Rapidly rotating stars. I. The self-consistent-field method
Abstract
A method is described by which one can determine the equilibrium structure of a star having kinetic energy of rotation comparable to its gravitational energy. It is assumed that the inertial forces are con- servative and that the star remains axially symmetrical. An iterative procedure is outlined by which the density distribution can be found which will be in equilibrium with the potential field derived from that density distribution In the present paper we emphasize the potential theory aspect of this problem
- Publication:
-
The Astrophysical Journal
- Pub Date:
- March 1968
- DOI:
- 10.1086/149506
- Bibcode:
- 1968ApJ...151.1075O