Tidal disruption process for a Newtonian star and non-spinning black hole

In this study, we analyze the tidal process which disrupts a Newtonian star on a parabolic orbit about a non-spinning black hole and places the debris on bound and unbound trajectories. We implement a three dimensional hydrodynamics and self-gravity code which also calculates the relativistic tidal interaction in a local moving frame centered on a star. We characterize the mass tidally stripped from the star and estimate the orbital parameters of the debris by local to black hole frame transformations. We discuss the bound and unbound ``kicks'' to the star off of its initial orbit in weak and partially disruptive encounters. We show super-Eddington return rates of debris which closely follow the canonical $t^{-5/3}$ fall-off. We also show results of encounters very close to the black hole ($\alt 10M$) and discuss the relativistic effects early in the return rate.