  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, $15\%$ of the debris can be accreted for a $10^7$ solar mass ($M_\odot$)
black hole. While for a $10^6M_\odot$ black hole, the value is $43\%$. 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 $10^{44} {\rm
erg \ s^{-1}}$. The results can be used to study the interaction of wind and
the circumnuclear medium around quiescent super-massive black holes.
