Natal kick models and their impact on binary black hole formation

Compact objects that form via core-collapse supernova explosions of the progenitors are expected to get a spatial velocity at their birth, referred to as natal kick, because of asymmetric mass ejection. For neutron stars, we can reconstruct the distribution of kick magnitudes from observations of proper motions of Galactic pulsars, but for black holes the data are scanty and complex to interpret. In this thesis work, we review the main observational hints for black hole natal kicks and study the main proposed models to describe them. In order to prove the self-consistency of these prescriptions, we present some histograms of the main parameters involved and compare the outcomes of three different distributions, underlying how the natal kick impact on binary black holes evolution still represents an open issue.