Chemical evolution in molecular clump-stellar wind interfaces

Details Chemical evolution in molecular clump-stellar wind interfaces Chemical evolution in molecular clump-stellar wind interfaces

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.243..405c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 243, April 1, 1990, p. 405-412. Research supported by t

Physics

35

Chemical Evolution, Interstellar Chemistry, Molecular Clouds, Star Formation, Stellar Winds, Abundance, Astronomical Models, Energy Transfer, Interstellar Matter, Stellar Mass

Scientific paper

Chemical diagnostics of the heating rate and mixing rate of stellar wind plasma with cool clump gas in star-forming regions are considered. Observation of the distributions of C0, C(+), and CH at the outer boundaries of clumps in B5, a region of low-mass star formation, would lead to considerable insight into the physics of the interaction of flows in diffuse media with the clumps which are embedded in them. Such interactions have important effects on the global flow structures in a large variety of diffuse astronomical sources, but B5, in the light of the present results, is especially well suited to the study of general physical processes of consequence in boundary layers.

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