Rapidly rotating, post-Newtonian neutron stars
Equilibrium models of rapidly rotating neutron stars supported by nonrelativistic, degenerate neutrons are examined in the Parametrized Post-Newtonian (PPN) framework. An energy variational principle is employed to analyze the effects of rapid rotation and relativistic gravity on the mass-density relation and maximum mass of neutron stars. The fractional increase in the mass of stable, equilibrium configurations due to rotation is smaller for neutron stars than for white dwarfs, a consequence of the destabilizing effects of post-Newtonian gravity. Currently viable conservative theories of gravity with high values of the PPN parameter ..beta.. can have significantly larger masses than predicted by general relativity. Also discussed qualitatively is the evolution of transient, rotating compact objects called ''fizzlers,'' which contract to form pulsars and black holes on secular (gravitational radiation) time scales. (AIP)
- Research Organization:
- Center for Radiophysics and Space Research, Cornell University
- OSTI ID:
- 7175705
- Journal Information:
- Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 207:1; ISSN ASJOA
- Country of Publication:
- United States
- Language:
- English
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