Modeling multipolar gravitational-wave emission from small mass-ratio mergers

被引：54

作者：

Barausse, Enrico ^{[1
,2
]}

Buonanno, Alessandra ^{[1
,2
,3
]}

Hughes, Scott A. ^{[4
,5
]}

Khanna, Gaurav ^{[6
]}

O'Sullivan, Stephen ^{[4
,5
]}

Pan, Yi ^{[1
,2
]}

机构：

[1] Univ Maryland, Maryland Ctr Fundamental Phys, Dept Phys, College Pk, MD 20742 USA

[2] Univ Maryland, Joint Space Sci Inst, Dept Phys, College Pk, MD 20742 USA

[3] Harvard Univ, Radcliffe Inst Adv Study, Cambridge, MA 02138 USA

[4] MIT, Dept Phys, Cambridge, MA 02139 USA

[5] MIT Kavli Inst, Cambridge, MA 02139 USA

[6] Univ Massachusetts Dartmouth, Dept Phys, N Dartmouth, MA 02747 USA

来源：

PHYSICAL REVIEW D | 2012年 / 85卷 / 02期

基金：

美国国家科学基金会;

关键词：

BLACK-HOLE; PERTURBATIONS; STABILITY;

D O I：

10.1103/PhysRevD.85.024046

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using the effective-one-body (EOB) formalism and a time-domain Teukolsky code, we generate inspiral, merger, and ringdown waveforms in the small-mass-ratio limit. We use EOB inspiral and plunge trajectories to build the Teukolsky-equation source term, and compute full coalescence waveforms for a range of black-hole spins. By comparing EOB waveforms that were recently developed for comparable-mass binary black holes to these Teukolsky waveforms, we improve the EOB model for the (2, 2), (2, 1), (3, 3), and (4, 4) modes. Our results can be used to quickly and accurately extract useful information about merger waves for binaries with spin and should be useful for improving analytic models of such binaries.

引用

页数：19

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