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The Effect of Helium Shell Flashes on Asymptotic Giant Branch Evolution

Published online by Cambridge University Press:  25 April 2016

E. Vassiliadis  and
P.R. Wood
E. Vassiliadis
Affiliation:
Mount Stromlo and Siding Spring Observatories, Private Bag, Weston Creek, ACT 2611
P.R. Wood
Affiliation:
Mount Stromlo and Siding Spring Observatories, Private Bag, Weston Creek, ACT 2611
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Abstract

Mass-loss has been incorporated into a series of evolutionary calculations of low to intermediate mass stars during Asymptotic Giant Branch (AGB) evolution. When helium shell flashes occur a superwind phase is a natural consequence of the mass-loss process. The structure of the stellar wind envelopes that result has been computed. The models may explain some previously curious features seen in OH/IR and CO line emission spectra.

Type
Galactic and Stellar
Information
Publications of the Astronomical Society of Australia , Volume 10 , Issue 1 , 1992 , pp. 30 - 32
Copyright
Copyright © Astronomical Society of Australia 1992

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References

Boothroyd, A. I. and Sackmann, I. J., 1988a, Astrophys. J., 328, 653.Google Scholar
Boothroyd, A. I. and Sackmann, I. J., 1988b, Astrophys. J., 328, 641.CrossRefGoogle Scholar
Bowen, G., 1988, Astrophys. J., 329, 844.Google Scholar
Castor, J. L. 1981, in Physical Processes in Red Giants, eds. Iben, I. and Renzini, A. (Reidel), p. 285.CrossRefGoogle Scholar
Eder, J., Lewis, B. M. and Terzian, Y., 1988, Astrophys. J. Suppl. Ser., 66, 183.CrossRefGoogle Scholar
Hearn, A. G., 1990, in From Miras to Planetary Nebulae: Which Path for Stellar Evolution?, eds. Mennessier, M. O. and Omont, A. (Editions Frontieres), p. 121.Google Scholar
Holzer, T. E. and MacGregor, K. B., 1985, in Mass Loss from Red Giants, eds. Morris, M. and Zuckerman, B. (Reidel), p.229.Google Scholar
Hughes, S. M. G. and Wood, P. R., 1990, Astron. J., 99, 784.Google Scholar
Jura, M. and Kleinmann, S. G., 1991, preprint.Google Scholar
te Lintel Hekkert, P., 1990, thesis, Leiden University.Google Scholar
van der Veen, W. E. C. J. and Rugers, M., 1989, Astron. Astrophys., 226, 183.Google Scholar
van der Veen, W. E. C. J. and Olofsson, H., 1990, in From Miras to Planetary Nebulae: Which Path for Stellar Evolution?, eds. Mennessier, M.O. and Omont, A. (Editions Frontieres), p.67.Google Scholar
Wood, P. R., 1979, Astrophys. J., 227, 220.CrossRefGoogle Scholar
Wood, P. R., 1990, in From Miras to Planetary Nebulae: Which Path for Stellar Evolution?, eds. Mennessier, M. O. and Omont, A. (Editions Frontieres), p. 67.Google Scholar