640 shows a near 1:1 correlation with X-rays in the MS stars as a function of R(CIV), but a more complex behavior among the giants, particularly the X-ray deficient stars. Curiously, He II shows a 1:1 correlation with Si IV among the X-ray deficient giants, displaced a factor of similar to 2 below the relation obeyed by the Clump giants and cooler MS stars. These behaviors are consistent with recombination domination in the dwarfs and Clump giants, but the situation among the warm luminous stars is ambiguous. The wide diversity of X-ray emission levels in the Clump-as exemplified by the Hyades K giants-emphasizes the sensitive role played by stellar evolution in controlling coronal activity. The wide diversity of X-ray emission in general points to a magnetic origin for the coronal heating. C1 UNIV COLORADO,JOINT INST LAB ASTROPHYS,BOULDER,CO 80309. UNIV HAWAII,INST ASTRON,HONOLULU,HI 96822. LOCKHEED PALO ALTO RES LABS,PALO ALTO,CA 94304. EUROPEAN SPACE AGCY,IUE OBSERV,E-28080 MADRID,SPAIN. NASA,GODDARD SPACE FLIGHT CTR,IUE OBSERV,GREENBELT,MD 20771. UNIV COMPLUTENSE MADRID,DEPT ASTROFIS,E-28040 MADRID,SPAIN. MAX PLANCK INST EXTRATERR PHYS,W-8046 GARCHING,GERMANY. UNIV LEICESTER,DEPT PHYS,LEICESTER LE1 7RH,LEICS,ENGLAND. UNIV LEICESTER,XRAY ASTRON GRP,LEICESTER LE1 7RH,LEICS,ENGLAND. VILLANOVA UNIV,DEPT ASTRON,VILLANOVA,PA 19085. UNIV OXFORD,DEPT THEORET PHYS,OXFORD OX1 3NP,ENGLAND. UNIV CATANIA,IST ASTRON,I-95125 CATANIA,ITALY. OSSERV ASTROFIS CATANIA,I-95125 CATANIA,ITALY. RP AYRES, TR (reprint author), UNIV COLORADO,CTR ASTROPHYS & SPACE ASTRON,CAMPUS BOX 389,BOULDER,CO 80309, USA. RI Pagano, Isabella/I-6934-2015; Montesinos, Benjamin/C-3493-2017; Mas-Hesse, J. Miguel /K-6805-2014 OI Pagano, Isabella/0000-0001-9573-4928; Montesinos, Benjamin/0000-0002-7982-2095; Mas-Hesse, J. Miguel /0000-0002-8823-9723 NR 96 TC 91 Z9 91 U1 0 U2 2 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 JAN PY 1995 VL 96 IS 1 BP 223 EP 259 DI 10.1086/192118 PG 37 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA PZ339 UT WOS:A1995PZ33900008 ER PT J AU WEAVER, KA ARNAUD, KA BOLDT, EA CHRISTIAN, D CORCORAN, M HOLT, SS JAHODA, K KELLEY, R MARSHALL, FE MUSHOTZKY, RF PETRE, R RAWLEY, G SERLEMITSOS, PJ SCHLEGEL, EM SMALE, AP SWANK, JH SZYMKOWIAK, AE AF WEAVER, KA ARNAUD, KA BOLDT, EA CHRISTIAN, D CORCORAN, M HOLT, SS JAHODA, K KELLEY, R MARSHALL, FE MUSHOTZKY, RF PETRE, R RAWLEY, G SERLEMITSOS, PJ SCHLEGEL, EM SMALE, AP SWANK, JH SZYMKOWIAK, AE TI CALIBRATING THE BROAD-BAND X-RAY TELESCOPE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE INSTRUMENTATION, DETECTORS; SPACE VEHICLES; X-RAYS, GENERAL ID SI(LI) DETECTOR AB This paper describes the calibration of the two solid-state Si(Li) X-ray detectors and the X-ray telescopes that flew as part of Goddard Space Flight Center's Broad Band X-Ray Telescope (BBXRT) experiment on board the space shuttle Columbia in 1990 December. During the 9 day shuttle mission, BBXRT performed similar to 150 observations of 82 celestial sources. The content of the archive is summarized here. Although BBXRT had a relatively short life, it stands as a milestone in X-ray astronomy as being the first instrument to offer moderate spectral resolution over a wide bandpass (0.3-12.0 keV). Among other things, this paper discusses the effective area calibration of the instrument, the flux calibration and flux corrections for off-axis observations, the detector background, and optimal background subtraction techniques. The on-axis effective area calibration for the central detector elements was performed using data from the Crab Nebula, while other carefully selected targets were used for calibration of the outer detector elements. The remaining systematic uncertainties in the effective area calibration for point sources observed both on and off axis are generally less than 5%-10%. The energy scale is known to better than 0.5% at 6.0 keV for both detectors. The results presented here have an impact on the calibration of other medium resolution X-ray experiments such as the CCDs on board ASCA (Astro-D) as well as the Advanced X-Ray Astrophysics Facility detectors. C1 NASA,GODDARD SPACE FLIGHT CTR,CODE 666,GREENBELT,MD 20771. INST PHYS & CHEM RES,WAKO,SAITAMA 35101,JAPAN. RI Jahoda, Keith/D-5616-2012; Swank, Jean/F-2693-2012; Kelley, Richard/K-4474-2012 NR 31 TC 9 Z9 9 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 JAN PY 1995 VL 96 IS 1 BP 303 EP 324 DI 10.1086/192120 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA PZ339 UT WOS:A1995PZ33900010 ER PT J AU BHATIA, AK KASTNER, SO AF BHATIA, AK KASTNER, SO TI THE NEUTRAL OXYGEN SPECTRUM .1. COLLISIONALLY EXCITED-LEVEL POPULATIONS AND LINE-INTENSITIES UNDER OPTICALLY THIN CONDITIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE ATOMIC DATA; ATOMIC PROCESSES ID OUTER ATMOSPHERIC STRUCTURE; ATOMIC OXYGEN; CROSS-SECTIONS; GIANT STARS; IUE; SPECTROSCOPY; TRANSITIONS; CONSTRAINTS; EXCITATION; QUASARS AB This is the first paper in a projected program to produce quantitative information on the spectrum of the neutral oxygen atom under a variety of excitation conditions. Radiative rates and effective collision strengths are assembled from the recent literature where available, or are calculated for as yet untreated transitions using the University College superstructure/distorted-wave computer package, to produce a complete set of atomic data for a 13 hybrid level model of neutral oxygen. Level populations and relative intensities for 28 allowed, intercombination, and forbidden oxygen lines are computed, under optically thin conditions, for the electron density range 4.0 < log N-e < 12.0 and the electron temperature values T-e = 5000, 10,000, 20,000, 50,000, and 100,000 K. Preliminary applications to observed intercombination/allowed and forbidden/allowed line ratios are discussed. C1 MATH SCI CONSULTANTS INC,GREENBELT,MD 20770. RP BHATIA, AK (reprint author), NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,ASTRON BRANCH,GREENBELT,MD 20771, USA. NR 39 TC 37 Z9 37 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 JAN PY 1995 VL 96 IS 1 BP 325 EP 341 DI 10.1086/192121 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA PZ339 UT WOS:A1995PZ33900011 ER PT J AU Bersanelli, M Smoot, GF Bensadoun, M DeAmici, G Limon, M Levin, S AF Bersanelli, M Smoot, GF Bensadoun, M DeAmici, G Limon, M Levin, S TI Measurements of the CMB spectrum at centimeter wavelengths SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article ID MICROWAVE BACKGROUND TEMPERATURE; GHZ; RADIATION; EMISSION; POLE AB Based on our recent absolute measurement at 2.0 GHz from the South Pole eve discuss the evaluation of atmospheric and Galactic foreground emission at centimeter wavelengths. Our differential measurements of Galactic emission compared to the Haslam map indicate a synchrotron spectral index alpha(syn) similar or equal to 2.6-2.7 between 0.4 and 2 GHz. C1 LAWRENCE BERKELEY LAB,BERKELEY,CA 94720. SPACE SCI LAB,BERKELEY,CA 94720. CALTECH,JET PROP LAB,CIT,PASADENA,CA 91109. NR 18 TC 8 Z9 8 U1 0 U2 0 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 32 IS 1-6 BP 7 EP 13 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU782 UT WOS:A1995VU78200003 ER PT J AU Kogut, A AF Kogut, A TI CMB spectrum measurements after COBE SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article ID BACKGROUND TEMPERATURE; SEPARATION; ANISOTROPY AB The spectrum of the cosmic microwave background (CMB) carries information on energetic processes in the universe from a redshift z similar to 10(6) to the present. COBE measurements limit deviations from a blackbody spectrum in the band 0.5-5 mm wavelength; however, physical processes relevant to structure formation (e.g., recent reionization, decay of primordial anisotropy, exotic particle decay) can generate spectral distortions which peak at longer wavelengths outside the COBE passband. Direct observational limits at these longer wavelengths are weak. I describe an instrument designed to measure the spectrum of the sky at wavelengths 1-10 cm to 100 mu K precision relative to a blackbody spectrum, and discuss the astrophysical and cosmological information to be gained from such a measurement. C1 NASA,GODDARD SPACE FLIGHT CTR,HUGHES STX,GREENBELT,MD 20771. RI Kogut, Alan/D-6293-2012 NR 8 TC 0 Z9 0 U1 0 U2 1 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 32 IS 1-6 BP 37 EP 43 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU782 UT WOS:A1995VU78200008 ER PT J AU Toffolatti, L Danese, L Franceschini, A Mandolesi, N Smoot, GF Bersanelli, M Vittorio, N Lasenby, A Partridge, RB Davies, R Sironi, G Cesarsky, C LachiezeRey, M MartinezGonzalez, E Beckman, J Rebolo, R Saez, D Debernardis, P Dalloglio, G Crane, P Janssen, M Puget, JL Bussoletti, E Raffelt, G Encrenaz, P Natale, V Tofani, G Merluzzi, P Scaramella, R Efstathiou, G AF Toffolatti, L Danese, L Franceschini, A Mandolesi, N Smoot, GF Bersanelli, M Vittorio, N Lasenby, A Partridge, RB Davies, R Sironi, G Cesarsky, C LachiezeRey, M MartinezGonzalez, E Beckman, J Rebolo, R Saez, D Debernardis, P Dalloglio, G Crane, P Janssen, M Puget, JL Bussoletti, E Raffelt, G Encrenaz, P Natale, V Tofani, G Merluzzi, P Scaramella, R Efstathiou, G TI Foreground contributions to 0.2-2 degrees CMB anisotropies SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article DE cosmic background radiation; galaxy, general infrared, galaxies; radio sources ID COSMIC BACKGROUND-RADIATION; DIFFERENTIAL MICROWAVE RADIOMETER; SMALL-SCALE FLUCTUATIONS; FAR-INFRARED EMISSION; CONFUSION NOISE; SOURCE COUNTS; GALAXIES; WAVELENGTHS; EVOLUTION; SPECTRUM AB We examine the