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At least 1,639 records · Page 91
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NASA NTRS1986

Elemental, isotopic and molecular abundances in comets

The chemical composition of comet nuclei and the factors affecting it are discussed, summarizing the results of recent theoretical, experimental, and observational investigations. Consideration is given to the evidence supporting the view that the nucleus is radially differentiation (except for a thin outer layer), surface differentiation by heat processing and outgassing, and mantle buildup on an undifferentiated core. The nature of the refractory and volatile components is examined, and the elemental and isotopic compositions are given in tables and characterized. The uncertain (except for H2O) molecular composition of the volatile fraction is considered, and it is suggested that some oxides or aldehydes (such as CO, CO2, and H2CO), but no large amounts of fully hydrogenated compounds (such as CH4 and NH3) are included.

Delsemme, A. H.↗
NASA NTRS1986

Carbon abundance measurements in oceanic basalts - The need for a consensus

Large systematic discrepancies currently exist among the carbon data reported for oceanic basalts by different laboratories. These discrepancies are likely attributable both to nonuniform criteria for the removal of carbon contamination from the samples, and to systematic errors in analytical procedures. In order to solve these problems, investigators must agree upon effective criteria for the removal of carbon contamination, and they must create an accurately calibrated set of basaltic glass carbon standards.

Des Marais, D. J.↗
NASA NTRS1986

Comprehensive models of diffuse interstellar clouds - Physical conditions and molecular abundances

The limitations of steady state models of interstellar clouds are explored by means of comparison with observational data corresponding to clouds in front of Zeta Per, Zeta Oph, Chi Oph, and Omicron Per. The improved cloud models were constructed to reproduce the observed H and H2(J) column densities for several lines of sight. The main difference from previous models is the treatment of self-shielding in the H2 lines. Other improvements over previous models are discussed as well.

Van Dishoeck, E. F.↗
NASA NTRS1986

The interstellar carbon abundance. II - Rho Ophiuchi and Beta Scorpii

A procedure designed to obtain increased sensitivity from high-dispersion IUE spectra by using a flat-field spectrum to remove nonrandom noise due to the response pattern of the SEC vidicon detector is described. Application of this procedure to spectra of Rho Oph and Beta(1) Sco near the spin-forbidden interstellar 2325 line of C II yields 2 sigma upper limits on absorption of W (lambda) not greater than about 4 mA. The resulting depletion of carbon from the interstellar gas toward Rho Oph exceeds a factor of 1.4.

Welty, D. E.↗
NASA NTRS1987

Supernovae 1983i and 1983v - Evidence for abundance variations in type Ib supernovae

Spectra are presented of SN 1983i 5 days after discovery and of SN 1983v 13 days after discovery. The similarity of these two spectra argues that they are of similar origin and phase. Theoretical atmosphere calculations provide evidence for a connection to the type Ib supernovae 1983n and 1984l, with SN 1983i and 1983v having a similar structure but less helium and more carbon and oxygen. Available photometry suggests that the spectra correspond to a phase about 20 days after maximum light. These spectra are consistent with an interpretation of type Ib supernovae arising in the bare cores of moderately massive stars, with individual events showing a range in He/O mass ratio from approximately 10 to less than 1.

Wheeler, J. C.↗
NASA NTRS1987

Mars regolith versus SNC meteorites - Possible evidence for abundant crustal carbonates

Viking XRF data of the Martian regolith are compared with data of typical igneous rocks of the earth, Moon, eucrite parent asteroid, and shergottite, nakhlite, and Chassigny (SNC) meteorites. It is suggested that regolith's low Ca/Si ratio, with respect to igneous rocks with similar (Mg + Fe)/Si ratios, is not a result of simple mixing of SNC-like rocks with other igneous rocks, but rather is due to the removal of Ca from the regolith as Ca-carbonate. Formation of a mass of carbonate equivalent to a 20-m-thick global shell could account for the removal of 1000 mbar of CO2 from the Martian atmosphere. This Ca/Si ratio is consistent with the hypothesis that the Martian climate was once far warmer and wetter than at present.

Warren, Paul H.↗
NASA NTRS1986

Correlated isotopic effects near the Fe abundance peak

A special class of refractory inclusions in carbonaceous meteorites show large isotopic anomalies in Ca, Ti, and Cr that are correlated by virtue of having been measured on the same samples. Large excesses in the neutron-rich isotopes Ca-48, Ti-50, and Cr-54 are comparable and consistent with theoretical calculations of the composition of materials produced during neutron-rich nuclear statistical equilibrium nucleosynthesis. This correlation suggests that materials from very near the core of an expoloding massive star may be injected into the interstellar medium.

