Equilibrium Sequences of Rotating Neutron Stars for New Microscopic Equations of State

Abstract

For four newly suggested microscopic equations of state of neutron star matter, we construct equilibrium sequences of rapidly rotating neutron stars in general relativity. The sequences are the normal and supramassive evolutionary sequences of constant rest mass. We find that for these equations of state the maximum (gravitational) mass rotating models occur (in central density and rotation rate $\Omega$) before the maximum--$\Omega$ models. We calculate equilibrium sequences for a constant value of $\Omega$ corresponding to the most rapidly rotating pulsar PSR 1937+21. Also calculated is the radius of the marginally stable orbit and its dependence on $\Omega$.

Accepted for publication in main journal of Astronomy and Astrophysics. Replaced with a new version of manuscript (previous submission was a wrong version and did not contain all figures). 6 pages manuscript with 5 tables and 8 figures separate

Cited by in corpus (1)

• Rotating Stars in Relativity