Post-Newtonian Models of Differentially Rotating Neutron Stars

Details Post-Newtonian Models of Differentially Rotating Neutron Stars Post-Newtonian Models of Differentially Rotating Neutron Stars

2002-07-24

arxiv.org/abs/gr-qc/0207097v1

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

22 pages, 9 figures, submitted to Phys. Rev. D

Scientific paper

A self-consistent field method is developed, which can be used to construct models of differentially rotating stars to first post-Newtonian order. The rotation law is specified by the specific angular momentum distribution j(m), where m is the baryonic mass fraction inside the surface of constant specific angular momentum. The method is then used to compute models of the nascent neutron stars resulting from the accretion induced collapse of white dwarfs. The result shows that the ratios of kinetic energy to gravitational binding energy of the relativistic models are slightly smaller than the corresponding values of the Newtonian models.

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