extent to which galactic and extragalactic foregrounds car, hamper the detection of primordial Cosmic Microwave Background (CMB) anisotropies. We limit our discussion to intermediate angular scales, 10' less than or similar to theta less than or similar to 2 degrees, since many current as well as future experiments have been designed to map CMB anisotropies at these angular scales. In fact, scales of greater than or similar to 10' are of crucial importance to test both the conditions in the early Universe and current theories of the gravitational collapse. C1 OSSERV ASTRON PADOVA, PADUA, ITALY. DIPARTIMENTO ASTRON, I-35122 PADUA, ITALY. ITESRECNR, BOLOGNA, ITALY. LAWRENCE BERKELEY LAB, BERKELEY, CA USA. CNR, IFCTR, MILAN, ITALY. UNIV ROMA TOR VERGATA, DIPARTIMENTO FIS, I-00173 ROME, ITALY. UNIV CAMBRIDGE, CAMBRIDGE CB2 1TN, ENGLAND. HAVERFORD COLL, HAVERFORD, PA 19041 USA. UNIV MILAN, DIPARTIMENTO FIS, MILAN, ITALY. CEA, CEN, SAP, SACLAY, FRANCE. UNIV CANTABRIA, E-39005 SANTANDER, SPAIN. IST ASTROFIS LAS CANARIAS, TENERIFE, SPAIN. UNIV VALENCIA, VALENCIA, SPAIN. UNIV ROMA LA SAPIENZA, DIPARTIMENTO FIS, I-00185 ROME, ITALY. EUROPEAN SO OBSERV, D-8046 GARCHING, GERMANY. CALTECH, JET PROP LAB, PASADENA, CA 91125 USA. UNIV PARIS 11, IAS, ORSAY, FRANCE. IST UNIV NAVALE, NAPLES, ITALY. MAX PLANCK INST PHYS & ASTROPHYS, D-80805 MUNICH, GERMANY. OBSERV MEUDON, F-92195 MEUDON, FRANCE. CNR, CAISMI, OSSERV ASTRON ARCETERI, FLORENCE, ITALY. OSSERV ASTRON CAPODIMONTE, I-80131 NAPLES, ITALY. OSSERV ASTRON ROMA, I-00136 ROME, ITALY. UNIV OXFORD, OXFORD, ENGLAND. RI Toffolatti, Luigi/K-5070-2014; Martinez-Gonzalez, Enrique/E-9534-2015 OI Toffolatti, Luigi/0000-0003-2645-7386; Martinez-Gonzalez, Enrique/0000-0002-0179-8590 NR 55 TC 12 Z9 12 U1 0 U2 0 PU GORDON BREACH PUBLISHING, TAYLOR & FRANCIS GROUP PI PHILADELPHIA PA 325 CHESTNUT ST, 8TH FL, PHILADELPHIA, PA 19106 USA SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 32 IS 1-6 BP 125 EP 135 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU782 UT WOS:A1995VU78200018 ER PT J AU Lineweaver, CH Smoot, GF Tenorio, L Kogut, A AF Lineweaver, CH Smoot, GF Tenorio, L Kogut, A TI The cosmic microwave background dipole anisotropy testing the standard model SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article ID LARGE-SCALE; STREAMING MOTIONS; LOCAL GROUP; UNIVERSE; GALAXIES; CLUSTERS; FLUCTUATIONS; RADIOMETERS; INSTRUMENT; ORIGIN AB We discuss the recently published dipole anisotropy measurement from the COBE* Differential Microwave Radiometer (DMR) first-year skymaps (Kogut et al., 1993). We present what can be called the ''standard kinetic interpretation'' of this dipole. This standard model is found to be consistent with all observations with the possible exception of some large scale bull flow measurements. A confirmed detection of an X-ray background dipole in agreement with the CMB dipole would eliminate the two alternative interpretations presented. C1 UNIV CALIF BERKELEY,LBL,BERKELEY,CA 94720. UNIV CALIF BERKELEY,SSL,BERKELEY,CA 94720. UNIV CALIF BERKELEY,CFPA,BERKELEY,CA 94720. HUGHES STX CORP,NASA,GAFC,GREENBELT,MD 20771. RI Kogut, Alan/D-6293-2012 NR 34 TC 1 Z9 1 U1 0 U2 0 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 32 IS 1-6 BP 173 EP 181 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU782 UT WOS:A1995VU78200022 ER PT J AU Tanaka, S Alsop, D Cheng, E Clapp, A Cottingham, D Devlin, M Fischer, M Gundersen, J Hagmann, C Holmes, W Hristov, V Koch, T Kreysa, E Lange, A Lim, M Lubin, P Mauskopf, P Meinhold, P Richards, P Smoot, G Timbie, P AF Tanaka, S Alsop, D Cheng, E Clapp, A Cottingham, D Devlin, M Fischer, M Gundersen, J Hagmann, C Holmes, W Hristov, V Koch, T Kreysa, E Lange, A Lim, M Lubin, P Mauskopf, P Meinhold, P Richards, P Smoot, G Timbie, P TI The Millimeter Wave Anisotropy Experiment (MAX) SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article DE cosmic microwave background, cosmology; observations ID MICROWAVE BACKGROUND-RADIATION; ANGULAR SCALES AB The balloon-borne Millimeter Wave Anisotropy Experiment (MAX) observes fluctuations in the cosmic microwave background (CMB) on one degree angular scales. Measurements at these angular scales constrain scenarios of large scale structure formation. This paper presents an overview of the MAX experiment and the data obtained thus far from the four flights of the MAX experiment. C1 UNIV CALIF BERKELEY,CTR PARTICLE ASTROPHYS,BERKELEY,CA 94720. UNIV CALIF BERKELEY,DEPT PHYS,BERKELEY,CA 94720. NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. UNIV CALIF SANTA BARBARA,DEPT PHYS,SANTA BARBARA,CA 93106. MAX PLANCK INST RADIOASTRON,D-5300 BONN 1,GERMANY. UNIV CALIF BERKELEY,LAWRENCE BERKELEY LAB,BERKELEY,CA 94720. RI Alsop, David/J-5764-2013 OI Alsop, David/0000-0002-8206-1995 NR 10 TC 2 Z9 2 U1 0 U2 0 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 32 IS 1-6 BP 223 EP 228 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU782 UT WOS:A1995VU78200028 ER PT J AU Page, L Cheng, E Ganga, K Meyer, S AF Page, L Cheng, E Ganga, K Meyer, S TI The far infrared survey: Cross-correlation with the first-year DMR maps and auto-correlation function SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article DE cosmology; cosmic microwave background ID DIFFERENTIAL MICROWAVE RADIOMETER AB The results of an analysis of the Far Infrared Survey (FIRS) are presented. The data set is a 3.8 degrees resolution map at a frequency of 170 GHz covering roughly 1/4 of the sky. The production of the FIRS map is described in detail. Two results are given. 1) There is a strong cross-correlation between the FIRS and the DMR first-year maps. That is, the two maps contain similar patterns of anisotropy in Delta T/T. Because the maps are sensitive to different systematic effects and galactic foregrounds and the analyses are entirely independent, this constitutes a confirmation of the COBE/DMR discovery (Smoot et al., 1992). We show new work and present some details of the FIRS analysis to help explain and reinforce this result. 2) The FIRS autocorrelation function is presented. FIRS alone also detects an anisotropy. Three independent statistical methods have been applied to the data; all yield Q(rms-PS) = 19 mu K for a primordial power law given by P(k) proportional to k. C1 PRINCETON UNIV,DEPT PHYS,PRINCETON,NJ 08544. NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. UNIV CHICAGO,DEPT PHYS,CHICAGO,IL 60637. NR 12 TC 1 Z9 1 U1 0 U2 0 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 32 IS 1-6 BP 239 EP 247 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU782 UT WOS:A1995VU78200030 ER PT J AU Kowitt, MS Cheng, ES Cottingham, DA Farooqui, K Fixsen, DJ Ganga, K Inman, CA Meyer, SS Page, LA Piccirillo, L Puchalla, JL Ruhl, J Schaefer, RK Silverberg, RF Timbie, PT Wilson, G Zhou, JW AF Kowitt, MS Cheng, ES Cottingham, DA Farooqui, K Fixsen, DJ Ganga, K Inman, CA Meyer, SS Page, LA Piccirillo, L Puchalla, JL Ruhl, J Schaefer, RK Silverberg, RF Timbie, PT Wilson, G Zhou, JW TI The MSAM/TopHat program of anisotropy measurements SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article ID DIFFERENTIAL MICROWAVE RADIOMETER; BACKGROUND-RADIATION; SCALE ANISOTROPY; 1ST-YEAR MAPS; BOLOMETERS; WAVELENGTH AB We describe a series of three complementary balloon-borne experiments to measure the Cosmic Microwave Background Radiation (CMBR) anisotropy on angular scales from 0.5 degrees to 180 degrees between 65 and 700 GHz. At the largest angular scales, we plan to finish mapping the entire sky from 150 to 690 GHz with 3.8 degrees resolution and sensitivity comparable to the COBE/DMR first year maps. The analysis of the first flight of this Far-Infrared Survey (FIRS) led to the confirmation of the COBE anisotropy discovery (Ganga et al., 1993). On smaller angular scales, we will upgrade our pointing telescope and refly the 0.5 degrees resolution Medium-Scale Anisotropy Measurement (MSAM) using the existing 150 to 690 GHz four-band radiometer, observing the same field as our previous flight, strengthening those results (Cheng el al., 1994). Two subsequent flights of this telescope with a new 65 to 170 GHz multi-band radiometer (MSAM II) will re-observed this same patch of sky to check that the results are not contaminated by foreground radiation. Concurrent with the above program, we will implement a new concept in CMBR measurement to provide the next step in observational capabilities. This experiment, named TopHat, will be mounted on the top of a balloon and will observe for two weeks in circumpolar flight from McMurdo Station, Antarctica. By providing a combination of reduced systematics and extended integration time, it offers a factor of 30 improvement in sensitivity to CMBR anisotropy over existing measurements. