Numerical models of irrotational binary neutron stars in general relativity

Details Numerical models of irrotational binary neutron stars in general relativity Numerical models of irrotational binary neutron stars in general relativity

1998-10-22

arxiv.org/abs/gr-qc/9810072v2

Phys.Rev.Lett. 82 (1999) 892-895

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

Minor corrections, improved figure, 5 pages, REVTeX, Phys. Rev. Lett. in press

Scientific paper

10.1103/PhysRevLett.82.892

We report on general relativistic calculations of quasiequilibrium configurations of binary neutron stars in circular orbits with zero vorticity. These configurations are expected to represent realistic situations as opposed to corotating configurations. The Einstein equations are solved under the assumption of a conformally flat spatial 3-metric (Wilson-Mathews approximation). The velocity field inside the stars is computed by solving an elliptical equation for the velocity scalar potential. Results are presented for sequences of constant baryon number (evolutionary sequences). Although the central density decreases much less with the binary separation than in the corotating case, it still decreases. Thus, no tendency is found for the stars to individually collapse to black hole prior to merger.

Affiliated with

Also associated with

No associations

Rating

Numerical models of irrotational binary neutron stars in general relativity does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Numerical models of irrotational binary neutron stars in general relativity, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Numerical models of irrotational binary neutron stars in general relativity will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-267100