Slowly Rotating Relativistic Stars. II. Models for Neutron Stars and Supermassive Stars
Abstract
The equilibrium configurations of rigidly rotating white dwarfs and neutron stars are calculated using the Harrison-Wheeler and the Tsuruta-Cameron V1 equations of state, along with the general-relativistic equations of structure. The equations of structure used are the exact relativistic equations with one ex- ception: they have been expanded in powers of the angular velocity ~2, and terms of higher order than ~ have been neglected. The equilibrium configurations of slowly rotating supermassive stars are also calculated
- Publication:
-
The Astrophysical Journal
- Pub Date:
- September 1968
- DOI:
- 10.1086/149707
- Bibcode:
- 1968ApJ...153..807H