Comparisons of eccentric binary black hole simulations with post-Newtonian models

被引：95

作者：

Hinder, Ian ^{[1
]}

Herrmann, Frank ^{[2
]}

Laguna, Pablo ^{[3
]}

Shoemaker, Deirdre ^{[3
]}

机构：

[1] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Golm, Germany

[2] Univ Maryland, Dept Phys, College Pk, MD 20742 USA

[3] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA

来源：

PHYSICAL REVIEW D | 2010年 / 82卷 / 02期

基金：

美国国家科学基金会;

关键词：

GRAVITATIONAL-RADIATION; KOZAI MECHANISM; EVOLUTION; SYSTEMS; MOTION; WAVES; SPIN; LIGO;

D O I：

10.1103/PhysRevD.82.024033

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present the first comparison between numerical relativity (NR) simulations of an eccentric binary black hole system with corresponding post-Newtonian (PN) results. We evolve an equal-mass, non-spinning configuration with an initial eccentricity e approximate to 0: 1 for 21 gravitational wave cycles before merger, and find agreement in the gravitational wave phase with an adiabatic eccentric PN model with 2 PN radiation reaction within 0.1 radians for 10 cycles. The NR and PN phase difference grows to 0.7 radians by 5 cycles before merger. We find that these results can be obtained by expanding the eccentric PN expressions in terms of the frequency-related variable x = (omega M)(2/3) with M the total mass of the binary. When using instead the mean motion n = 2 pi/P, where P is the orbital period, the comparison leads to significant disagreements with NR.

引用

页数：15

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