Final spin and radiated energy in numerical simulations of binary black holes with equal masses and equal, aligned or antialigned spins

被引：75

作者：

Hemberger, Daniel A. ^{[1
]}

Lovelace, Geoffrey ^{[2
,3
]}

Loredo, Thomas J. ^{[1
]}

Kidder, Lawrence E. ^{[1
]}

Scheel, Mark A. ^{[3
]}

Szilagyi, Bela ^{[3
]}

Taylor, Nicholas W. ^{[3
]}

Teukolsky, Saul A. ^{[1
]}

机构：

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

[2] Calif State Univ Fullerton, Gravitat Wave Phys & Astron Ctr, Fullerton, CA 92831 USA

[3] CALTECH, Pasadena, CA 91125 USA

来源：

PHYSICAL REVIEW D | 2013年 / 88卷 / 06期

基金：

美国国家科学基金会; 加拿大创新基金会;

关键词：

CALIBRATION; EVOLUTION;

D O I：

10.1103/PhysRevD.88.064014

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The behavior of merging black holes (including the emitted gravitational waves and the properties of the remnant) can currently be computed only by numerical simulations. This paper introduces ten numerical relativity simulations of binary black holes with equal masses and equal spins aligned or antialigned with the orbital angular momentum. The initial spin magnitudes have vertical bar chi(i vertical bar) less than or similar to & 0: 95 and are more concentrated in the aligned direction because of the greater astrophysical interest of this case. We combine these data with five previously reported simulations of the same configuration, but with different spin magnitudes, including the highest spin simulated to date, chi(i) approximate to 0: 97. This data set is sufficiently accurate to enable us to offer improved analytic fitting formulas for the final spin and for the energy radiated by gravitational waves as a function of initial spin. The improved fitting formulas can help to improve our understanding of the properties of binary black hole merger remnants and can be used to enhance future approximate waveforms for gravitational wave searches, such as effective-one-body waveforms.

引用

页数：13

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