Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.231..409b&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 231, March 15, 1988, p. 409-417. SERC-supported researc
Astronomy and Astrophysics
Astronomy
198
Chemical Composition, Cosmochemistry, Interstellar Matter, Molecular Clouds, Abundance, High Temperature Gases, Hydrogen Clouds, Orion Nebula, Planetary Nebulae
Scientific paper
The authors present a detailed time-dependent chemical model which has been developed to describe the chemical composition of hot molecular cores in dense star-forming interstellar clouds. They follow the chemical evolution of a cold collapsing clump of gas, including the accretion and subsequent reaction of material on to the surface of interstellar grains, until the density of molecular hydrogen in the clump becomes equal to 107cm-3. At this point they halt the collapse and assume that some heating event, perhaps associated with the formation of a nearby star, liberates the molecular mantles back into the gas phase. Comparison between the calculated abundances and those observed in the Orion Hot Core shows that such a model is likely to be qualitatively correct. In particular, the evidence that both hydrogenation and deuteration occur on the grain surface is very strong.
Brown David P.
Charnley Steven B.
Millar Thomas J.
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