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Two-fluid models for the winds of OB stars

Published online by Cambridge University Press:  01 April 2008

J. H. Guo*
Affiliation:
National Astronomical Observatories/Yunnan Observatory, Chinese Academy of Sciences, P. O. Box 110, Kunming 650011, China. email: guojh@ynao.ac.cn
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Abstract

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A two-fluid model to OB stars is investigated, in which the flow is described by a set of two components, One for the dense clumps and the other for the smooth gas. The two components are coupled by friction drag. The velocity structure of clumps is assumed to be beta law, thus, the velocity structure of the second component could be attained by shooting method. The result is compared with the X-ray observations.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

References

Cohen, D. H. et al. 2006, MNRAS, 368, 1905CrossRefGoogle Scholar
Feldmeier, A., Puls, J., & Pauldrach, W. A. 1997, A&A, 322, 878Google Scholar
Lucy, L. B. & Solomon, P. M. 1970, ApJ, 159, 879CrossRefGoogle Scholar
Lucy, L. B. & White, R. L. 1980, ApJ, 241, 300CrossRefGoogle Scholar
Pistinner, S. & Shaviv, G. 1993, 1993, ApJ, 414, 612CrossRefGoogle Scholar
Soo, S. L. 1989, Particulates and Continuum: Pultiphase Fluid Dynamics (New York: Hemisphere)Google Scholar
Waldron, W. L. & Cassinelli, J. P. 2000, ApJ, 548, L45CrossRefGoogle Scholar
Waldron, W. L. & Cassinelli, J. P. 2007, ApJ, 668, 456Google Scholar