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Dark Matter Signatures of Supermassive Black Hole Binaries

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arxiv 1905.03790 v2 pith:OLBEGJOZ submitted 2019-05-09 astro-ph.HE

Smadar Naoz , Joseph Silk , Jeremy D. Schnittman This is my paper · ORCID
classification astro-ph.HE
keywords darkmattersmbhhighclumpgravitationalparticlesbinaries
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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 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 that is 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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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Triple radio flares from tidal disruption events: jet-wind collisions and the discovery of a third radio flare from AT2020vwl

    astro-ph.HE 2026-07 conditional novelty 7.0 of 10

    The TDE AT2020vwl showed a third radio flare at the time a jet-wind collision was predicted from its first two flares, the first predicted-and-confirmed third flare.

  2. Black hole supercolliders

    gr-qc 2025-06 conditional novelty 5.0 of 10

    Retrograde plunging accretion flows around near-extremal Kerr black holes can collide with free-falling particles at TeV-scale center-of-mass energies.

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