Dark Matter Signatures of Supermassive Black Hole Binaries

被引：10

作者：

Naoz, Smadar ^{[1
,2
]}

Silk, Joseph ^{[3
,4
,5
]}

Schnittman, Jeremy D. ^{[6
,7
]}

机构：

[1] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA

[2] Univ Calif Los Angeles, Mani L Bhaumik Inst Theoret Phys, Los Angeles, CA 90095 USA

[3] Sorbonne Univ, Inst Astrophys Paris, UMR CNRS 7095, 98 Bis,Blvd Arago, F-75014 Paris, France

[4] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[5] Univ Oxford, Beecroft Inst Particle Astrophys & Cosmol, Oxford OX1 3RH, England

[6] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

[7] Maryland Joint Space Sci Inst, College Pk, MD 20742 USA

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2019年 / 885卷 / 02期

关键词：

Black hole physics; Dark matter; Supermassive black holes; Double quasars; Galaxy nuclei; ACTIVE GALACTIC NUCLEUS; QUASARS; ECCENTRICITY; ACCRETION; EVOLUTION; DISCOVERY; MODEL; PAIR; MASS;

D O I：

10.3847/2041-8213/ab4fed

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

A natural consequence of the galaxy formation paradigm is the existence of supermassive black hole (SMBH) binaries. Gravitational perturbations from a far-away SMBH companion can induce high orbital eccentricities on dark matter (DM) particles orbiting the primary SMBH via the eccentric Kozai?Lidov mechanism. This process yields an influx of DM particles into the primary SMBH ergosphere, where test particles linger for long timescales. This influx results in high self-gravitating densities, forming a DM clump that is extremely close to the SMBH. In such a situation, the gravitational-wave (GW) emission between the dark matter clump and the SMBH is potentially detectable by LISA. If dark matter self-annihilates, the high densities of the clump will result in a unique codetection of GW emission and high-energy electromagnetic signatures.

引用

页数：6

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