The gas dynamics of H II regions. VI - H II regions in collapsing massive molecular clouds

Details The gas dynamics of H II regions. VI - H II regions in collapsing massive molecular clouds The gas dynamics of H II regions. VI - H II regions in collapsing massive molecular clouds

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...108...25y&link_type=abstract

Astronomy and Astrophysics, vol. 108, no. 1, Apr. 1982, p. 25-41.

Astronomy and Astrophysics

Astrophysics

27

Astronomical Models, Gas Dynamics, Gravitational Collapse, H Ii Regions, Molecular Clouds, B Stars, O Stars, Stellar Mass, Stellar Motions

Scientific paper

Two-dimensional numerical calculations of the evolution of H II regions associated with self-gravitating, massive molecular clouds are presented. Parameters include the birthplace of the exciting star, the stellar motion, and the mass and rotation of the molecular cloud. The evolution of freely falling clouds leads to a central density condensation, and to partial evaporation at an average rate of 0.005 solar mass/yr only in those cases where a champagne flow occurs. On the other hand if 100 O stars are placed at the center of a freely-falling cloud of 300,000 solar masses no evaporation takes place. In some cases secondary density condensations appear in the flow. If rotation is included, the free-fall collapse is stopped and the evaporation rate is larger. These results together with observational data concerning molecular clouds allow the conclusion that massive molecular clouds with OB stars can be evaporated in 10 million yr.

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