I am a postdoctoral researcher studying how black hole feeding and AGN mechanical and radiative feedback shape the galaxy and black hole co-evolution. Right now, I am exploring how simplified black hole accretion models adopted in cosmological simulations capture the interplay between feeding and feedback, by using 2D hydrodynamical simulations.


The figure above shows the temporal evolution of the black hole mass, accretion rate, stellar mass and star formation rate for a typical simulation. The hot halo cools producing a cold, infalling shell that quickly fragments due to the Rayleigh–Taylor instability, producing a multiphase ISM characterized by a hot, diffuse component plus clumpy cold gas. When the cold clumps reach the galaxy center, they are accreted on the black hole, triggering AGN feedback, that ionizes and evacuates the black hole surroundings, producing hot bubbles and suppressing star formation. Eventually, the external cold clumps are able to penetrate the hot bubble, producing another accretion event. This accretion-feedback cycle produces a highly fluctuating black hole accretion rate and star formation rate time evolution.  A movie of this simulations is available here [https://youtu.be/zMP8vi8kCl0]