Computer Science
Scientific paper
May 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982gecoa..46..777l&link_type=abstract
(Meteoritical Society, Annual Meeting, 44th, Berne, Switzerland, Aug. 17-21, 1981.) Geochimica et Cosmochimica Acta, vol. 46, Ma
Computer Science
1
Chemical Composition, Gas Composition, Interstellar Gas, Molecular Clouds, Planetary Nebulae, Carbon Monoxide, Cool Stars, Cosmic Dust, Gas Density, Grains, Stellar Evolution, Chemistry, Composition, Gases, Grains, Clouds, Formation, Density, Dust, Interplanetary Dust, Models, Observations, Spectra, Abundance, Heavy Elements, Carbon Monoxide, Metals, Optical Properties, Infrared, Absorption, Ultraviolet, Wavelengths
Scientific paper
It is shown that dense, molecular interstellar clouds contain most of their carbon, magnesium and heavier elements in the form of grains, as silicates, silicon carbide, graphite and ices. Most hydrogen and noble gases are in the gaseous phase, with oxygen and nitrogen being probably distributed between gas and grains. It is suggested that grains form in the expanding atmospheres of cool stars, then survive in the denser parts of the diffuse medium. Ice mantles grow from molecules in the gas phase in the interior of dense clouds and seem to be destroyed outside them, perhaps due to the effect of UV radiation. It is noted that grain mantles are potential sources of complex organic molecules in the early solar system.
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