m=1 instability and gravitational wave signal in binary neutron star mergers

被引：51
作者：
Lehner, Luis [1 ]
Liebling, Steven L. [2 ]
Palenzuela, Carlos [3 ,4 ]
Motl, Patrick M. [5 ]
机构：
[1] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada
[2] Long Isl Univ, Dept Phys, Greenvale, NY 11548 USA
[3] Univ Illes Balears, Dept Fis, E-07122 Palma de Mallorca, Baleares, Spain
[4] Inst Estudis Espacials & Catalunya, E-07122 Palma de Mallorca, Baleares, Spain
[5] Indiana Univ Kokomo, Sch Sci, Kokomo, IN 46904 USA
来源：
PHYSICAL REVIEW D | 2016年 / 94卷 / 04期
基金：
加拿大自然科学与工程研究理事会; 美国国家科学基金会;
关键词：
NUMERICAL RELATIVITY; EQUATIONS;
D O I：
10.1103/PhysRevD.94.043003
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We examine the development and detectability of the m = 1 instability in the remnant of binary neutron star mergers. The detection of the gravitational mode associated with the m = 1 degree of freedom could potentially reveal details of the equation of state. We analyze the postmerger epoch of simulations of both equal- and nonequal-mass neutron star mergers using three realistic, microphysical equations of state and neutrino cooling. Our studies show such an instability develops generically and within a short dynamical time to strengths that are comparable to or stronger than the m = 2 mode, which is the strongest during the early postmerger stage. We estimate the signal to noise ratio that might be obtained for the m = 1 mode and discuss the prospects for observing this signal with available Earth-based detectors. Because the m = 1 occurs at roughly half the frequency of the more powerful m = 2 signal and because it can potentially be long lived, targeted searches could be devised to observe it. We estimate that with constant amplitude direct detection of the mode could occur up to a distance of roughly 14 Mpc, whereas a search triggered by the inspiral signal could extend this distance to roughly 100 Mpc.
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页数：9
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