Molecular abundances and nucleation in protostellar envelopes

Details Molecular abundances and nucleation in protostellar envelopes Molecular abundances and nucleation in protostellar envelopes

Aug 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.103..143r&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 103, no. 1, Aug. 1984, p. 143-154. Research supported by the Fundacao de A

Astronomy and Astrophysics

Astrophysics

4

Abundance, Interstellar Matter, Nucleation, Protostars, Stellar Envelopes, Carbon, Gas Dissociation, Hydrogen, Iron, Magnesium, Oxygen

Scientific paper

The molecular structure of a massive protostellar envelope is studied using the model developed by Larson (1972). Molecular and atomic abundances are obtained on the basis of the dissociation equilibrium theory. The time-independent homogeneous nucleation theory is applied to estimate the nucleation rate using molecules as the starting point for the grain condensation process.

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