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. GLOBAL SCI & TECHNOL INC,GREENBELT,MD 20771. BROWN UNIV,DEPT PHYS,PROVIDENCE,RI 02912. APPL RES CORP,GREENBELT,MD 20771. PRINCETON UNIV,DEPT PHYS,PRINCETON,NJ 08544. UNIV CHICAGO,ENRICO FERMI INST,CHICAGO,IL 60637. UNIV CHICAGO,DEPT ASTRON & ASTROPHYS,CHICAGO,IL 60637. UNIV DELAWARE,BARTOL RES INST,NEWARK,DE 19716. RI Schaefer, Robert/C-2119-2016 OI Schaefer, Robert/0000-0003-3692-0223 NR 24 TC 7 Z9 7 U1 0 U2 0 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 32 IS 1-6 BP 273 EP 281 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU782 UT WOS:A1995VU78200034 ER PT J AU Janssen, MA Lawrence, CR AF Janssen, MA Lawrence, CR TI Primordial structure investigation (PSI): A low-cost space mission to image the intermediate-scale cosmic background anisotropy SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article DE cosmic microwave background AB Preliminary results are presented for the Primordial Structure Investigation mission study. PSI is a concept for a high-sensitivity, low-cost mission to image the Cosmic Microwave Background on intermediate angular-scales (0.5 degrees-10 degrees). The mission objective is to measure the anisotropy of the CMB with sufficient sensitivity, and over a large enough solid angle, to unlock the wealth of evidence that the anisotropy holds for the origin of structure and the nature of the universe. PSI consists of an 80-cm aperture fed by 32 radiometers (eight at each of four frequencies), carried into heliocentric orbit on a spinning spacecraft. Total power radiometers, based on current HEMT (High Electron Mobility Transistor) and MMIC (Monolothic Microwave Integrated Circuit) technologies, provide low noise, stable gain, and low power dissipation to allow passive cooling. The spacecraft is constrained to fit the projected launch capabilities of a Taurus vehicle, has a mass of 213 kg, consumes 230 W, and is designed for a 5-year lifetime. The mission will image similar to 10(3) pixels to a sensitivity of 1 mu K, or similar to 10(4) pixels to a sensitivity of 3 mu K, at each frequency. This study supports the feasibility of a low-cost space approach to the problem of determining the intermediate angular-scale anisotropies. Costing of our baseline design has not been completed, but we anticipate a mission within the guidelines of the anticipated NASA Mid-sized Explorer Program. However, further work is needed in the areas of HEMT development and characterization, optics design, and the multi-frequency strategy for the removal of galactic foreground emission to fully justify the present concept. C1 CALTECH,JET PROP LAB,PASADENA,CA. NR 5 TC 2 Z9 2 U1 0 U2 0 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 32 IS 1-6 BP 289 EP 296 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU782 UT WOS:A1995VU78200036 ER PT J AU Smoot, GF Mandolesi, N Bersanelli, M Cesarsky, C LachiezeRey, M Danese, L Vittorio, N DeBernardis, P Dalloglio, G Sironi, G Crane, P Janssen, M Partridge, B Beckman, J Rebolo, R Puget, JL Bussoletti, E Raffelt, G Davies, R Encrenaz, P Natale, V Tofani, G Merluzzi, P Toffolatti, L Scaramella, R MartinezGonzales, E Saez, D Lasenby, A Kogut, A Efstathiou, G AF Smoot, GF Mandolesi, N Bersanelli, M Cesarsky, C LachiezeRey, M Danese, L Vittorio, N DeBernardis, P Dalloglio, G Sironi, G Crane, P Janssen, M Partridge, B Beckman, J Rebolo, R Puget, JL Bussoletti, E Raffelt, G Davies, R Encrenaz, P Natale, V Tofani, G Merluzzi, P Toffolatti, L Scaramella, R MartinezGonzales, E Saez, D Lasenby, A Kogut, A Efstathiou, G TI COBRAS: A space mission for mapping the CMB structure at 0.5 degrees resolution SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article DE cosmic background radiation; satellite; anisotropy AB We describe the mission concept of the COBRAS (Cosmic Background Radiation Anisotropy Satellite) mission. The primary goal is to map the CBR anisotropy with an angular resolution of 0.5 degrees and with a sensitivity of Delta T/T approximate to 10(-6). The proposed mission requires a special orbit, preferably far from earth, and good shielding as well as current state-of-the-art receiver technology. COBRAS will find the signatures of structure formation in a mission combining full sky coverage with a few deep scans covering about 10% of the sky. C1 UNIV CALIF BERKELEY,LAWRENCE BERKELEY LAB,BERKELEY,CA 94720. CNR,IST TESRE,I-40126 BOLOGNA,ITALY. CNR,IFCTR,I-20133 MILAN,ITALY. CEN,CEA,SAP,SACLAY,FRANCE. UNIV PADUA,DIPARTIMENTO ASTRON,I-35122 PADUA,ITALY. UNIV ROMA TOR VERGATA,DIPARTIMENTO FIS,I-00173 ROME,ITALY. UNIV ROMA LA SAPIENZA,DIPARTIMENTO FIS,I-00185 ROME,ITALY. UNIV MILAN,DIPARTIMENTO FIS,MILAN,ITALY. EUROPEAN SO OBSERV,D-8046 GARCHING,GERMANY. CALTECH,JET PROP LAB,PASADENA,CA. HAVERFORD COLL,HAVERFORD,PA 19041. INST ASTROFIS CANARIAS,TENERIFE,SPAIN. UNIV PARIS 11,IAS,ORSAY,FRANCE. IST UNIV NAVALE,NAPLES,ITALY. MAX PLANCK INST PHYS & ASTROPHYS,D-80805 MUNICH,GERMANY. OBSERV MEUDON,F-92195 MEUDON,FRANCE. CNR,OSSERVATORIO ASTROFIS ARCETRI,CAISMA,I-00185 ROME,ITALY. OSSERV ASTRON CAPODIMONTE,I-80131 NAPLES,ITALY. OSSERV ASTRON PADOVA,PADUA,ITALY. OSSERV ASTRON ROMA,I-00136 ROME,ITALY. UNIV VALENCIA,VALENCIA,SPAIN. UNIV CAMBRIDGE,CAMBRIDGE CB2 1TN,ENGLAND. UNIV OXFORD,OXFORD,ENGLAND. RI Kogut, Alan/D-6293-2012; Toffolatti, Luigi/K-5070-2014 OI Toffolatti, Luigi/0000-0003-2645-7386 NR 11 TC 3 Z9 3 U1 0 U2 0 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 32 IS 1-6 BP 297 EP 308 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU782 UT WOS:A1995VU78200037 ER PT J AU Mandolesi, N Smoot, GF Bersanelli, M Cesarsky, C LachiezeRey, M Danese, L Vittorio, N DeBernardis, P Dalloglio, G Sironi, G Crane, P Janssen, M Partridge, B Beckman, J Rebolo, R Puget, JL Bussoletti, E Raffelt, G Davies, R Encrenaz, P Natale, V Tofani, G Merluzzi, P Toffolatti, L Scaramella, R MartinezGonzales, E Saez, D Lasenby, A Efstathiou, G AF Mandolesi, N Smoot, GF Bersanelli, M Cesarsky, C LachiezeRey, M Danese, L Vittorio, N DeBernardis, P Dalloglio, G Sironi, G Crane, P Janssen, M Partridge, B Beckman, J Rebolo, R Puget, JL Bussoletti, E Raffelt, G Davies, R Encrenaz, P Natale, V Tofani, G Merluzzi, P Toffolatti, L Scaramella, R MartinezGonzales, E Saez, D Lasenby, A Efstathiou, G TI COBRAS: Goal and experimental approach SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article DE cosmology; cosmic microwave background ID TRANSISTORS AB We present the primary observational goal of the COBRAS mission and discuss the relative advantages of radiometric and bolometric techniques. A preliminary payload concept is presented. The COBRAS instrument and payload characteristics are based on a multifrequency observation in the < 130 GHz regime and are described here in some detail. Alternatives and additions, including a possible extension to higher frequencies, are considered. C1 CNR,ITESRE,I-40129 BOLOGNA,ITALY. UNIV CALIF BERKELEY,LAWRENCE BERKELEY LAB,BERKELEY,CA 94720. CNR,IFCTR,I-20133 MILAN,ITALY. CEN,CEASAP,SACLAY,FRANCE. UNIV PADUA,DIPARTIMENTO ASTRON,I-35122 PADUA,ITALY. UNIV ROMA TOR VERGATA,DIPARTIMENTO FIS,I-00173 ROME,ITALY. UNIV ROMA LA SAPIENZA,DIPARTIMENTO FIS,I-00185 ROME,ITALY. UNIV MILAN,DIPARTIMENTO FIS,MILAN,ITALY. EUROPEAN SO OBSERV,D-8046 GARCHING,GERMANY. CALTECH,JET PROP LAB,PASADENA,CA. HAVERFORD COLL,HAVERFORD,PA 19041. INST ASTROFIS CANARIAS,TENERIFE,SPAIN. UNIV PARIS 11,IAS,ORSAY,FRANCE. IST UNIV NAVALE,NAPLES,ITALY. MAX PLANCK INST PHYS & ASTROPHYS,D-80805 MUNICH,GERMANY. OBSERV MEUDON,F-92195 MEUDON,FRANCE. CNR,OSSERVATORIO ASTROFIS ARCETRI,CAISMI,I-00185 ROME,ITALY. OSSERV ASTRON CAPODIMONTE,I-80131 NAPLES,ITALY. OSSERV ASTRON PADOVA,PADUA,ITALY. OSSERV ASTRON ROMA,I-00136 ROME,ITALY. UNIV VALENCIA,VALENCIA,SPAIN. UNIV CAMBRIDGE,CAMBRIDGE CB2 1TN,ENGLAND. UNIV OXFORD,OXFORD,ENGLAND. RI Toffolatti, Luigi/K-5070-2014 OI Toffolatti, Luigi/0000-0003-2645-7386 NR 12 TC 3 Z9 3 U1 0 U2 0 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 32 IS 1-6 BP 309 EP 318 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA VU782 UT WOS:A1995VU78200038 ER PT J AU CORWIN, HG HELOU, G MADORE, BF SCHMITZ, M BENNETT, J WU, X LAGUE, C SUN, H AF CORWIN, HG HELOU, G MADORE, BF SCHMITZ, M BENNETT, J WU, X LAGUE, C SUN, H TI THE NASA IPAC EXTRAGALACTIC DATABASE - A STATUS-REPORT SO ASTROPHYSICAL LETTERS & COMMUNICATIONS LA English DT Article; Proceedings Paper CT World of Galaxies II Meeting CY SEP 05-07, 1994 CL LYON, FRANCE SP LYON MEUDON EXTRAGAKACT DATABASE, OBSERV LYON, CNRS, REG RHONE ALPES, RELAT INT UNIV CLAUDE BERNARD, MAIRIE SAINT GENIS LAVAL, ECOLE NOMALE SUPER LYON, OFF TOURISME VILLE LYON DE GALAXIES; ONLINE CATALOGS; ASTROMETRY AB The NASA/IPAC Extragalactic Database (NED) has been in operation since June of 1990. NED's ''object-oriented'' architecture, based on the merger of many catalogues of extragalactic objects, has been discussed at previous conferences (e.g. Helou et al. 1991 and Schmitz et al. 1994), so we shall give only a brief summary of it here. We shall instead concentrate on some of the cataloguing issues that we have had to deal with, especially astrometry of galaxies. RP CORWIN, HG (reprint author), CALTECH,JET PROP LAB,CTR INFRARED PROC & ANAL,4800 OAK GROVE DR,PASADENA,CA 91125, USA. NR 8 TC 1 Z9 1 U1 0 U2 0 PU GORDON BREACH SCI PUBL LTD PI READING PA C/O STBS LTD PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0888-6512 J9 ASTROPHYS LETT COMM JI Astrophys. Lett. Comm. PY 1995 VL 31 IS 1-6 BP 9 EP 12 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QX914 UT WOS:A1995QX91400003 ER PT J AU SHAO, M AF SHAO, M TI PROSPECTS FOR GROUND-BASED INTERFEROMETRIC ASTROMETRY SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article; Proceedings Paper CT 2nd International Conference on Planetary Systems: Formation, Evolution and Detection CY DEC 13-15, 1993 CL WAIKOLA, HI SP NASA ID ATMOSPHERIC LIMITATIONS RP SHAO, M (reprint author), CALTECH,JET PROPULS LAB,PASADENA,CA 91109, USA. NR 5 TC 7 Z9 7 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA SPUIBOULEVARD 50, PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD JAN PY 1995 VL 223 IS 1-2 BP 119 EP 121 DI 10.1007/BF00989163 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA QQ536 UT WOS:A1995QQ53600017 ER PT S AU DGANI, R AF DGANI, R BE Harpaz, A Soker, N TI Planetary nebulae - Interstellar medium interaction: Theory review SO ASYMMETRICAL PLANETARY NEBULAE SE ANNALS OF THE ISRAEL PHYSICAL SOCIETY LA English DT Proceedings Paper CT