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Dark Matter Signatures of Supermassive Black Hole Binaries

, and . (2019)cite arxiv:1905.03790Comment: 5 pages, 3 figures, submitted.

Abstract

A natural consequence of the galaxy formation paradigm is the existence of supermassive black hole (SMBH) binaries. Gravitational perturbations from a massive far away SMBH can induce high orbital eccentricities on dark matter particles orbiting the primary SMBH, via the eccentric Kozai-Lidov mechanism. This process yields an influx of dark matter particles into the primary SMBH ergosphere, where test particles linger for long timescales. This influx results in high self-gravitating densities, forming a dark matter clump extremely close to the SMBH. In such a situation, the gravitational wave 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 co-detection of gravitational wave emission and high energy electromagnetic signatures.

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Dark Matter Signatures of Supermassive Black Hole Binaries

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