Speaker
Description
We present spherically symmetric fluid simulations of black hole accretion in self-interacting dark matter (SIDM) halos, focusing on how collisional heat transport and gravothermal evolution regulate the central inflow. The black hole is modeled as a growing central point mass, and its accretion rate evolves self-consistently with the inner halo structure. Varying the SIDM halo parameters, we identify distinct accretion regimes set by the competition between dynamical inflow and conductive heat transport. In regimes where inflow outpaces conduction, the black hole can grow rapidly, accreting a substantial mass on a short timescale. These results provide a framework for assessing when SIDM can substantially alter seed black hole growth and for linking accretion histories to constraints on SIDM models.
| Research Area | Dark Matter: theory |
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