The formation of molecules in protostellar winds

Details The formation of molecules in protostellar winds The formation of molecules in protostellar winds

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991apj...373..254g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 373, May 20, 1991, p. 254-265. Research supported by NASA and NSF.

Other

70

Abundance, Interstellar Chemistry, Pre-Main Sequence Stars, Protostars, Stellar Winds, Carbon Monoxide, Reaction Kinetics, Stellar Models, Temperature Distribution

Scientific paper

The production and destruction processes for molecules in very fast protostellar winds are analyzed and modeled with a one-dimensional chemical kinetics code. Radial density and temperature distributions suggested by protostellar theory are explored as are a range of mass-loss rates. The efficiency of in situ formation of heavy molecules is found to be high if the wind temperature falls sufficiently rapidly, as indicated by theory. The degree of molecular conversion is a strong function of the mass-loss rate and of density gradients associated with the acceleration and collimation of the wind. Even in cases where essentially all of the heavy atoms are processed into molecules, a significant fraction of atomic hydrogen remains so that highly molecular, protostellar winds are able to emit the 21-cm line. Although CO has a substantial abundance in most models relevant to very young protostars, high abundances of other molecules such as SiO and H2O signify more complete association characteristic of winds containing regions of very high density. Although the models apply only to regions close to the protostar, they are in qualitative accord with recent observations at much larger distances of both atomic and molecular emission from extremely high-velocity flow.

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