Conference on Asymmetrical Planetary Nebulae CY AUG 07-11, 1994 CL ORANIM, HAIFA UNIV, HAIFA, ISRAEL HO ORANIM, HAIFA UNIV C1 CALTECH,JET PROP LAB,CTR INFRARED PROC & ANAL,PASADENA,CA 91109. NR 0 TC 6 Z9 6 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TECHNO HOUSE, REDCLIFFE WAY, BRISTOL, ENGLAND BS1 6NX SN 0309-8710 BN 0-7503-0330-1 J9 ANN ISR PHY PY 1995 VL 11 BP 219 EP 228 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BD39M UT WOS:A1995BD39M00035 ER PT S AU BRACE, LH HARTLE, RE THEIS, RF AF BRACE, LH HARTLE, RE THEIS, RF BE Taylor, FW TI THE NIGHTWARD ION FLOW SCENARIO AT VENUS REVISITED SO ATMOSPHERES OF VENUS AND MARS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT C3.1 Meeting of COSPAR-Scientific-Commission-C, at the 13th COSPAR Scientific Assembly CY JUL 11-21, 1994 CL HAMBURG, GERMANY SP Comm Space Res, NASA, European Space Agcy ID NIGHTSIDE IONOSPHERE; MAGNETIC-FIELD; ELECTRON-TEMPERATURE; EMPIRICAL-MODELS; PLASMA MOTION; MAINTENANCE; TRANSPORT; IONOTAIL; DENSITY; CLOUDS AB In this paper, we indicate how existing Pioneer Venus Orbiter (PVO) data might be used to gain a better understanding of nightward ion flow in the Venusian ionosphere. Calculations based on PVO measurements made at solar maximum suggest that the global nightward flow of O+ may be significantly greater than is required to maintain the observed nightside ionosphere densities. The validity of this conclusion depends upon (1) the accuracy with which the flow can be determined from the PVO ion density and velocity measurements and (2) the validity of the ionosphere theory used to estimate the required downward O+ flux on the night side. If the measurements and theory are assumed to be accurate, the excess nightward flow implies a significant rate of ion escape from the planet, particularly at times of low solar wind dynamic pressure, Psw, when the ionopause rises to allow increased nightward flow. To illustrate a potentially important mechanism for ion escape from Venus, we present Orbiter Electron Temperature Probe (OETP) observations of plasma clouds and scavenged ionospheric plasma observed above the ionopause. We then employ OETP and Orbiter Retarding Potential Analyzer (ORPA) data to reexamine the global ion flow for average Psw conditions, and we find the net flow to be in agreement with previous estimates. We also find that the net transterminator flow at average Psw approaches the limiting upward ion flow available from the dayside ionosphere, a limit which is imposed by O+ collisions with O-2(+) OETP measurements in the terminator ionosphere show that N-e declines at times of low Psw. This suggests that the dayside ionosphere is unable to supply the increased demand when the ionopause rises above its average height, thus requiring an upward diversion of some of the nightward now to populate the overlying, newly-created ionosphere. We predict that the ion velocities will also be found to decrease at times of low Psw, in part due to the source-limited flow, and in part because the expansion of the ionosphere diminishes the ''nozzle effect'' that has been identified as a source of nightward ion acceleration. Collectively, these effects act to limit the increase in the net nightward ion now at times of low Psw. Since O+-O-2(+) collisions will impart an upward velocity to the O-2(+) ions, the O+ diffusion limit may be a soft one, so the nightward flow can continue to increase somewhat as Psw declines. The collision process should also enhance the O-2(+) concentration in the dayside upper ionosphere and, to the extent that the O-2(+) participates in the nightward flow, should produce O-2(+) enhancements on the night side as well. These expectations could be verified by an examination of the orbit-to-orbit changes in ion composition and velocity in response to Psw variations. C1 NASA,GODDARD SPACE FLIGHT CTR,ATMOSPHERES LAB,GREENBELT,MD 20771. RP BRACE, LH (reprint author), UNIV MICHIGAN,SPACE PHYS RES LAB,ANN ARBOR,MI 48109, USA. NR 44 TC 12 Z9 12 U1 0 U2 0 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0273-1177 BN 0-08-042626-3 J9 ADV SPACE RES PY 1995 VL 16 IS 6 BP 99 EP 112 DI 10.1016/0273-1177(95)00255-D PG 14 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA BD35E UT WOS:A1995BD35E00013 ER PT B AU Stolarski, RS McPeters, RD Gleason, JF AF Stolarski, RS McPeters, RD Gleason, JF BE Wang, WC Isaksen, ISA TI Ozone trends from satellite data SO ATMOSPHERIC OZONE AS A CLIMATE GAS: GENERAL CIRCULATION MODEL SIMULATIONS SE NATO ADVANCED SCIENCE INSTITUTE SERIES, SERIES I, GLOBAL ENVIRONMENT CHANGE LA English DT Proceedings Paper CT Advanced Study Institute on Atmospheric Ozone as a Climate Gas CY JUN 19-23, 1994 CL LILLEHAMMER, NORWAY SP NATO C1 NASA,GODDARD SPACE FLIGHT CTR 916,GREENBELT,MD 20771. RI Gleason, James/E-1421-2012; Stolarski, Richard/B-8499-2013; McPeters, Richard/G-4955-2013 OI Stolarski, Richard/0000-0001-8722-4012; McPeters, Richard/0000-0002-8926-8462 NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN 33 PA HEIDELBERGER PLATZ 3, W-1000 BERLIN 33, GERMANY BN 3-540-60009-4 J9 NATO ASI SER SER I PY 1995 VL 32 BP 397 EP 410 PG 14 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA BF12W UT WOS:A1995BF12W00024 ER PT B AU WILSON, KE BISWAS, A BLOOM, S CHAN, V AF WILSON, KE BISWAS, A BLOOM, S CHAN, V BE Dainty, JC TI Effect of aperture averaging on a 570 Mbps 42 km horizontal path optical link SO ATMOSPHERIC PROPAGATION AND REMOTE SENSING IV SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Atmospheric Propagation and Remote Sensing IV CY APR 17-19, 1995 CL ORLANDO, FL SP Soc Photo Opt Instrumentat Engineers C1 CALTECH,JET PROP LAB,PASADENA,CA 91125. NR 0 TC 1 Z9 1 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1824-2 J9 P SOC PHOTO-OPT INS PY 1995 VL 2471 BP 244 EP 253 DI 10.1117/12.211934 PG 10 WC Remote Sensing; Optics SC Remote Sensing; Optics GA BD53M UT WOS:A1995BD53M00025 ER PT J AU GULTEPE, I STARR, DO AF GULTEPE, I STARR, DO TI A COMPARISON OF EVAPORATIVE COOLING WITH INFRARED HEATING BENEATH A CIRRUS CLOUD SO ATMOSPHERIC RESEARCH LA English DT Article ID OCTOBER 1986 FIRE; LIDAR; EVOLUTION; CLIMATE AB Data for this study were collected by the instruments mounted on the NCAR King Air and rawinsonde during the First ISCCP (International Satellite Cloud Climatology Project) Regional Experiment (FIRE) on 19 October, 1986. The main purpose of this study is to understand the basic concept of evaporative cooling in a dry layer below a cirrus generating cell. Relative humidity with respect to liquid water RH(w) and temperature lapse rate gamma(e) below the cirrus base at about 6.7 km were about 40% and 3.7 degrees C km(-1), respectively. Evaporative cooling rate (ECR) in the 1.5 km thick subcloud layer was estimated to be approximately 0.1 to 2 degrees C h(-1) and it was found to be comparable with the infrared heating rate calculated from radiation measurements. Because of ice crystal evaporation, RH(w) in the same layer may reach saturation with respect to ice in 1.5 hours. RP GULTEPE, I (reprint author), NASA,GODDARD SPACE FLIGHT CTR,CODE 913,GREENBELT,MD 20771, USA. NR 22 TC 4 Z9 4 U1 0 U2 0 PU ELSEVIER SCIENCE PUBL CO INC PI NEW YORK PA 655 AVENUE OF THE AMERICAS, NEW YORK, NY 10010 SN 0169-8095 J9 ATMOS RES JI Atmos. Res. PD JAN PY 1995 VL 35 IS 2-4 BP 217 EP 231 DI 10.1016/0169-8095(94)00020-E PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA QM270 UT WOS:A1995QM27000010 ER PT B AU MISHCHENKO, MI TRAVIS, LD LACIS, AA CARLSON, BE AF MISHCHENKO, MI TRAVIS, LD LACIS, AA CARLSON, BE BE Santer, RP TI SATELLITE REMOTE SENSING OF NONSPHERICAL TROPOSPHERIC AEROSOLS SO ATMOSPHERIC SENSING AND MODELING SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Atmospheric Sensing and Modeling CY SEP 29-30, 1994 CL ROME, ITALY SP COMMISS EUROPEAN COMMUNITIES, DIRECTORATE GEN SCI RES & DEV, EUROPEAN OPT SOC, SOC PHOTO OPT INSTRUMENTAT ENGINEERS, CNR, ITALIAN ASSOC REMOTE SENSING C1 NASA,GODDARD INST SPACE STUDIES,HUGHES STX CORP,NEW YORK,NY 10025. RI Mishchenko, Michael/D-4426-2012 NR 0 TC 0 Z9 0 U1 0 U2 1 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1641-X J9 P SOC PHOTO-OPT INS PY 1995 VL 2311 BP 150 EP 161 PG 12 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BC28Y UT WOS:A1995BC28Y00016 ER PT B AU MCCORMICK, MP CHIOU, EW AF MCCORMICK, MP CHIOU, EW BE Santer, RP TI ANNUAL VARIATIONS OF WATER VAPOR IN THE STRATOSPHERE AND UPPER TROPOSPHERE BASED ON SAGE-II OBSERVATIONS DURING 1986-1991 SO ATMOSPHERIC SENSING AND MODELING SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Atmospheric Sensing and Modeling CY SEP 29-30, 1994 CL ROME, ITALY SP COMMISS EUROPEAN COMMUNITIES, DIRECTORATE GEN SCI RES & DEV, EUROPEAN OPT SOC, SOC PHOTO OPT INSTRUMENTAT ENGINEERS, CNR, ITALIAN ASSOC REMOTE SENSING C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23681. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1641-X J9 P SOC PHOTO-OPT INS PY 1995 VL 2311 BP 182 EP 189 PG 8 WC Meteorology & Atmospheric Sciences; Remote Sensing SC Meteorology & Atmospheric Sciences; Remote Sensing GA BC28Y UT WOS:A1995BC28Y00019 ER PT B AU Thomason, LW McCormick, MP Zawodny, JM AF Thomason, LW McCormick, MP Zawodny, JM BE Santer, RP TI The stratospheric aerosol and gas experiment III SO ATMOSPHERIC SENSING AND MODELING II SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Atmospheric Sensing and Modeling II CY SEP 27-28, 1995 CL PARIS, FRANCE SP CNES, NASA, CNR, EOS, Soc Photo Opt Instrumentat Engineers, Commiss European Communities, Directorate Gen Sci Res & Dev C1 NASA,LANGLEY RES CTR,DIV ATMOSPHER SCI,HAMPTON,VA 23681. