## Equilibrium sequences of rotating neutron stars for new realistic Equations of State
^{1} Indian Institute of Astrophysics, Bangalore 560
034,India^{2} Dipartimento di Fisica, Universitá di Pisa, and
INFN Sezione di Pisa, Piazza Torricelli 2, I-56100 Pisa, Italy
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 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 ) before the maximum- models. We calculate equilibrium sequences for a constant value of corresponding to the most rapidly rotating pulsar PSR 1937+21. Also calculated is the radius of the marginally stable orbit and its dependence on , relevant for modeling of kilo-Hertz quasi-periodic oscillations in X-ray binaries.
* Also at Raman Research Institute, Bangalore 560 080, INDIA ## Contents- 1. Introduction
- 2. Rapidly and rigidly rotating relativistic stars
- 3. Numerical procedure
- 4. New Equation of State models
- 5. Results and discussion
- 5.1. EOS model BPAL21
- 5.2. EOS model BBB1
- 5.3. EOS model BBB2
- 5.4. EOS model BPAL32
- References
© European Southern Observatory (ESO) 1998 Online publication: June 2, 1998 |