H II bubbles and disruption of molecular clouds

Details H II bubbles and disruption of molecular clouds H II bubbles and disruption of molecular clouds

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....90...65m&link_type=abstract

Astronomy and Astrophysics, vol. 90, no. 1-2, Oct. 1980, p. 65-69.

Astronomy and Astrophysics

Astrophysics

14

Molecular Clouds, Nebulae, Stellar Envelopes, Astronomical Models, B Stars, Gas Expansion, Gravitational Effects, H Ii Regions, Main Sequence Stars, Open Clusters

Scientific paper

The possibility that molecular clouds are disrupted by expanding H II regions within them is examined. The results show that the self-gravity of the dense shell that is swept up can halt the expansion if the cloud is sufficiently massive. For hydrostatic clouds the mass required to prevent disruption by the expansion of the H II region of a typical star is approximately 7 x 10 to the 4th solar masses. This upper mass limit for disruption drops dramatically if the molecular clouds are in free-fall. However, indications exist that the clouds are not in free-fall, and this mode of cloud disruption could account for the absence of CO emission in older open clusters, the configuration of the region around lambda Ori, and observed H I shells.

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