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPIE - INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA PO BOX 10, BELLINGHAM, WA 98227-0010 BN 0-8194-1946-X J9 P SOC PHOTO-OPT INS PY 1995 VL 2582 BP 72 EP 79 DI 10.1117/12.228525 PG 8 WC Meteorology & Atmospheric Sciences; Remote Sensing; Optics SC Meteorology & Atmospheric Sciences; Remote Sensing; Optics GA BE76S UT WOS:A1995BE76S00007 ER PT S AU MLYNCZAK, MG AF MLYNCZAK, MG BE Shepherd, GG Skinner, WR Thrane, E Chakrabarty, DK Lubken, FJ Blix, T Kliore, AJ Keating, GM TI ENERGETICS OF THE MIDDLE ATMOSPHERE - THEORY AND OBSERVATION REQUIREMENTS SO ATMOSPHERIC STUDIES OF EARTH, VENUS AND MARS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT C1.1, C2.3, C2.2 Meetings and C2.1, C2 Symposiums of COSPAR Scientific Commission C, at the 13th COSPAR Scientific Assembly CY JUL 11-21, 1994 CL HAMBURG, GERMANY SP Comm Space Res ID RADIATIVE-TRANSFER MODEL; INFRARED LIMB EMISSION; MU-M BANDS; LOWER THERMOSPHERE; THERMODYNAMIC-EQUILIBRIUM; MESOSPHERIC OZONE; CARBON-DIOXIDE; EFFICIENCY; MESOPAUSE; HYDROGEN AB This paper presents an overview of the significant advances which have been made over the past three years in the understanding of the energy budget of the mesosphere and lower thermosphere. Recent calculations of key heat source terms are presented and compared. Observation requirements to further the understanding are also presented. In particular, the ozone concentration is shown to be of considerable importance to the mesospheric heat budget through absorption of solar ultraviolet radiation and participation in exothermic reactions. Two techniques by which ozone may be determined from space-based instruments employing infrared emission sensing are also reviewed and compared. Very accurate knowledge of the departure from local thermodynamic equilibrium in the observed emission features is required to reliably determine the ozone concentration. RP MLYNCZAK, MG (reprint author), NASA,LANGLEY RES CTR,MAIL STOP 401B,HAMPTON,VA 23681, USA. RI Mlynczak, Martin/K-3396-2012 NR 34 TC 17 Z9 17 U1 0 U2 0 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0273-1177 BN 0-08-042660-3 J9 ADV SPACE RES PY 1995 VL 17 IS 11 BP 117 EP 126 DI 10.1016/0273-1177(95)00739-2 PG 10 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA BE07R UT WOS:A1995BE07R00016 ER PT S AU BRACE, LH THEIS, RF AF BRACE, LH THEIS, RF BE Shepherd, GG Skinner, WR Thrane, E Chakrabarty, DK Lubken, FJ Blix, T Kliore, AJ Keating, GM TI AN EXTENSION OF THE VIRA ELECTRON-TEMPERATURE AND DENSITY MODELS TO INCLUDE SOLAR-CYCLE VARIATIONS SO ATMOSPHERIC STUDIES OF EARTH, VENUS AND MARS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT C1.1, C2.3, C2.2 Meetings and C2.1, C2 Symposiums of COSPAR Scientific Commission C, at the 13th COSPAR Scientific Assembly CY JUL 11-21, 1994 CL HAMBURG, GERMANY SP Comm Space Res ID VENUS IONOSPHERE; NIGHTSIDE IONOSPHERE; MAINTENANCE; EUV AB The original VIRA ionosphere model was based primarily on the Pioneer Venus Orbiter (PVO) data obtained at solar maximum (F10.7-200) in 1979 and 1980 when periapsis was being maintained deep in the Venusian ionosphere. In situ measurements provided data on temperature, composition, density, and drift velocity, while the radio occultation method provided height profiles of electron density, N-e. The solar cycle variation was deduced by comparison with the Venera 9 and 10 occultation data from the previous solar minimum. No data were available on the solar cycle variations of other ionospheric parameters, because periapsis had already risen out of the ionosphere by the time solar activity began to decline early in 1983. During the Entry period in the Fall of 1992, however, PVO got a brief glimpse of the nightside ionosphere at lower solar activity (F10.7-120). During the intervening decade important in situ data were obtained on the upper nightside ionosphere that extends far down stream from the planet. This region was found to be highly sensitive to solar wind interactions and solar activity. In this paper, we discuss ways in which the later PVO data can be used to extend the VIRA model to higher altitudes and to include the solar cycle variations. As an example, we present some pre-entry Orbiter Electron Temperature Probe measurements that provide new clues as to the dayside T-e behavior at low solar activity. C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. RP BRACE, LH (reprint author), MICROBIOL UNIT,SPACE PHYS RES LAB,ANN ARBOR,MI 48109, USA. NR 17 TC 1 Z9 1 U1 1 U2 1 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0273-1177 BN 0-08-042660-3 J9 ADV SPACE RES PY 1995 VL 17 IS 11 BP 181 EP 190 PG 10 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA BE07R UT WOS:A1995BE07R00025 ER PT S AU GREBOWSKY, JM KASPRZAK, WT HARTLE, RE DONAHUE, TM AF GREBOWSKY, JM KASPRZAK, WT HARTLE, RE DONAHUE, TM BE Shepherd, GG Skinner, WR Thrane, E Chakrabarty, DK Lubken, FJ Blix, T Kliore, AJ Keating, GM TI A NEW LOOK AT VENUS THERMOSPHERE H DISTRIBUTION SO ATMOSPHERIC STUDIES OF EARTH, VENUS AND MARS SE ADVANCES IN SPACE RESEARCH LA English DT Article; Proceedings Paper CT C1.1, C2.3, C2.2 Meetings and C2.1, C2 Symposiums of COSPAR Scientific Commission C, at the 13th COSPAR Scientific Assembly CY JUL 11-21, 1994 CL HAMBURG, GERMANY SP Comm Space Res AB Pioneer Venus Orbiter measurements in the ionosphere, at low altitudes in 1978-1980 and from the entry phase of the mission in late 1992, are used to determine the neutral H concentrations, on an orbit by orbit basis, in the altitude region where H+ is in chemical equilibrium. The chemical equilibrium region is selected based on the characteristic chemical and diffusion times for each measurement, This results in a dataset of H concentrations at Venus from in situ measurements covering all local times and diverse solar activity conditions. A comparison of H with He measurements shows parallel local time behavior. The H concentrations in the bulge region may have a slight inverse correlation with F10.7, whereas the He bulge data(from ONMS) near 175 km do not. C1 UNIV MICHIGAN,ANN ARBOR,MI 48109. RP GREBOWSKY, JM (reprint author), NASA,GODDARD SPACE FLIGHT CTR,CODE 914,GREENBELT,MD 20771, USA. RI Grebowsky, Joseph/I-7185-2013 NR 7 TC 9 Z9 9 U1 0 U2 0 PU PERGAMON PRESS LTD PI OXFORD PA THE BOULEVARD LANGFORD LANE KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0273-1177 BN 0-08-042660-3 J9 ADV SPACE RES PY 1995 VL 17 IS 11 BP 191 EP 195 PG 5 WC Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Geology; Meteorology & Atmospheric Sciences GA BE07R UT WOS:A1995BE07R00026 ER PT S AU KALLMAN, TR AF KALLMAN, TR BE Rowan, WL TI X-RAY DIAGNOSTICS OF COSMIC PHOTOIONIZED PLASMAS SO ATOMIC PROCESSES IN PLASMAS SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 9th American-Physical-Society Topical Conference on Atomic Processes in Plasmas CY SEP 19-23, 1993 CL SAN ANTONIO, TX SP AMER PHYS SOC C1 NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-411-2 J9 AIP CONF PROC PY 1995 IS 322 BP 36 EP 52 PG 17 WC Physics, Atomic, Molecular & Chemical; Physics, Particles & Fields; Spectroscopy SC Physics; Spectroscopy GA BC84N UT WOS:A1995BC84N00004 ER PT J AU BELLAN, J HARSTAD, K AF BELLAN, J HARSTAD, K TI STEADY INJECTION OF IDENTICAL CLUSTERS OF EVAPORATING DROPS EMBEDDED IN JET VORTICES SO ATOMIZATION AND SPRAYS LA English DT Article ID PARTICLE DISPERSION; MIXING LAYER; TURBULENT AB A model has been developed that describes the evaporation of clusters of drops in a flowing gaseous jet. Each one of these clusters is embedded into a coherent vortex and the drops evaporate as the clusters convect downstream together with the vortex. Because there is a continuous injection of clusters, each cluster represents in fact a statistical average of clusters at that particular location. Thus, the formulation contains a conservation equation for the cluster number density, conservation equations for the gas in the jet, and conservation equations for the drops in the cluster and the vortex containing the cluster. The cluster and vortex models are coupled to the gaseous jet model through boundary conditions. The heat necessary to evaporate the drops comes from the surroundings of the gaseous jet, and this is described through a global, diffusive entrainment model. It is assumed that the turbulent diffusion coefficient is proportional either to the local vortex strength or to the cluster velocity and the multiplier is named the entrainment coefficient. Results are presented here for the stationary case representing the situation when identical clusters are continuously injected and the injection rate is constant. Thus, if a ''snapshot'' of the calculation is taken at any time, the cluster is observed at that time and the clusters in its wake represent the history of the cluster at previous times. parametric studies cover the influence of the initial air/fuel mass ratio, the entrainment coefficient, and the initial drop and gas velocities inside the vortices. The results show that quantitative predictions of the evaporation time, the penetration of the clusters into the ambient, and the temperature of the jet depend on details of the entrainment of hot gas into the jet. RP BELLAN, J (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 15 TC 13 Z9 13 U1 0 U2 0 PU BEGELL HOUSE INC PI NEW YORK PA 79 MADISON AVE, STE 1202, NEW YORK, NY 10016-7892 SN 1044-5110 J9 ATOMIZATION SPRAY JI Atom. Sprays PD JAN-FEB PY 1995 VL 5 IS 1 BP 1 EP 16 PG 16 WC Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA RB989 UT WOS:A1995RB98900001 ER PT J AU BELLAN, J HARSTAD, K AF BELLAN, J HARSTAD, K TI UNSTEADY