The gravitational collapse of the dust toward the newly formed rotating black holes in Kerr and 4-D Einstein–Gauss–Bonnet Gravities

Studying the gravitational collapse of dust particles toward newly formed black holes has gained popularity following the observation of gravitational waves resulting from black hole mergers . In this paper, we focus on modeling the descent of dust debris toward a black hole using a numerical code that incorporates relativistic hydrodynamics within the framework of General Relativity and Einstein–Gauss–Bonnet gravity. We explore the influence of various parameters, such as the black hole’s rotation parameter a and the EGB coupling constant α , on the curvature effects observed. Both parameters significantly impact the dynamics of the accretion disk formed around the black holes. Furthermore, we discuss the gravitational collapse process in two distinct scenarios. It is also observed that the mass accretion rate is significantly influenced by these two parameters. The rate at which mass is accreted onto a black hole directly impacts the black hole’s growth and evolutionary trajectory.