  Shock waves play an important role in turbulent astrophysical media by
compressing the gas and dissipating the turbulent energy into the thermal
energy. We here study shocks in magnetohydrodynamic turbulence using
high-resolution simulations. Turbulent Mach numbers of
$\mathcal{M}_\text{turb}=0.5-7$ and initial magnetic fields of plasma beta
$\beta_0=0.1 - 10$ are considered, targeting turbulences in interstellar and
intracluster media. Specifically, we present the statistics of fast and slow
shocks, such as the distribution of shock Mach numbers ($M_\text{s}$) and the
energy dissipation at shocks, based on refined methodologies for their
quantifications. While most shocks form with low $M_\text{s}$, strong shocks
follow exponentially decreasing distributions of $M_\text{s}$. More shocks
appear for larger $\mathcal{M}_\text{turb}$ and larger $\beta_0$. Fast shock
populations dominate over slow shocks if $\beta_0\gg1$, but substantial
populations of slow shocks develop in the cases of $\beta\lesssim1$, i.e.,
strong background fields. The shock dissipation of turbulent energy occurs
preferentially at fast shocks with $M_\text{s}\lesssim$ a few to several, and
the dissipation at strong shocks shows exponentially decreasing functions of
$M_\text{s}$. The energy dissipation at shocks, normalized to the energy
injection, $\epsilon_\text{shock}/\epsilon_\text{inj}$, is estimated to be in
the range of $\sim0.1-0.5$, except for the case of
$\mathcal{M}_\text{turb}=0.5$ and $\beta_0=0.1$ where the shock dissipation is
negligible. The fraction decreases with $\mathcal{M}_\text{turb}$; it is close
to $\sim0.4-0.6$ for $\mathcal{M}_\text{turb}=0.5$, while it is $\sim0.1-0.25$
for $\mathcal{M}_\text{turb}=7$. The rest of the turbulent energy is expected
to dissipate through the turbulent cascade.
