Numerical study of synchronized binary neutron stars in the post-Newtonian approximation of general relativity

Details Numerical study of synchronized binary neutron stars in the post-Newtonian approximation of general relativity Numerical study of synchronized binary neutron stars in the post-Newtonian approximation of general relativity

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997phrvd..55.6019s&link_type=abstract

Physical Review D (Particles, Fields, Gravitation, and Cosmology), Volume 55, Issue 10, 15 May 1997, pp.6019-6029

Physics

32

Post-Newtonian Approximation, Perturbation Theory, Related Approximations, Wave Generation And Sources, Relativistic Stars: Structure, Stability, And Oscillations, Neutron Stars

Scientific paper

In order to investigate general relativistic effects on the hydrodynamic evolution of coalescing binary neutron stars (BNS's) just before merging, we numerically calculate equilibrium sequences of BNS's in synchronized circular orbits using the first post-Newtonian (PN) approximation of general relativity. The numerical solutions are obtained by solving the integral form of the Euler equation in the PN approximation for a uniformly rotating fluid, which was derived by Chandrasekhar. NS's are modeled by means of the polytropic equation of state with the polytropic exponent Γ=2, and the stiffness is adjusted using the polytropic constant K. From numerical calculations, we find that by the PN effect, the critical orbital radius rcrit, where the hydrodynamic instability pointed out by Lai, Rasio, and Shapiro occurs, becomes smaller than the Newtonian result and as a result the corresponding angular frequency at rcrit is larger than that of the Newtonian binary.

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