  Supersonic turbulence generates distributions of shock waves. Here, we
analyse the shock waves in three-dimensional numerical simulations of uniformly
driven supersonic turbulence, with and without magnetohydrodynamics and
self-gravity. We can identify the nature of the turbulence by measuring the
distribution of the shock strengths.
  We find that uniformly driven turbulence possesses a power law distribution
of fast shocks with the number of shocks inversely proportional to the square
root of the shock jump speed. A tail of high speed shocks steeper than Gaussian
results from the random superposition of driving waves which decay rapidly. The
energy is dissipated by a small range of fast shocks. These results contrast
with the exponential distribution and slow shock dissipation associated with
decaying turbulence.
  A strong magnetic field enhances the shock number transverse to the field
direction at the expense of parallel shocks. A simulation with self-gravity
demonstrates the development of a number of highly dissipative accretion
shocks. Finally, we examine the dynamics to demonstrate how the power-law
behaviour arises.
