General relativistic models of binary neutron stars in quasiequilibrium

被引:112
作者
Baumgarte, TW [1 ]
Cook, GB
Scheel, MA
Shapiro, SL
Teukolsky, SA
机构
[1] Univ Illinois, Dept Phys, Urbana, IL 61801 USA
[2] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA
[3] Univ Illinois, Dept Astron, Urbana, IL 61801 USA
[4] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA
[5] Cornell Univ, Dept Phys, Ithaca, NY 14853 USA
[6] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA
关键词
D O I
10.1103/PhysRevD.57.7299
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We perform fully relativistic calculations of binary neutron stars in corotating, circular orbit. While Newtonian gravity allows for a strict equilibrium, a relativistic binary system emits gravitational radiation, causing the system to lose energy and slowly spiral inwards. However, since inspiral occurs on a time scale much longer than the orbital period, we can treat the binary to be in quasiequilibrium. In this approximation, we integrate a subset of the Einstein equations coupled to the relativistic equation of hydrostatic equilibrium to solve the initial value problem for binaries of arbitrary separation. We adopt a polytropic equation of state to determine the structure and maximum mass of neutron stars in close binaries for polytropic indices n = 1, 1.5 and 2. We construct sequences of constant rest-mass and locate turning points along energy equilibrium curves to identify the onset of orbital instability. In particular, we locate the innermost stable circular orbit and its angular velocity. We construct the first contact binary systems in full general relativity. These arise whenever the equation of state is sufficiently soft (n greater than or similar to 1.5). A radial stability analysis reveals no tendency for neutron stars in close binaries to collapse to black holes prior to merger.
引用
收藏
页码:7299 / 7311
页数:13
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