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AGB mass loss

Published online by Cambridge University Press:  30 August 2012

Lee A. Willson  and
Qian Wang
Lee A. Willson
Affiliation:
Department of Physics and Astronomy, Iowa State University, Ames, Iowa, USA50010 email: lwillson@iastate.edu
Qian Wang
Affiliation:
Department of Physics and Astronomy, Iowa State University, Ames, Iowa, USA50010 email: lwillson@iastate.edu
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Abstract

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Mass loss on the AGB removes most of the envelope and leaves a compact remnant to become a white dwarf and perhaps first the central star of a planetary nebula. The envelope mass provides an upper limit on the material available to form the PN, and the terminal mass loss rate plus the small remnant mass left on the core determines how much of that would still be available to form the PN after the star has evolved far enough to the blue. Given a mass loss formula based on observations or models, we can find the deathline where −dMstar/dt = (M/L) dL/dt and can find the contours of constant mass loss rate on a plot of M vs. L. From such plots we can derive the mass available for a PN and the lowest mass single star that can produce a PN of a given mass. However, some details important for PN formation remain uncertain, including the maximum mass loss rate achieved and the envelope mass left when AGB mass loss ceases.

Keywords

Stars: mass lossstars: AGB and post-AGBMirasstars: windsoutflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S283: Planetary Nebulae: An Eye to the Future , July 2011 , pp. 71 - 78
Copyright
Copyright © International Astronomical Union 2012

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