Close-limit approximation to neutron star collisions

被引:18
作者
Allen, GD [1 ]
Andersson, N
Kokkotas, KD
Laguna, P
Pullin, JA
Ruoff, J
机构
[1] Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany
[2] Univ Southampton, Dept Math, Southampton SO17 1BJ, Hants, England
[3] Aristotelian Univ Salonika, Dept Math, GR-54006 Salonika, Greece
[4] Penn State Univ, Ctr Gravitat Phys & Geometry, University Pk, PA 16802 USA
[5] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany
来源
PHYSICAL REVIEW D | 1999年 / 60卷 / 10期
基金
美国国家科学基金会;
关键词
D O I
10.1103/PhysRevD.60.104021
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We develop a close-limit approximation to the head-on collision of two neutron stars similar to that used to treat the merger of black hole binaries. This approximation can serve as a useful benchmark test for future fully non-linear studies. For neutron star binaries, the close-limit approximation involves assuming that the merged object can be approximated as a perturbed, stable neutron star during the ring-down phase of the coalescence. We introduce a prescription for the construction of initial data sets, discuss the physical plausibility of the various assumptions involved, and briefly investigate the character of the gravitational radiation produced during the merger. The numerical results show that several of the merged object's fluid pulsation modes are excited to a significant level. [S0556-2821(99)06422-X].
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页数:3
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