Speaker
Description
If a star travels close enough to a massive compact object can cause its disruption due to strong tidal forces overcoming the stellar self-gravity. This scenario results into a bright, characteristic electromagnetic signature known as a tidal disruption event (TDE). The numerical modelling of such phenomena is extremely challenging due to the extreme conditions that the star is subject to, e.g. strong tidal stretching and compression, as well as shocks, all in the vicinity of a massive black hole. In this work, we present our efforts for developing a module for the code SPHINCS that allows performing global hydrodynamic simulations of stellar disruptions in a Kerr spacetime. The code simulates the fluid under the General Relativistic Smoothed-Particle Hydrodynamics approach. We will present the implementation, validation tests, and first applications.