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Convection and pulsation in red giant stars

Published online by Cambridge University Press:  01 August 2006

P. R. Wood
P. R. Wood*
Affiliation:
Research School of Astronomy & Astrophysics, Australian National University, Cotter Road, Weston Creek ACT 2611, Australia email: wood@mso.anu.edu.au
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Abstract

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Convection strongly influences the periods, stability and amplitudes of pulsation in red giant stars. For example, changing the efficiency of convection (the mixing length parameter) changes the radius and the effective temperature of a red giant, which in turn changes the pulsation period at a given luminosity. Since essentially all the energy flux outside the nuclear-burning core is carried by convection, it is the variation of convective energy transport throughout the pulsation cycle that determines pulsation stability. In both linear and nonlinear pulsation models, the turbulent viscosity that results from the interaction of pulsation with turbulent convection provides a strong damping effect on pulsation and, in nonlinear models, it determines the limiting amplitude. In this paper, these and other topics are discussed.

Keywords

Stars: AGB and post-AGBstars: oscillationsstars: late-type
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S239: Convection in Astrophysics , August 2006 , pp. 343 - 348
Copyright
Copyright © International Astronomical Union 2007

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