INJECTION OF SEQUENCES OF DROP CLUSTERS IN VORTICES DEPICTING PORTIONS OF A SPRAY SO ATOMIZATION AND SPRAYS LA English DT Article ID TURBULENT; PLANE; LAYER AB A model of unsteady injection of sequences of drop clusters embedded in jet vortices was applied to describe both vortices in the shear layer of a spray and small-scale vortical structures in the core of a spray. In the first case, the vortices are large compared to the size of the spray, they rotate fast with respect to the injection rate, and their number per area of spray is small. In the second case, the vortices are small compared to the size of the spray, they rotate slowly with respect to the injection rate, and their number per area of spray is large. Results were obtained for injection sequences where either the drop size or the air/fuel mass ratio varied from cluster to cluster in the injection sequence. The variation was a monotonic increase, a monotonic decrease, or a sinusoidal variation. The results thus obtained were compared to baseline results from steady-state calculations. Additionally, both the entrainment from the ambient into the jet and the initial number of clusters per jet area were varied so as to ascertain their influence on cluster penetration and jet properties. The results show that penetration of a cluster into the ambient is a function of the characteristics of the cluster sequence following the cluster, that the jet temperature is controlled by entrainment from the ambient into the jet in the shear-layer application whereas conduction also becomes important in the spray-core application, and that the fuel mass fraction in the jet is a function of the initial characteristics of the clusters as well as entrainment. RP BELLAN, J (reprint author), CALTECH,JET PROP LAB,4800 OAK GROVE DR,PASADENA,CA 91109, USA. NR 16 TC 4 Z9 4 U1 0 U2 0 PU BEGELL HOUSE INC PI NEW YORK PA 79 MADISON AVE, STE 1202, NEW YORK, NY 10016-7892 SN 1044-5110 J9 ATOMIZATION SPRAY JI Atom. Sprays PD JAN-FEB PY 1995 VL 5 IS 1 BP 17 EP 44 PG 28 WC Engineering, Multidisciplinary; Engineering, Chemical; Engineering, Mechanical; Materials Science, Multidisciplinary; Physics, Applied SC Engineering; Materials Science; Physics GA RB989 UT WOS:A1995RB98900002 ER PT S AU DAVIS, WL MCKAY, CP AF DAVIS, WL MCKAY, CP BE Haubold, HJ Onuora, LI TI LIQUID WATER ON EARLY MARS SO BASIC SPACE SCIENCE SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT 3rd United-Nations/European-Space-Agency Workshop on Basic Space Science CY OCT 18-22, 1993 CL LAGOS, NIGERIA SP UN, EUROPEAN SPACE AGCY, GERMAN SPACE AGENCY, INT CTR THEORET PHYS, NASA, PLANETARY SOC C1 NASA,AMES RES CTR,DIV SPACE SCI,MOFFETT FIELD,CA 94035. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AIP PRESS PI WOODBURY PA AMERICAN INSTITUTE OF PHYSICS 500 SUNNYSIDE BOULEVARD, WOODBURY, NY 11797-2999 SN 0094-243X BN 1-56396-328-0 J9 AIP CONF PROC PY 1995 IS 320 BP 75 EP 85 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BC86K UT WOS:A1995BC86K00009 ER PT S AU Schwarcz, D KeskiKuha, RAM AF Schwarcz, D KeskiKuha, RAM BE Jacobson, DC Luzzi, DE Heinz, TF Iwaki, M TI Degradation in EUV reflectance of ion-sputtered SiC films SO BEAM-SOLID INTERACTIONS FOR MATERIALS SYNTHESIS AND CHARACTERIZATION SE MATERIALS RESEARCH SOCIETY SYMPOSIUM PROCEEDINGS LA English DT Proceedings Paper CT Symposium on Beam-Solid Interactions for Materials Synthesis and Characterization, at the 1994 MRS Fall Meeting CY NOV 28-DEC 02, 1994 CL BOSTON, MA SP MRS C1 NASA,GODDARD SPACE FLIGHT CTR,GREENBELT,MD 20771. NR 0 TC 9 Z9 9 U1 0 U2 1 PU MATERIALS RESEARCH SOC PI PITTSBURGH PA 9800 MCKNIGHT RD, SUITE 327, PITTSBURGH, PA 15237 SN 0272-9172 BN 1-55899-255-3 J9 MATER RES SOC SYMP P PY 1995 VL 354 BP 535 EP 540 PG 6 WC Materials Science, Characterization & Testing SC Materials Science GA BE68S UT WOS:A1995BE68S00080 ER PT J AU KOENIG, DW MISHRA, SK PIERSON, DL AF KOENIG, DW MISHRA, SK PIERSON, DL TI REMOVAL OF BURKHOLDERIA-CEPACIA BIOFILMS WITH OXIDANTS SO BIOFOULING LA English DT Article DE SPACECRAFT; BIOFILMS; OXIDANTS; BIOFILM TREATMENT; BURKHOLDERIA (PSEUDOMONAS) CEPACIA ID BACTERIA AB Iodine is used to disinfect the water system aboard US space shuttles and is the anticipated biocide for the international space station. Water quality on spacecraft must be maintained at the highest possible levels for the safety of the crew. Furthermore, the treatment process used to maintain the quality of water on spacecraft must be robust and operate for long periods with minimal crew intervention. Biofilms are recalcitrant and pose a major threat with regard to chronic contamination of spacecraft water systems, We measured the effectiveness of oxidizing biocides on the removal and regrowth of Burkholderia (Pseudomonas) cepacia biofilms. B. cepacia, isolated from the water distribution system of the space shuttle Discovery was grown in continuous culture to produce a bacterial contamination source for biofilm formation and removal studies, A 10(7) CFU . ml(-1) B. cepacia suspension, in distilled water, was used to form biofilms on 3000 mu m(2) glass surfaces. Rates of attachment were measured directly with image analysis and were found to be 7.8, 15.2, and 22.8 attachment events . h(-1) for flow rates of 20.7, 15.2, and 9.8 ml . min(-1), respectively. After 18 h of formation, the B. cepacia biofilms were challenged with oxidants (ozone, chlorine, and iodine) and the rates of biofilm removal determined by image analysis. Fifty percent of the biofilm material was removed in the first hour of continuous treatment with 24 mg . l(-1) chlorine or 2 mg . l(-1) ozone. Iodine (48 mg . l(-1)) did not remove any measurable cellular material after 6 h continuous contact. After this first removal of biofilms by the oxidants. the surface was allowed to refoul and was again treated with the biocide. Iodine was the only compound that was unable to remove cellular debris from either primary or secondary biofilms. Moreover, treating primary biofilms with iodine increased the rate of formation of secondary biofilms, from 4.4 to 5.8 attachment events . h(-1). Ail the oxidants tested inactivated the B. cepacia associated with both primary and secondary biofilms. The amount of biocide needed to inactivate 50% of planktonic B. cepacia in 10 min at 25 degrees C was 8.4, 0.5, and 0.2 mg . l(-1) for iodine, chlorine, and ozone, respectively. The data suggest that iodine may not be the best chemical for treating of biofilms when removal of cellular material is required. C1 NASA,LYNDON B JOHNSON SPACE CTR,BIOMED OPERAT & RES BRANCH,HOUSTON,TX 77058. RP KOENIG, DW (reprint author), NASA,LYNDON B JOHNSON SPACE CTR,KRUG LIFE SCI,MAIL CODE SD4,HOUSTON,TX 77058, USA. NR 21 TC 9 Z9 9 U1 0 U2 2 PU HARWOOD ACAD PUBL GMBH PI READING PA C/O STBS LTD, PO BOX 90, READING, BERKS, ENGLAND RG1 8JL SN 0892-7014 J9 BIOFOULING JI Biofouling PY 1995 VL 9 IS 1 BP 51 EP 62 PG 12 WC Biotechnology & Applied Microbiology; Marine & Freshwater Biology SC Biotechnology & Applied Microbiology; Marine & Freshwater Biology GA TA686 UT WOS:A1995TA68600005 PM 11541193 ER PT S AU Kolb, EW Abney, M Copeland, EJ Liddle, AR Lidsey, JE AF Kolb, EW Abney, M Copeland, EJ Liddle, AR Lidsey, JE BE Occhionero, F TI The potential of potential reconstruction SO BIRTH OF THE UNIVERSE AND FUNDAMENTAL PHYSICS SE LECTURE NOTES IN PHYSICS LA English DT Proceedings Paper CT International Workshop on the Birth of the Universe and Fundamental Physics CY MAY 18-21, 1994 CL ROME, ITALY SP Comune Roma, European Astron Soc, European Phys Soc, Accad Nazl Lincei, Italian Soc Gen Rel & Gravit, Consiglio Nazl Ric, Ist Nazl Fis Nucl, European Space Agcy, Banca Nazl Lavoro C1 FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN 33 PA HEIDELBERGER PLATZ 3, W-1000 BERLIN 33, GERMANY SN 0075-8450 BN 3-540-60024-8 J9 LECT NOTES PHYS PY 1995 VL 455 BP 35 EP 44 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA BE87S UT WOS:A1995BE87S00005 ER PT S AU Lidsey, JE AF Lidsey, JE BE Occhionero, F TI Inflation and gravitational waves SO BIRTH OF THE UNIVERSE AND FUNDAMENTAL PHYSICS SE LECTURE NOTES IN PHYSICS LA English DT Proceedings Paper CT International Workshop on the Birth of the Universe and Fundamental Physics CY MAY 18-21, 1994 CL ROME, ITALY SP Comune Roma, European Astron Soc, European Phys Soc, Accad Nazl Lincei, Italian Soc Gen Rel & Gravit, Consiglio Nazl Ric, Ist Nazl Fis Nucl, European Space Agcy, Banca Nazl Lavoro C1 FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN 33 PA HEIDELBERGER PLATZ 3, W-1000 BERLIN 33, GERMANY SN 0075-8450 BN 3-540-60024-8 J9 LECT NOTES PHYS PY 1995 VL 455 BP 53 EP 60 PG 8 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA BE87S UT WOS:A1995BE87S00007 ER PT S AU Mather, JC AF Mather, JC BE Occhionero, F TI COBE observations of the big bang SO BIRTH OF THE UNIVERSE AND FUNDAMENTAL PHYSICS SE LECTURE NOTES IN PHYSICS LA English DT Proceedings Paper CT International Workshop on the Birth of the Universe and Fundamental Physics CY MAY 18-21, 1994 CL ROME, ITALY SP Comune Roma, European Astron Soc, European Phys Soc, Accad Nazl Lincei, Italian Soc Gen Rel & Gravit, Consiglio Nazl Ric, Ist Nazl Fis Nucl, European Space Agcy, Banca Nazl Lavoro C1 NASA,GODDARD SPACE FLIGHT CTR,ASTRON & SOLAR PHYS LAB,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN 33 PA HEIDELBERGER PLATZ 3, W-1000 BERLIN 33, GERMANY SN 0075-8450 BN 3-540-60024-8 J9 LECT NOTES PHYS PY 1995 VL 455 BP 235 EP 242 PG 8 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA BE87S UT WOS:A1995BE87S00040 ER PT S AU Amendola, L AF Amendola, L BE Occhionero, F TI Beyond the central limit theorem SO BIRTH OF THE UNIVERSE AND FUNDAMENTAL PHYSICS SE LECTURE NOTES IN PHYSICS LA English DT Proceedings Paper CT International Workshop on the Birth of the Universe and Fundamental Physics CY MAY 18-21, 1994 CL ROME, ITALY SP Comune Roma, European Astron Soc, European Phys Soc, Accad Nazl Lincei, Italian Soc Gen Rel & Gravit, Consiglio Nazl Ric, Ist Nazl Fis Nucl, European Space Agcy, Banca Nazl Lavoro C1 FERMILAB NATL ACCELERATOR LAB,NASA,FERMILAB ASTROPHYS CTR,BATAVIA,IL 60510. