Segregation of Stellar-Mass Black Holes at the Galactic Center

Razieh Emami, Abraham Loeb

Published 2019-03-06Version 1

We simulate the star cluster near the center of the Milky Way galaxy. Using the Fokker Planck approach we consider the time evolution of the density profile of stars and stellar mass black holes (BHs) for various initial profiles. BHs sink toward the center of the galaxy where they are swallowed by SgrA*. We show that the mass loss increases the mass of SgrA* by up to 20 % for shallow initial radial profile with a power-law slope $\gamma = 0.8$, and BH mass of $40 M_{\odot}$. We model the consumption rate analytically and compare it with the results from simulation. Stars make the main contribution in increasing the mass of SgrA*.