Structure and evolution of very close binary systems. I. Stucture equations including rotational and tidal distortions and calculations for 2, 1, and 0.65 M sun zeroage mainsequence stars.
Abstract
A method is developed which allows an efficient and accurate investigation of the structure and evolution of a rotationally and tidally distorted star in a close binary system. The method involves no division into different approximation regimes, and the structure equations are written in essentially the same form as the one for spherical stars. The explicit effects of the distortions are included through basically just one correction factor which can be readily calculated. We also discuss in some detail the envelope integration in the case of superadiabatic convection. Models for zeroage mainsequence stars of 2, 1, and 0.65 M0 are computed as a check on our formulation and compared with those obtained using other methods. Subject headings: stars: binaries  stars: evolution  stars: interiors  stars: rotation
 Publication:

The Astrophysical Journal
 Pub Date:
 November 1979
 DOI:
 10.1086/157458
 Bibcode:
 1979ApJ...233..950C
 Keywords:

 Binary Stars;
 Stellar Evolution;
 Stellar Models;
 Stellar Structure;
 Main Sequence Stars;
 Mathematical Models;
 Tables (Data);
 Astrophysics;
 Close Binaries:Evolution;
 Close Binaries:Structure