Hostname: page-component-cd9895bd7-mkpzs Total loading time: 0 Render date: 2024-12-23T15:39:50.807Z Has data issue: false hasContentIssue false
  • English
  • Français

Evolution of A Rotating Star of Nine Solar Masses

Published online by Cambridge University Press:  12 April 2016

R. Kippenhahn ,
E. Meyer-Hofmeister  and
H.-C. Thomas
R. Kippenhahn
Affiliation:
Universitätssternwarte Göt fingen and Max-Planck-Institut für Physik und Astrophysik, München, Germany
E. Meyer-Hofmeister
Affiliation:
Universitätssternwarte Göt fingen and Max-Planck-Institut für Physik und Astrophysik, München, Germany
H.-C. Thomas
Affiliation:
Universitätssternwarte Göt fingen and Max-Planck-Institut für Physik und Astrophysik, München, Germany

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.

To compute the evolution of a rotating star, the following approximations were used in order to obtain some of the main effects of rotation with simple models of spherical symmetry:

Type
Part I / The Effects of Rotation on Stellar Interiors and Evolution
Information
International Astronomical Union Colloquium , Volume 4: Stellar Rotation , 1970 , pp. 60 - 62
Copyright
Copyright © Reidel 1970

References

Fricke, K.: 1968, Z. Astrophys. 68, 317.CrossRefGoogle Scholar
Goldreich, P. and Schubert, G., 1967, Astrophys. J. 150, 571.CrossRefGoogle Scholar
Kippenhahn, R., Weigert, A., and Hofmeister, E.: 1967, in Methods in Computational Physics, vol. 7, (ed. by Alder, B., Fernbach, S., and Rothenberg, M.), Academic Press, New York and London, p. 129.Google Scholar
Mestel, L.: 1953, Monthly Notices Roy. Astron. Soc. 113, 716.CrossRefGoogle Scholar