Papanastassiou, D. A.↗
NASA NTRS1987

Extinction and abundance properties of Alpha Scorpii circumstellar grains

The UV extinction and element depletions in the circumstellar envelope Alpha Sco are investigated using IUE, Copernicus, and AS data of Alpha Sco B which can be seen in absorption through the cool-star envelope. The circumstellar reddening, depletions, and spectral extinction toward Alpha Sco B are estimated. Evidence is presented which suggests that the circumstellar grains are large and siliceous.

Snow, Theodore P., Jr.↗
NASA NTRS1987

Radio observations of carbon monoxide toward Zeta Ophiuchi - Velocity structure, isotopic abundances, and physical properties

This paper presents a small-scale map of the molecular gas around the line of sight toward Zeta Oph made with measurements of the (C-12)O (1-0) emission obtained at high signal-to-noise ratio and high velocity resolution. In addition, a measurement of the (C-12)O (2-1) line emission and a detection of (C-13)O along the line of sight to the star are reported. The results show that the CO emission toward the star is composed from at least four components with peak velocities at -2.0, -0.7, 0.0, and +0.6 km/s. The radio observations yield a total CO column density of 1.4 x 10 to the 15th/sq cm, with about one-half of the total CO column density being in the main component at -0.7 km/s. The main cmponent is uniform over the map, but the other components are variable, suggesting that the cloud is clumpy. The data on the two CO transitions imply that the excitation temperature and the density of the main component are about 7 K and 800/cu cm, respectively.

Langer, William D.↗
NASA NTRS1987

The abundance of interstellar CO

Data from recent observations of interstellar CO column densities are compiled in tables and graphs and compared with the predictions of theoretical models. The energy-level structure of CO and the excitation of interstellar CO are discussed; UV-absorption and IR line observations are characterized; and techniques used to estimate the CO column density from mm-wavelength observations (based on calibration of the CO line intensity with the column density of H2) are described in detail. Consideration is then given to CO chemistry under interstellar-cloud conditions (isotope fractionation and photodissociation) and models for diffuse, translucent, and dense clouds. A number of unsolved problems requiring additional observations or laboratory investigations are identified.

Van Dishoeck, Ewine F.↗
NASA NTRS1988

I(CO)/N(H2) conversions and molecular gas abundances in spiral and irregular galaxies

Observations of emission in the J = 1-0 rotational transition of interstellar CO are used to obtain column densities and masses of hydrogen. By taking into account the effects of variations in molecular cloud parameters on conversion factors between integrated CO intensity and molecular hydrogen column density, it is shown that conversion factors are very sensitive to the kinetic temperature of the emitting gas. Results indicate that the gas temperatures in systems with high star formation rates can be quite high, and it is suggested that use of a standard conversion factor will lead to systematic overestimation of the amount of molecular gas.

Maloney, Philip↗
NASA NTRS1988

The difference in hydrogen abundance between two classes of type I X-ray bursts

The hypothesis that the bright type I X-ray bursts differ from faint bursts in that a hydrogen-rich envelope is ejected in the former type and not in the latter is theoretically discussed and experimentally investigated. Color-temperature versus luminosity diagrams of X-ray bursts from MXB 1636-536 and MXB 1608-522 are constructed based on observations from the Tenma satellite and are used to study the hydrogen richness of the surface of the neutron stars resulting from the outbursts. Systematic differences between the bright and faint class diagrams are found which confirm the hypothesis.

Ebisuzaki, Toshikazu↗
NASA NTRS1988

Monodeuterated methane in the outer solar system. III - Its abundance of Titan

The 3nv2 band of CH3D has been detected in spectra of Titan recorded at 1.6 microns with the Fourier transform spectrometer at the 4 m telescope of the Kitt Peak National Observatory. A value of the CH3D/Ch4 mixing ratio is obtained from a comparison between the observed Titan spectra and synthetic spectra. This value is about 2 times higher than the value measured on Uranus (de Bergh et al. 1981, 1986) and about 6 times higher than on Jupiter and on Saturn (Courtin et al. 1984; de Bergh et al.). The value found on Titan for D/H in methane is comparable to the D/H ratio measured in terrestrial H2O.

De Bergh, C.↗
NASA NTRS1987

Mars regolith versus SNC meteorites: Evidence for abundant crustal carbonates

Viking XRF analyses are compared with those for terrestrial and lunar basalt samples, and eucritic meteorites (of possible Mars origin). The comparison indicates depletion of Ca relative to Si in the Mars regolith. It is suggested that carbonate formation during a warmer, wetter epoch early in Mars' history could have been responsible.

Warren, Paul H.↗