Radiative hydrodynamical simulations of super-Eddington accretion flow in tidal disruption event: the accretion flow and wind

One key question in tidal disruption events theory is that how much of the fallback debris can be accreted to the black hole. Based on radiative hydrodynamic simulations, we study this issue for efficiently `circularized’ debris accretion flow. We find that for a black hole disrupting a solar type star, $15\mathrm{\%}$ of the debris can be accreted for a ${10}^7$ solar mass ($M_{\odot }$) black hole. While for a ${10}^6{M}_{\odot }$ black hole, the value is $43\mathrm{\%}$. We find that wind can be launched in the super-Eddington accretion phase regardless of the black hole mass. The maximum velocity of wind can reach $0.7c$ (with $c$ being speed of light). The kinetic power of wind is well above ${10}^{44}\mathrm{e}\mathrm{r}\mathrm{g}{\mathrm{s}}^{-1}$. The results can be used to study the interaction of wind and the circumnuclear medium around quiescent super-massive black holes.