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The distribution of orbital energies imparted into stellar debris followingthe close encounter of a star with a supermassive black hole is the principalfactor in determining the rate of return of debris to the black hole, and thusin determining the properties of the resulting lightcurves from such events. Wepresent simulations of tidal disruption events for a range of $\beta\equivr_{\rm t}/r_{\rm p}$ where $r_{\rm p}$ is the pericentre distance and $r_{\rmt}$ the tidal radius. We perform these simulations at different spatialresolutions to determine the numerical convergence of our models. We comparesimulations in which the heating due to shocks is included or excluded from thedynamics. For $\beta \lesssim 8$ the simulation results are well-converged atsufficiently moderate-to-high spatial resolution, while for $\beta \gtrsim 8$the breadth of the energy distribution can be grossly exaggerated byinsufficient spatial resolution. We find that shock heating plays anon-negligible role only for $\beta \gtrsim 4$, and that typically the effectof shock heating is mild. We show that self-gravity can modify the energydistribution over time after the debris has receded to large distances for all$\beta$. Primarily, our results show that across a range of impact parameters,while the shape of the energy distribution varies with $\beta$, the width ofthe energy spread imparted to the bulk of the debris is closely matched to thecanonical spread, $\Delta E = GM_\bullet R_\star/r_{\rm t}^2$, for the range of$\beta$ we have simulated.

Stars Crushed by Black Holes. I. On the Energy Distribution of Stellar Debris in Tidal Disruption Events