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN 33 PA HEIDELBERGER PLATZ 3, W-1000 BERLIN 33, GERMANY SN 0075-8450 BN 3-540-60024-8 J9 LECT NOTES PHYS PY 1995 VL 455 BP 259 EP 262 PG 4 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA BE87S UT WOS:A1995BE87S00043 ER PT B AU Mango, EJ Gill, JW AF Mango, EJ Gill, JW GP INST IND ENGINEERS INST IND ENGINEERS TI Revolutionizing maintenance on the space shuttle SO BREAKTHROUGH MAINTENANCE: PROCEEDINGS OF THE 12TH INTERNATIONAL MAINTENANCE CONFERENCE LA English DT Proceedings Paper CT 12th International Maintenance Conference - Breakthrough Maintenance CY OCT 16-17, 1995 CL SAN ANTONIO, TX SP Inst Ind Engineers AB Administration's (NASA) Space Shuttle program has been the pinnacle of the United States space flight experience for the last 15 years. Its reusable design and flexible cargo capability have provided over 65 human space missions in a wide range of astronautical and earth science experiments, The Space Shuttle Program is now in transition from being the vehicle of space science to truly providing space transportation to other space platforms. The NASA budget will be reduced $5 Billion over the next 5 years. This reduction will take place at a time when the future manifest supports at least seven missions with the Russian MIR and the start of Space Station Alpha orbital construction. Throughout these budget reductions, flight hardware safety and mission success remain the top priorities. The processing and checkout between each Space Shuttle Orbiter mission is governed by the Master Verification Plan (MVP). This plan states the structured methodology used for verifying that the shuttle is ready for flight. The methodology is based on the inherent design of the individual shuttle subsystems. Critical hardware is put through an extensive test and checkout process between each flight; regardless of the hardware's previous performance, time on the The National Aeronautics hardware or system invasion. The process includes verification of each redundant path of a system, and each redundant system, through a set of test requirements. These requirements are the Operations Maintenance and Requirement Specifications (OMRS). Each requirement corresponds to a type of procedure to be executed on the flight hardware prior to commit for flight. Within the preparations of a single Shuttle launch, approximately 7900 requirements are successfully executed. In order to accept additional cuts in the Shuttle budget, and maintain safe and successful human space flight, the NASA Administrator has stated that NASA must revolutionize the way we do business. To that end, engineers and managers at Kennedy Space Center have developed a new maintenance concept for the Space Shuttle Orbiter fleet. Reliability Centered Maintenance is a structured methodology which addresses the complex reliability characteristics of each individual system. RCM contains two unique processes, the "Baseline" and the "Reliability" process. The RCM "Baseline" process develops the MVP tasks to be accomplished. This structured methodology considers the direct, and adverse, effect on vehicle safety of each potential failure and then develops an applicable and effective task that will maintain the inherent reliability of each system. The RCM "Reliability" process objectively measures the actual system performance operating under the MVP, and feeds back to the "Baseline" process when the systems deviate from their performance expectations. The "Reliability" process monitors the implementation of corrective action to assure that the intended results are achieved. The methods of Reliability Centered Maintenance have been used in other industries, and the concepts are now being integrated into the unique realm of human space launch vehicles. When the MVP is augmented with Reliability Centered Maintenance concepts, the program will yield an overall reduction in maintenance requirements, a defensible basis for OMRS adjustments derived on actual operating experience, and use of inflight data to validate maintainability. This process will provide real substance from which budget reductions can be achieved without any reductions in safety or reliability. C1 NASA, KSC, Vehicle Engn Project Off, Kennedy Space Ctr, FL 32899 USA. RP Mango, EJ (reprint author), NASA, KSC, Vehicle Engn Project Off, Kennedy Space Ctr, FL 32899 USA. NR 5 TC 0 Z9 0 U1 0 U2 0 PU INST INDUSTRIAL ENGINEERS PI NORCROSS PA 25 TECHNOLOGY PARK/ATLANTA, NORCROSS, GA 30092 USA BN 0-89806-161-X PY 1995 BP 15 EP 23 PG 9 WC Engineering, Industrial SC Engineering GA BM77H UT WOS:000079726500003 ER PT B AU Mukai, K AF Mukai, K BE Buckley, DAH Warner, B TI ASCA observations of magnetic cataclysmic variables SO CAPE WORKSHOP ON MAGNETIC CATACLYSMIC VARIABLES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Cape Workshop on Magnetic Cataclysmic Variables CY JAN 23-27, 1995 CL UNIV CAPE TOWN, GRAD SCH BUSINESS, CAPE TOWN, SOUTH AFRICA SP Univ Cape Town, Fdn Res Dev, S African Gvt Dept Arts Culture Sci & Technol HO UNIV CAPE TOWN, GRAD SCH BUSINESS C1 NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY PHYS LAB,GREENBELT,MD 20771. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 1-886733-06-6 J9 ASTR SOC P PY 1995 VL 85 BP 119 EP 127 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BF08T UT WOS:A1995BF08T00017 ER PT B AU Barrett, P AF Barrett, P BE Buckley, DAH Warner, B TI Gamma-ray emission from Cataclysmic Variables SO CAPE WORKSHOP ON MAGNETIC CATACLYSMIC VARIABLES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Cape Workshop on Magnetic Cataclysmic Variables CY JAN 23-27, 1995 CL UNIV CAPE TOWN, GRAD SCH BUSINESS, CAPE TOWN, SOUTH AFRICA SP Univ Cape Town, Fdn Res Dev, S African Gvt Dept Arts Culture Sci & Technol HO UNIV CAPE TOWN, GRAD SCH BUSINESS C1 NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 1-886733-06-6 J9 ASTR SOC P PY 1995 VL 85 BP 141 EP 144 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BF08T UT WOS:A1995BF08T00021 ER PT B AU Mukai, K AF Mukai, K BE Buckley, DAH Warner, B TI Future X-ray missions: Prospects for magnetic cataclysmic variables SO CAPE WORKSHOP ON MAGNETIC CATACLYSMIC VARIABLES SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Cape Workshop on Magnetic Cataclysmic Variables CY JAN 23-27, 1995 CL UNIV CAPE TOWN, GRAD SCH BUSINESS, CAPE TOWN, SOUTH AFRICA SP Univ Cape Town, Fdn Res Dev, S African Gvt Dept Arts Culture Sci & Technol HO UNIV CAPE TOWN, GRAD SCH BUSINESS C1 NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. NR 0 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 BN 1-886733-06-6 J9 ASTR SOC P PY 1995 VL 85 BP 493 EP 495 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BF08T UT WOS:A1995BF08T00093 ER PT J AU HUNG, CC AF HUNG, CC TI ROOM-TEMPERATURE FLUORINE-INDUCED DECREASE IN THE STABILITY OF BROMINE AND IODINE-INTERCALATED CARBON-FIBERS SO CARBON LA English DT Article DE DEINTERCALATION; BROMINATED CARBON FIBERS; IODINATED CARBON FIBERS; FLUORINE-INDUCED DEINTERCALATION; THERMAL STABILITY; INTERCALATE EXCHANGE ID GRAPHITE AB Upon exposure to room-temperature fluorine, intercalated carbon fibers (containing either bromine alone or iodine and bromine together) become heavier and less stable. For Amoco P-100 graphitized carbon fibers, which were intercalated with 18 wt% bromine, 1 hour of fluorine exposure resulted in a large weight increase but caused only a small decrease in thermal stability. An additional 89 hours of fluorine exposure time resulted in small additional increases in fiber weight, but significant further decreases in fiber thermal stability. Such phenomena of weight increase and stability decrease do not occur if the intercalated fibers are exposed to 250 degrees C fluorine. These observations suggest that, at room temperature, fluorine is absorbed quickly by the intercalated fibers and is intercalated slowly into the fibers. Most of the original intercalates are replaced by fluorine in the process of fluorine intercalation. In an inert environment, the bromine intercalated fibers are much more thermally stable. After 800 degrees C vacuum heating for 2 weeks, the brominated fibers lost about 45% of their bromine, and their resistivity increased from 64 mu Omega-cm to a range of 95-170 mu Omega-cm. This is still much lower than the value of 300 mu Omega-cm for pristine P-100. For practical purposes, to preserve their thermal stability, brominated fibers need to be protected from exposure to fluorine at room temperature or to any intercalate at a temperature where, upon direct contact with graphite, an intercalation compound can easily be formed. RP HUNG, CC (reprint author), NASA,LEWIS RES CTR,CLEVELAND,OH 44135, USA. NR 9 TC 1 Z9 1 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0008-6223 J9 CARBON JI Carbon PY 1995 VL 33 IS 3 BP 309 EP 313 DI 10.1016/0008-6223(94)00129-N PG 5 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA QQ113 UT WOS:A1995QQ11300008 ER PT J AU HUNG, CC AF HUNG, CC TI FERRIC-CHLORIDE GRAPHITE-INTERCALATION COMPOUNDS PREPARED FROM GRAPHITE FLUORIDE SO CARBON LA English DT Article DE INTERCALATION; FERRIC CHLORIDE; GRAPHITE FLUORIDE DEFLUORINATION; NONGRAPHITIZED CARBON INTERCALATION; IRON HALIDE CARBON COMPOSITE; IRON OXIDE CARBON COMPOSITE AB The reaction between graphite fluoride and ferric chloride was observed in the temperature range of 300 to 400 degrees C. The graphite fluorides used for this reaction have an sp(3) electronic structure and are electrical insulators. They can be made by fluorinating either carbon fibers or powder having various degrees of graphitization. Reaction is fast and spontaneous and can occur in the presence of air. The ferric chloride does not have to be predried. The products have an sp(2) electronic structure and are electrical conductors. They contain first-stage FeCl3 intercalated graphite. Some of the products contain FeCl2 . 