Champagne Flows and Winds in H II Regions

Details Champagne Flows and Winds in H II Regions Champagne Flows and Winds in H II Regions

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003rmxac..15..166l&link_type=abstract

Winds, Bubbles, and Explosions: a conference to honor John Dyson, Pátzcuaro, Michoacán, México, September 9-13, 2002 (Eds. S. J.

Astronomy and Astrophysics

Astronomy

3

Hii Regions, Stars: Formation, Stars: Mass Loss

Scientific paper

We discuss the expansion of an initially self-gravitating, static, singular cloud core characterized by a power-law density distribution, rho ~ r^-n, with 3/2 < n < 3. This core is heated out of mechanical balance by the formation of a massive star at its center. If the initial ionization and heating is approximated to occur instantaneously at t = 0, the subsequent flow (for r >> 100 AU) caused by the resulting imbalance between self-gravity and thermal pressure is self-similar. Because of the steep density profile, pressure gradients produce a shock front that travels into the cloud, accelerating the gas to supersonic velocities in what has been called the ``champagne phase''. The expansion of the inner region at t > 0 is connected to the outer envelope of the now ionized cloud core through this shock whose strength is an increasing function of the exponent n. We also discuss the evolution of the strong stellar winds of massive stars inside these champagne flows.

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