Simulations of black-hole binaries with unequal masses or nonprecessing spins: Accuracy, physical properties, and comparison with post-Newtonian results

被引：58

作者：

Hannam, Mark ^{[1
,2
]}

Husa, Sascha ^{[3
]}

Ohme, Frank ^{[4
]}

Mueller, Doreen ^{[5
]}

Bruegmann, Bernd ^{[5
]}

机构：

[1] Univ Vienna, Fac Phys, A-1090 Vienna, Austria

[2] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales

[3] Univ Illes Balears, Dept Fis, E-07122 Palma de Mallorca, Spain

[4] Max Planck Inst Gravitat Phys, D-14475 Potsdam, Germany

[5] Univ Jena, Inst Theoret Phys, D-07743 Jena, Germany

来源：

PHYSICAL REVIEW D | 2010年 / 82卷 / 12期

基金：

英国科学技术设施理事会;

关键词：

GRAVITATIONAL-WAVES; COMPACT BINARIES; INITIAL DATA; DYNAMICS; EQUATIONS; SYSTEMS; MOTION; MERGER; ORDER;

D O I：

10.1103/PhysRevD.82.124008

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present gravitational waveforms for the last orbits and merger of black-hole-binary systems along two branches of the black-hole-binary parameter space: equal-mass binaries with equal nonprecessing spins, and nonspinning unequal-mass binaries. The waveforms are calculated from numerical solutions of Einstein's equations for black-hole binaries that complete between six and ten orbits before merger. Along the equal-mass spinning branch, the spin parameter of each black hole is chi(i) = S-i/M-i(2) is an element of [-0.85, 0.85], and along the unequal-mass branch the mass ratio is q = M-2/M-1 is an element of [1, 4]. We discuss the construction of low-eccentricity puncture initial data for these cases, the properties of the final merged black hole, and compare the last 8-10 gravitational-wave cycles up to M omega = 0.1 with the phase and amplitude predicted by standard post-Newtonian (PN) approximants. As in previous studies, we find that the phase from the 3.5PN TaylorT4 approximant is most accurate for nonspinning binaries. For equal-mass spinning binaries the 3.5PN TaylorT1 approximant (including spin terms up to only 2.5PN order) gives the most robust performance, but it is possible to treat TaylorT4 in such a way that it gives the best accuracy for spins chi(i) > -0.75. When high-order amplitude corrections are included, the PN amplitude of the (l = 2, m = +/- 2) modes is larger than the numerical relativity amplitude by between 2-4%.

引用

页数：22

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