Quasiequilibrium sequences of synchronously rotating binary neutron stars with constant rest masses in general relativity -- Another approach without using the conformally flat condition --

Details Quasiequilibrium sequences of synchronously rotating binary neutron stars with constant rest masses in general relativity -- Another approach without using the conformally flat condition -- Quasiequilibrium sequences of synchronously rotating binary neutron stars with constant rest masses in general relativity -- Another approach without using the conformally flat condition --

2001-12-31

arxiv.org/abs/astro-ph/0112571v1

Phys.Rev. D65 (2002) 064030

Astronomy and Astrophysics

Astrophysics

15 pages (including 18 figures). Accepted for publication in Physical Review D. Scheduled to appear in 15 March, 2002

Scientific paper

10.1103/PhysRevD.65.064030

We have computed quasiequilibrium sequences of synchronously rotating compact binary star systems with constant rest masses. This computation has been carried out by using the numerical scheme which is different from the scheme based on the conformally flat assumption about the space. Stars are assumed to be polytropes with polytropic indices of N=0.5, N=1.0, and N=1.5. Since we have computed binary star sequences with a constant rest mass, they provide approximate evolutionary tracks of binary star systems. For relatively stiff equations of state (N < 1.0), there appear turning points along the quasiequilibrium sequences plotted in the angular momentum -- angular velocity plane. Consequently secular instability against exciting internal motion sets in at those points. Qualitatively, these results agree with those of Baumgarte et al. who employed the conformally flat condition. We further discuss the effect of different equations of state and different strength of gravity by introducing two kinds of dimensionless quantities which represent the angular momentum and the angular velocity. Strength of gravity is renormalized in these quantities so that the quantities are transformed to values around unity. Therefore we can clearly see relations among quasiequilibrium sequences for a wide variety of strength of gravity and for different compressibility.

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