  We study the statistics of density for supersonic turbulence in a medium with
magnetic pressure larger than the gaseous pressure. This study is motivated by
molecular cloud research. Our simulations exhibit clumpy density structures,
which contrast increases with the Mach number. At 10 Machs densities of some
clumps are three orders of magnitude higher than the mean density. These clumps
give rise to flat and approximately isotropic density spectrum corresponding to
the random distribution of clumps in space. We claim that the clumps originate
from our random, isotropic turbulence driving. When the contribution from those
clumps is suppressed by studying logarithm of density, the density statistics
exhibit scale-dependent anisotropy consistent with the models where density
structures arise from shearing by Alfv\'en waves. It is noteworthy that
originally such models were advocated for the case of low-Mach, nearly
incompressible turbulence.
