Stellar winds in molecular clouds

Details Stellar winds in molecular clouds Stellar winds in molecular clouds

Jun 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...238..860s&link_type=abstract

Astrophysical Journal, Part 1, vol. 238, June 15, 1980, p. 860-866.

Astronomy and Astrophysics

Astrophysics

44

Interstellar Matter, Molecular Gases, Nebulae, O Stars, Stellar Winds, Bubbles, Cosmology, H Ii Regions, Hydrogen Ions, Infrared Radiation, Radio Emission, Stellar Luminosity, Ultraviolet Radiation

Scientific paper

It is shown that strong stellar winds from O stars may dominate the evolution of compact H II regions in molecular clouds. For a cloud with a density of 100,000/cu cm, the pressure-driven bubble expands to about 0.2 pc radius in 10,000 years, after which time the interior cools and wind momentum continues to drive the shell. Grains accumulate in a shell outside the bubble, radiating the star's UV luminosity in the far-IR. Consideration is given to the IR and radio appearance of these sources, and to the probable effects of the progenitor on the supernova remnant.

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