Towards a self-consistent relativistic model of the exterior gravitational field of rapidly rotating neutron stars

Abstract

We present a self-consistent, relativistic model of rapidly rotating neutron stars describing their exterior gravitational field. This is achieved by matching the new solution of Einstein's field equations found by Manko et al. (2000) and the numerical results for the interior of neutron stars with different equations of state calculated by Cook et al. (1994). This matching process gives constraints for the choice of the five parameters of the vacuum solution. Then we investigate some properties of the gravitational field of rapidly rotating neutron stars with these fixed parameters.

arXiv comment11 pages, 18 figures, accepted for publication in MNRAS

References in corpus (4)

• Highly accurate calculation of rotating neutron stars
• Energy Release During Disk Accretion onto a Rapidly Rotating Neutron Star
• Possible evidence of quark matter in neutron star X-ray binaries
• Remarks on the Charged, Magnetized Tomimatsu-Sato $\delta =2$ Solution

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