N-BODY DYNAMICS OF INTERMEDIATE MASS-RATIO INSPIRALS IN STAR CLUSTERS

被引：39

作者：

Haster, Carl-Johan ^{[1
,2
,3
]}

Antonini, Fabio ^{[2
,3
]}

Kalogera, Vicky ^{[2
,3
]}

Mandel, Ilya ^{[1
]}

机构：

[1] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England

[2] CIERA, 2145 Sheridan Rd, Evanston, IL 60208 USA

[3] Dept Phys & Astron, 2145 Sheridan Rd, Evanston, IL 60208 USA

来源：

ASTROPHYSICAL JOURNAL | 2016年 / 832卷 / 02期

关键词：

black hole physics; gravitation; gravitational waves; BLACK-HOLE BINARIES; ALGORITHMIC REGULARIZATION; PRIMORDIAL BINARIES; GRAVITATIONAL-WAVES; KOZAI MECHANISM; STELLAR-MASS; EVOLUTION; ECCENTRICITY; MERGERS; PERTURBATIONS;

D O I：

10.3847/0004-637X/832/2/192

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The intermediate mass-ratio inspiral of a stellar compact remnant into an intermediate-mass black hole (IMBH) can produce a gravitational wave (GW) signal that is potentially detectable by current ground-based GW detectors (e.g., Advanced LIGO) as well as by planned space-based interferometers (e.g., eLISA). Here, we present results from a direct integration of the post-Newtonian N-body equations of motion describing stellar clusters containing an IMBH and a population of stellar-mass black holes (BHs) and solar-mass stars. We take particular care to simulate the dynamics closest to the IMBH, including post-Newtonian effects up to an order of 2.5. Our simulations show that the IMBH readily forms a binary with a BH companion. This binary is gradually hardened by transient three-body or four-body encounters, leading to frequent substitutions of the BH companion, while the binary's eccentricity experiences large-amplitude oscillations due to the Lidov-Kozai resonance. We also demonstrate suppression of these resonances by the relativistic precession of the binary orbit. We find an intermediate mass-ratio inspiral in 1 of the 12 cluster models we evolved for similar to 100 Myr. This cluster hosts a 100M circle dot IMBH embedded in a population of 32 10M circle dot BH and 32,000 1M circle dot stars. At the end of the simulation, after similar to 100 Myr of evolution, the IMBH merges with a BH companion. The IMBH-BH binary inspiral starts in the eLISA frequency window (greater than or similar to 1 mHz) when the binary reaches an eccentricity1-e similar or equal to 10(-3). After similar or equal to 10(5) yr the binary moves into the LIGO frequency band with a negligible eccentricity. We comment on the implications for GW searches, with a possible detection within the next decade.

引用

页数：11

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