  Compressible magnetohydrodynamic (MHD) turbulence is a common feature of
astrophysical systems such as the solar atmosphere and interstellar medium.
Such systems are rife with shock waves that can redistribute and dissipate
energy. For an MHD system, three broad categories of shocks exist (slow, fast
or intermediate) however the occurrence rates of each shock type is not known
for turbulent systems. Here we present a method for detecting and classifying
the full range of MHD shocks applied to the Orszag-Tang vortex. Our results
show that the system is dominated by fast and slow shocks, with far less
frequent intermediate shocks appearing most readily near magnetic reconnection
sites. We present a potential mechanism that could lead to the formation of
intermediate shocks in MHD systems, and study the coherency and abundances of
shocks in compressible MHD turbulence.
