Equilibrium structures of rotationally and tidally distorted stellar models

Details Equilibrium structures of rotationally and tidally distorted stellar models Equilibrium structures of rotationally and tidally distorted stellar models

Jan 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ap%26ss.163...23m&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 163, no. 1, Jan. 1990, p. 23-39.

Statistics

Computation

12

Binary Stars, Gravitational Effects, Main Sequence Stars, Stellar Models, Stellar Rotation, Companion Stars, Computational Astrophysics, Distortion, Roche Limit, Stellar Structure

Scientific paper

A method is presented for computing the equilibrium structures of rotationally distorted stars and the rotationally and tidally distorted primary components of stars in binary systems. The method is based on the averaging technique of Kippenhahn and Thomas (1970) and utilizes the concepts of Roche equipotentials (Kopal, 1972). The method takes into account terms up to second-order of smallness in the rotational and tidal distortion parameters. The use of the method in obtaining the equilibrium structures of certain rotationally and/or tidally distorted models of main-sequence stars is illustrated.

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