Binary neutron stars in quasiequilibrium
Binary neutron stars in quasiequilibrium
复制标题
准平衡中的双中子星
DOI：
10.1088/0067-0049/188/1/187
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发表时间：
2010
期刊：
影响因子：
--
通讯作者：
K. Taniguchi and M. Shibata
中科院分区：
文献类型：
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作者：
Hajime Ishimori;Morimitsu Tanimoto;貞廣泰造;K. Taniguchi and M. Shibata
在广义相对论的各种状态方程下，构造了中子星双星的准平衡序列。在Isenberg-Wilson-马修斯近似下，将Einstein的约束方程与流体定常平衡的相对论方程在无旋流动假设下一起求解。我们专注于不等质量序列以及等质量序列，并比较这些结果。我们研究了中子星星的质量比、总质量和状态方程随时间变化时，准平衡序列、序列端点、轨道角速度的结合能和总角动量沿着的行为.发现质量脱落极限下的轨道角速度可由解析估算得出的经验公式确定。我们还提供了160个序列的表，这将是有用的指导方针的数值模拟的螺旋和合并在不久的将来进行。
Quasi-equilibrium sequences of binary neutron stars are constructed for a variety of equations of state in general relativity. Einstein's constraint equations in the Isenberg–Wilson–Mathews approximation are solved together with the relativistic equations of hydrostationary equilibrium under the assumption of irrotational flow. We focus on unequal-mass sequences as well as equal-mass sequences, and compare those results. We investigate the behavior of the binding energy and total angular momentum along a quasi-equilibrium sequence, the endpoint of sequences, and the orbital angular velocity as a function of time, changing the mass ratio, the total mass of the binary system, and the equation of state of a neutron star. It is found that the orbital angular velocity at the mass-shedding limit can be determined by an empirical formula derived from an analytic estimation. We also provide tables for 160 sequences, which will be useful as a guideline of numerical simulations for the inspiral and merger performed in the near future.