Student Posters Repository

The Galactic Centre (GC) is a unique place to study the extreme dynamical processes occurring near a massive black hole (MBH). In this work I study the role of supernova (SN) explosions occurring in massive binary stellar systems lying in a discy structure within the innermost pc. In this poster I show the results of a suite of regularized 3-body simulations of binaries orbiting the central MBH, while the primary star undergoes a SN explosion. The simulations are evolved by means of a fully regularized N-body code that implements the Mikkola’s algorithmic regularization. This code is designed for studying the dynamical evolution of few-body systems in which strong gravitational encounters are frequent and the mass ratio between the interacting objects is large. This scheme removes the singularity of the two-body gravitational potential and allows extremely high integration accuracy. In my study, SN kicks scatter the lighter stars in the pair on completely new orbits, with higher eccentricity and inclination. In contrast, stellar black holes (BHs) and massive stars retain memory of the orbit of their progenitor star. My results suggest that SN kicks are not sufficient to eject BHs from the GC: all BHs that form in situ in the central parsec of our Galaxy probably remain in the GC.