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The Effect of Mass-Loss On the Evolution of HII Regions in the L.M.C.

Published online by Cambridge University Press:  04 August 2017

I.R.G. Wilson  and
M. A. Dopita
I.R.G. Wilson
Affiliation:
Royal Greenwich Observatory, Herstmonceux Castle, Hailsham East Sussex, United Kingdom BN27 1RP Mount Stromlo and Siding Spring Observatories, Private Bag Woden P.O. Canberra Australia 2606
M. A. Dopita
Affiliation:
Mount Stromlo and Siding Spring Observatories, Private Bag Woden P.O. Canberra Australia 2606

Abstract

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Empirical calibrations based on prior studies of Galactic OB Stars are used to determine the integrated stellar wind mechanical luminosity (Lw) and the integrated Lyman continuum photon luminosity (S*) for 10 OB clusters in the L.M.C. These values of Lw and S*, together with narrow band H-α surface photometry of an overlapping sample of 15 L.M.C. HII regions, are used to show that the large shell-like HII regions, in the L.M.C. are stellar wind bubbles 3 to 5 million years old. In order to reproduce the general properties of these HII shells, a thick cushion of shocked stellar wind gas must have been present on the inside of the shell for most of the life time of the nebula, and the shell itself must be ram pressure confined by the HI/molecular cloud out of which it formed.

Type
Interstellar Matter
Information
Symposium - International Astronomical Union , Volume 108: Structure and Evolution of the Magellanic Clouds , 1984 , pp. 385 - 388
Copyright
Copyright © Reidel 1984 

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