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E. Villaver (STScI/ESA), M. Robberto (STScI), N. Panagia (STScI/ESA)
Massive OB stars heavily affect their environment through their powerful winds and strong UV radiation fields. Winds erode the parent molecular cloud forming cavities -- wind driven bubbles -- that have a very small UV opacity. The radiative and dynamical properties of H II regions have been extensively modeled over the last four decades after the pioneering works of Stromgren and Kahn. However, a complete model of a main sequence wind-driven bubble applicable to the Orion nebula does not exist. We revisit the standard calculations of H II regions by computing a wind+ H II region structure suited to reproduce the observed properties of the Orion region. We explore the effects of the photoionization flow generated at the IF, the external pressure structure, and the effects of multiple stars each contributing its wind and radiation.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.