Gravitational waveforms for neutron star binaries from binary black hole simulations

被引：26

作者：

Barkett, Kevin ^{[1
]}

Scheel, Mark A. ^{[1
]}

Haas, Roland ^{[1
,2
]}

Ott, Christian D. ^{[1
]}

Bernuzzi, Sebastiano ^{[1
,3
,4
]}

Brown, Duncan A. ^{[5
]}

Szilagyi, Bela ^{[6
]}

Kaplan, Jeffrey D. ^{[1
]}

Lippuner, Jonas ^{[1
]}

Muhlberger, Curran D. ^{[7
]}

Foucart, Francois ^{[8
,9
]}

Duez, Matthew D. ^{[10
]}

机构：

[1] CALTECH, Walter Burke Inst Theoret Phys, TAPIR, Pasadena, CA 91125 USA

[2] Max Planck Inst Gravitat Phys, Albert Einstein Inst, Potsdam, Germany

[3] Univ Parma, DiFeST, I-43124 Parma, Italy

[4] INFN Parma, I-43124 Parma, Italy

[5] Syracuse Univ, Dept Phys, Syracuse, NY 13244 USA

[6] CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA

[7] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA

[8] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA

[9] Univ Toronto, Canadian Inst Theoret Astrophys, 60 St George St, Toronto, ON M5S 3H8, Canada

[10] Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA

来源：

PHYSICAL REVIEW D | 2016年 / 93卷 / 04期

基金：

美国国家科学基金会; 加拿大创新基金会;

关键词：

D O I：

10.1103/PhysRevD.93.044064

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Gravitational waves from binary neutron star (BNS) and black hole/neutron star (BHNS) inspirals are primary sources for detection by the Advanced Laser Interferometer Gravitational-Wave Observatory. The tidal forces acting on the neutron stars induce changes in the phase evolution of the gravitational waveform, and these changes can be used to constrain the nuclear equation of state. Current methods of generating BNS and BHNS waveforms rely on either computationally challenging full 3D hydrodynamical simulations or approximate analytic solutions. We introduce a new method for computing inspiral waveforms for BNS/BHNS systems by adding the post-Newtonian (PN) tidal effects to full numerical simulations of binary black holes (BBHs), effectively replacing the nontidal terms in the PN expansion with BBH results. Comparing a waveform generated with this method against a full hydrodynamical simulation of a BNS inspiral yields a phase difference of <1 radian over similar to 15 orbits. The numerical phase accuracy required of BNS simulations to measure the accuracy of the method we present here is estimated as a function of the tidal deformability parameter lambda.

引用

页数：6

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