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Mass loss from pulsating cool stars

Published online by Cambridge University Press:  01 April 2008

Qian Wang ,
Lee Anne Willson  and
Steven Kawaler
Qian Wang
Affiliation:
Department of Physics and Astronomy, Iowa State University, Ames, IA 50010, USA email: [email protected], [email protected], [email protected]
Lee Anne Willson
Affiliation:
Department of Physics and Astronomy, Iowa State University, Ames, IA 50010, USA email: [email protected], [email protected], [email protected]
Steven Kawaler
Affiliation:
Department of Physics and Astronomy, Iowa State University, Ames, IA 50010, USA email: [email protected], [email protected], [email protected]
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Abstract

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It has long been clear that most, if not all, of the mass loss experienced by stars from 0.8 to 8 solar masses occurs near the tip of the AGB and/or the RGB. Evolutionary studies have incorporated empirical mass loss laws but theoretical models suggest quite different dependence of mass loss rate on stellar parameters. We are combining evolutionary model calculations with ISUEVO with mass loss modeling using the Bowen code in a systematic study of final stages of stellar evolution. We mapped the RGB (without steady mass loss) to the “Death Zone” as a function of mixing length, mass, and metallicity. We compared these results with observation data from Origlia. We are investigating a possible mass loss mechanism through companions as a complement to mass loss through pulsation. By the end of the project we expect to provide a reliable prescription for AGB mass loss.

Keywords

Stars: mass lossstars: AGB and post-AGB
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 259 - 260
Copyright
Copyright © International Astronomical Union 2008

References

Bowen, G. H. 1988, ApJ, 329, 299Google Scholar
Bowen, G. H. & Willson, L. A. 1991, ApJ, 375, L53CrossRefGoogle Scholar
Höfner, S. & Anderson, A. 2007, 465, L39, L39–L42Google Scholar
Kawaler, S. 2005, ApJ, 621, Issue 1, pp. 432–444CrossRefGoogle Scholar
Origlia, L. et al. 2002, ApJ, 571; 458–468CrossRefGoogle Scholar
Struck, C. et al. 2004, MNRAS, 353, Issue 2, pp. 559–570CrossRefGoogle Scholar
Sweigart, A., Greggio, L., & Renzini, A. 1990, ApJ, 364; 527–539CrossRefGoogle Scholar
Willson, L. A. 2000, ARAA, 38, 573–611Google Scholar
Willson, L. A. 2007, Vienna proceedings, eds. Kerschbaum, Franz, Charbonnel, Corinne and Wing, Robert, page (to appear)Google Scholar
Willson, L. A. 2007, this volumeGoogle Scholar
Woitke, P. 2006, 460, L9, L9–L12Google Scholar