Hostname: page-component-8448b6f56d-c47g7 Total loading time: 0 Render date: 2024-04-23T22:32:16.561Z Has data issue: false hasContentIssue false
  • English
  • Français

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

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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