Speaker
Dr
Mehrab Momennia
(UMSNH)
Description
The dark matter-black hole interaction is modeled with the help of the accretion of a Vlasov gas into a rotating Kerr black hole. We provide exact analytic expressions for the particle, mass, and angular momentum accretion rates in the form of integrals. These integrals are computed numerically and compared to more explicit relations in the slow-rotation approximation. The explicit analytic formulas are used to derive characteristic time scales of the black hole mass growth and the associated spin-down in two different scenarios: assuming that the ambient energy density is either constant or decreases on a cosmological scale.