Electromagnetic chirp of a compact binary black hole: A phase template for the gravitational wave inspiral

被引：57

作者：

Haiman, Zoltan ^{[1
,2
]}

机构：

[1] Columbia Univ, Dept Astron, 550 West 120th St, New York, NY 10027 USA

[2] NYU, Dept Phys, 4 Washington Pl, New York, NY 10003 USA

来源：

PHYSICAL REVIEW D | 2017年 / 96卷 / 02期

关键词：

X-RAY; GENERAL-RELATIVITY; ACCRETION DISKS; MASS; EVOLUTION; EMISSION; DYNAMICS; MERGERS; MODEL; DISCS;

D O I：

10.1103/PhysRevD.96.023004

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The gravitational waves (GWs) from a binary black hole (BBH) with masses 10(4) less than or similar to M less than or similar to 10(7) M-circle dot can be detected with the Laser Interferometer Space Antenna (LISA) once their orbital frequency exceeds 10(-4)-10(-5) Hz. The binary separation at this stage is a = O(100)R-g (gravitational radius), and the orbital speed is v/c = O(0.1). We argue that at this stage, the binary will be producing bright electromagnetic (EM) radiation via gas bound to the individual BHs. Both BHs will have their own photospheres in x-ray and possibly also in optical bands. Relativistic Doppler modulations and lensing effects will inevitably imprint periodic variability in the EM light curve, tracking the phase of the orbital motion, and serving as a template for theGWinspiral waveform. Advanced localization of the source by LISAweeks to months prior to merger will enable a measurement of this EM chirp by wide-field x-ray or optical instruments. A comparison of the phases of the GWand EM chirp signals will help break degeneracies between system parameters, and probe a fractional difference Delta v in the propagation speed of photons and gravitons as low as Delta v/c approximate to 10(-17).

引用

页数：8

共 64 条

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