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A Simple Method for the Solution of the Stellar Structure Equations Including Rotation and Tidal Forces

Published online by Cambridge University Press:  12 April 2016

R. Kippenhahn  and
H.-C. Thomas
R. Kippenhahn
Affiliation:
Universitätssternwarte Göttingen and Max-Planck-Institut für Physik und Astrophysik, München, Germany
H.-C. Thomas
Affiliation:
Universitätssternwarte Göttingen and Max-Planck-Institut für Physik und Astrophysik, München, Germany

Abstract

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In the following a method is presented for computing the internal structure of nonspherical stars assuming that the force per gram causing the deviation from spherical symmetry is conservative. The method has the advantage that in a normal (spherical) stellar structure code only slight changes have to be made in order to obtain nonspherical stellar models. The method can be applied as well to rotating stars as to stars distorted by tidal effects. Although it is similar to that of Faulkner et al. (1968) in the case of purely rotating stars, it is not necessary to use the division into two zones, where either slow rotation or negligible contribution to the gravitional potential is assumed.

Type
Part I / The Effects of Rotation on Stellar Interiors and Evolution
Information
International Astronomical Union Colloquium , Volume 4: Stellar Rotation , 1970 , pp. 20 - 29
Copyright
Copyright © Reidel 1970

References

Faulkner, J., Roxburgh, I. W., and Strittmatter, P. A.: 1968, Astrophys. J. 151, 203.CrossRefGoogle Scholar
Jackson, S.: 1970, Astrophys. J. (in press).Google Scholar
Kippenhahn, R., Thomas, H.-C., and Weigert, A.: 1968, Z. Astrophys. 69, 265.Google Scholar
Sackmann, I. J. and Anand, S. P. S.: 1969, preprint.Google Scholar