  Stars that pass too close to a supermassive black hole are disrupted by the
black hole's tidal gravity and leads to some debris being ejected while the
remainder accretes into the black hole. To better study the physics of this
debris, we use the moving mesh code MANGA to follow the evolution of the star
from its initial encounter to its complete destruction. By varying the impact
parameter ($\beta$) of the star, we studied the energy distribution of the
remaining material and the fallback rate of the material into the black hole as
a function of time. We show that the spread of energy in the debris and peak
luminosity time ($t_{\rm peak}$) are both directly related to the impact
parameter. In particular, we find a $\beta^{1/2}$ scaling for the energy spread
for $\beta=2-10$ and a frozen evolution for $\beta\gtrsim 10$. We discuss
implication of this scaling for the rise time of the light curve and broadness
of the luminosity peak for these lower $\beta$'s. These relationships provide a
possible means of inferring the impact parameters for observed TDEs.
