EQUILIBRIUM SEQUENCES OF ROTATING NEUTRON-STARS FOR NEW REALISTIC EQUATIONS OF STATE

For four newly suggested realistic 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 suprama ssive evolutionary sequences of constant rest mass. We find that for t hese equations of state the maximum (gravitational) mass rotating mode ls occur (in central density and rotation rate Omega) before the maxim um-Omega models. We calculate equilibrium sequences for a constant val ue 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, relevant for modeling of kilo-Hertz quasi-per iodic oscillations in X-ray binaries.