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Convective Cores in Stellar Models

Published online by Cambridge University Press:  12 April 2016

I.W. Roxburgh  and
M. Monteiro
I.W. Roxburgh
Affiliation:
Astronomy Unit, Queen Mary and Westfield College, University of London
M. Monteiro
Affiliation:
Astronomy Unit, Queen Mary and Westfield College, University of London

Abstract

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The condition for homogeneous radiative stellar models to be marginally stable to convection at the centre is investigated for the family of models where the opacity к and energy generation ε are given by power laws in temperature and density κ = κo ρα T−β, ε = εo ρ Tη. The Naur-Osterbrock (1953) condition 6η > 6 + 10β − 15α is a necessary but not sufficient condition. A better estimate is obtained by taking the effective polytropic index n = dlogP/dlogT - 1 to be a linear function of temperature T throughout the model. This gives the condition

The predictions of this condition agree well with results for a set of stellar models 0 ≤ α ≤ 1, 0≤ β ≤ 5.

Type
Part I Convection and turbulence as the basis of magnetic activity
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 95 - 97
Copyright
Copyright © Springer-Verlag 1991

References

Naur, P., and Osterbrock, D.E.: 1953, “Convettive Cores in Stars”, Astrophys J. 117, 306.Google Scholar
Roxburgh, I.W.: 1985, “Present Problems of the Solar Interior”, Solar Physics, 100, 21.Google Scholar