Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989ssrv...51..235t&link_type=abstract
Space Science Reviews (ISSN 0038-6308), vol. 51, Dec. 1989, p. 235-337.
Astronomy and Astrophysics
Astronomy
34
Astronomy, Interstellar Chemistry, Interstellar Matter, Molecular Clouds, Stellar Envelopes, Abundance, Gas-Ion Interactions, H Ii Regions, Molecular Interactions, Shock Wave Interaction, Ultraviolet Radiation
Scientific paper
Model comparisons of the four currently recognized regimes of astrochemistry with actual observations are conducted. The ion-molecule-gas-phase-chemistry models explain fairly well the simpler molecular species in diffuse and cold quiescent dense interstellar clouds, as well as in the outer envelopes of circumstellar clouds. The dust-grain-chemistry models may modify the ion-molecule chemistry in regions, shocks, or other heating agents serving to promote surface reactions and to desorb molecules frozen on grains; dust-grain chemistry has no role in cold quiescent clouds except to adsorb gas phase molecules. The models of shock-chemistry occurring in regions of star formation appear to be important in explaining certain molecular species and in disrupting grains. The circumstellar-envelope models combine several chemistries, including those of thermochemical equilibrium in the dense inner regions and ion-molecule in the outer regions, with grain processes also likely. The limitations of all current models are also discussed.
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