Hostname: page-component-cd9895bd7-dzt6s Total loading time: 0 Render date: 2024-12-13T08:36:00.354Z Has data issue: false hasContentIssue false
  • English
  • Français

Convective motions as an indicator of solar structure

Published online by Cambridge University Press:  04 August 2017

R. Van der Borght  and
P. Fox
R. Van der Borght
Affiliation:
Monash University, Clayton (Vic.) Australia
P. Fox
Affiliation:
Monash University, Clayton (Vic.) Australia

Extract

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.

Most stars contain regions which are convectively unstable and one of the more daunting tasks facing astrophysics today is to find a satisfactory theoretical formulation of turbulent energy transport in stars. Various theories have been proposed, such as the mixing-length formalism and its extensions, and it would be most useful if one could test the accuracy of such models in view of their importance in the theory of stellar structure and evolution.

Type
I. EVOLUTION OF LOW AND INTERMEDIATE MASS STARS OBSERVATIONS AND MODELS
Information
Symposium - International Astronomical Union , Volume 105: Observational Tests of the Stellar Evolution Theory , 1984 , pp. 71 - 74
Copyright
Copyright © Reidel 1984 

References

Böhm, K.H., Astrophys. J., 137, 881 (1963).CrossRefGoogle Scholar
Graham, E. and Moore, D.R., Mon. Not. R. Astron. Soc., 183, 617 (1978).Google Scholar
Kohl, K., Z. f. Ap., 64, 472 (1966).Google Scholar
Van der Borght, R., Proc. Astr. Soc. Aust., 3, 91 (1977).CrossRefGoogle Scholar
Van der Borght, R., J. Comp. Appl. Math., 6, 283 (1980).CrossRefGoogle Scholar
Van der Borght, R. and Fox, P., Proc. Astr. Soc. Aust., 5 (1983) (to appear).CrossRefGoogle Scholar