2H(2)O, others contain FeF3, in concentrations that depend on the intercalation condition. The graphite intercalated compounds (GIC) deintercalated slowly in air at room temperature, but deintercalated quickly and completely at 370 degrees C. Deintercalation is accompanied by the disappearance of iron halides and the formation of rust (hematite) distributed unevenly on the fiber surface. When heated to 400 degrees C in pure N-2 (99.99 vol%), this new GIC deintercalates without losing its molecular structure. However, when the compounds are exposed to 800 degrees C N-2 in a quartz tube, they lost most of their halogen atoms and formed iron oxides (other than hematite), distributed evenly in or on the fiber. RP HUNG, CC (reprint author), NASA,LEWIS RES CTR,CLEVELAND,OH 44135, USA. NR 9 TC 8 Z9 9 U1 2 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0008-6223 J9 CARBON JI Carbon PY 1995 VL 33 IS 3 BP 315 EP 322 DI 10.1016/0008-6223(94)00125-J PG 8 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA QQ113 UT WOS:A1995QQ11300009 ER PT J AU KOWBEL, W WITHERS, JC AF KOWBEL, W WITHERS, JC TI CVD AND CVR SILICON-BASED FUNCTIONALLY GRADIENT COATINGS ON C-C COMPOSITES SO CARBON LA English DT Article DE C-C COMPOSITES; CVR; CVD; FUNCTIONALLY GRADIENT COATINGS; OXIDATION PROTECTION ID CARBON-CARBON COMPOSITES; FIBERS AB Carbon-carbon (C-C) composites are considered an emerging technology critical to several military and commercial applications. However, C-C composites' inherent susceptibility to air oxidation at temperatures above 500 degrees C greatly limits their use to primarily price-insensitive military and space applications. Over the past several decades huge RandD efforts were conducted to develop an effective oxidation protection system for C-C composites. The acceptance of coating cracking was the basis of the majority of these efforts, resulting in an extensive and costly development of inhibitors and sealants. This paper addresses new and innovative approaches to the oxidation protection of C-C composites based upon crack-free coatings produced by Chemical Vapor Deposition (CVD) and Chemical Vapor Reaction (CVR) technology. Correlation between coating properties and the oxidation behavior of the coated C-C composites is discussed. C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23681. RP KOWBEL, W (reprint author), MER CORP,7960 S KOLB,TUCSON,AZ 85706, USA. NR 21 TC 47 Z9 53 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD, ENGLAND OX5 1GB SN 0008-6223 J9 CARBON JI Carbon PY 1995 VL 33 IS 4 BP 415 EP 426 DI 10.1016/0008-6223(94)00166-W PG 12 WC Chemistry, Physical; Materials Science, Multidisciplinary SC Chemistry; Materials Science GA QV565 UT WOS:A1995QV56500010 ER PT J AU FAIRBRIDGE, RW AF FAIRBRIDGE, RW TI EOLIANITES AND EUSTASY - EARLY CONCERTS ON DARWINS VOYAGE OF HMS BEAGLE SO CARBONATES AND EVAPORITES LA English DT Review ID SEA-LEVEL; SEQUENCES; BAHAMAS; ISLAND AB ''Eolianite'' and ''Eustasy'' sue both 20th century terms and even in their most rudimentary beginnings were not alluded to in most early 1901 century treatises of geology. Darwin saw beachrock for the first time in 1832 when HMS Beagle stopped at Recife (Pernambuco) in Brazil, then saw raised shore terraces in Patagonia and Chile, followed by coral atolls in mid-Pacific, and examined eolianites on Ascension. S.W. Australia, South Africa and on St. Helena, during the Beagle's extended voyage (1831-1836). The subsidence theory of atolls, based on studies of Capt. Fitzroy's navy charts, was formulated already before reaching Recife, and the crustal uplift in Patagonia offered a perfectly logical contrast to Pacific subsidence that eventually led to the concept of ''tectono-eustasy''. Although a decade or so before Charpentier, Agassiz and Geikie, the Ice-Age glaciation must have been clearly implanted in Darwin's mind, for he also reasoned on the assumption of its hydrologic implications, now known as ''glacio-eustasy''. Darwin repeatedly observed lime-cemented sandstones (later to be called ''eolian calcarenites'' by Grabau and ''eolianites'' by Sayles) in coastal settings. Their steep dips and bedding orientation suggested wind-borne (''aeolian'') transport from seaward, from a continental or insular shelf, now inundated by what - he reasoned - was a rise of sea level or sinking of the land. Darwin's observations of eolianites at King George's Sound in southwestern Australia in the last year of the voyage of the Beagle (March 1836) may perhaps have been the final ''crucial experiment'' that convinced him of the fundamental concept the worldwide nature of eustasy. C1 NATO,GODDARD INST SPACE STUDIES,NEW YORK,NY 10025. RP FAIRBRIDGE, RW (reprint author), COLUMBIA UNIV,2880 BROADWAY,NEW YORK,NY 10025, USA. NR 108 TC 6 Z9 7 U1 0 U2 0 PU NORTHEASTERN SCIENCE FOUNDATION INC PI TROY PA PO BOX 746, TROY, NY 12181-0746 SN 0891-2556 J9 CARBONATE EVAPORITE JI Carbonates Evaporites PY 1995 VL 10 IS 1 BP 92 EP 101 PG 10 WC Geology SC Geology GA RD927 UT WOS:A1995RD92700009 ER PT B AU Cannizzo, JK AF Cannizzo, JK BE Bianchini, A DellaValle, M Orio, M TI Four topics in accretion disk theory SO CATACLYSMIC VARIABLES SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Conference on Cataclysmic Variables CY JUN 20-24, 1994 CL ABANO TERME, ITALY SP CNR, Italian Space Ind Alenia, Banca Antoniana, Community Council Abano, Community Council Padova, Univ Padova, Astronom Observatory Padova, Int Sci Fdn C1 NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. NR 0 TC 1 Z9 1 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-3676-3 J9 ASTROPHYS SPACE SC L PY 1995 VL 205 BP 343 EP 348 PG 6 WC Neurosciences SC Neurosciences & Neurology GA BE85N UT WOS:A1995BE85N00097 ER PT B AU Schlegel, EM Mukai, K AF Schlegel, EM Mukai, K BE Bianchini, A DellaValle, M Orio, M TI ROSAT observations of 3 cataclysmic variables SO CATACLYSMIC VARIABLES SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Meeting Abstract CT Conference on Cataclysmic Variables CY JUN 20-24, 1994 CL ABANO TERME, ITALY SP CNR, Italian Space Ind Alenia, Banca Antoniana, Community Council Abano, Community Council Padova, Univ Padova, Astronom Observatory Padova, Int Sci Fdn C1 NASA,GSFC,GREENBELT,MD. NR 0 TC 0 Z9 0 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-3676-3 J9 ASTROPHYS SPACE SC L PY 1995 VL 205 BP 475 EP 475 PG 1 WC Neurosciences SC Neurosciences & Neurology GA BE85N UT WOS:A1995BE85N00131 ER PT B AU Mukai, K Naylor, T AF Mukai, K Naylor, T BE Bianchini, A DellaValle, M Orio, M TI Hibernation - Problems end alternatives SO CATACLYSMIC VARIABLES SE ASTROPHYSICS AND SPACE SCIENCE LIBRARY LA English DT Proceedings Paper CT Conference on Cataclysmic Variables CY JUN 20-24, 1994 CL ABANO TERME, ITALY SP CNR, Italian Space Ind Alenia, Banca Antoniana, Community Council Abano, Community Council Padova, Univ Padova, Astronom Observatory Padova, Int Sci Fdn C1 NASA,GODDARD SPACE FLIGHT CTR,HIGH ENERGY ASTROPHYS LAB,GREENBELT,MD 20771. RI Naylor, Tim /A-9465-2015 NR 0 TC 5 Z9 5 U1 0 U2 0 PU KLUWER ACADEMIC PUBL PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 0-7923-3676-3 J9 ASTROPHYS SPACE SC L PY 1995 VL 205 BP 517 EP 522 PG 6 WC Neurosciences SC Neurosciences & Neurology GA BE85N UT WOS:A1995BE85N00137 ER PT J AU HOFLUND, GB UPCHURCH, BT KIELIN, EJ SCHRYER, DR AF HOFLUND, GB UPCHURCH, BT KIELIN, EJ SCHRYER, DR TI INFLUENCE OF AN FE PROMOTER ON SILICA-SUPPORTED PT/SNOX CATALYSTS USED FOR LOW-TEMPERATURE CO OXIDATION SO CATALYSIS LETTERS LA English DT Article DE CO OXIDATION; PLATINIZED TIN OXIDE ID REDUCIBLE OXIDE MATERIALS; SURFACE CHARACTERIZATION; CARBON-MONOXIDE; GOLD CATALYSTS; TIN; PRETREATMENT; PERFORMANCE; REDUCTION; BEHAVIOR; AU/MNOX AB Silica-supported Pt/SnOx catalysts used for low-temperature CO oxidation have been prepared without and with an Fe promoter. Reaction studies demonstrate that the addition of the Fe promoter results in higher catalytic activity in the presence of 8 at% CO2 and a lower decay rate. Ion scattering spectroscopy (ISS) has been used to examine the outermost atomic layers of the promoted and nonpromoted catalysts before and after activation by a reductive pretreatment. The nonpromoted catalyst exhibits agglomeration of the platinized tin oxide film exposing the catalytically inactive silica support. This agglomeration does not occur when Fe is present, and a large catalytically active surface area is maintained during the reduction. C1 NASA,LANGLEY RES CTR,HAMPTON,VA 23665. RP HOFLUND, GB (reprint author), UNIV FLORIDA,DEPT CHEM ENGN,GAINESVILLE,FL 32611, USA. NR 27 TC 11 Z9 11 U1 0 U2 1 PU BALTZER SCI PUBL BV PI AMSTERDAM PA ASTERWEG 1A, 1031 HL AMSTERDAM, NETHERLANDS SN 1011-372X J9 CATAL LETT JI Catal. Lett. PY 1995 VL 31 IS 2-3 BP 133 EP 141 DI 10.1007/BF00808827 PG 9 WC Chemistry, Physical SC Chemistry GA QN398 UT WOS:A1995QN39800001 ER EF