Dark Matter Signatures of Supermassive Black Hole Binaries
S. Naoz, and J. Silk. (2019)cite arxiv:1905.03790Comment: 5 pages, 3 figures, submitted.
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