  A wide variety of astrophysical phenomena involve the flow of turbulent
magnetized gas with relativistic velocity or energy density. Examples include
gamma-ray bursts, active galactic nuclei, pulsars, magnetars, micro-quasars,
merging neutron stars, X-ray binaries, some supernovae, and the early universe.
In order to elucidate the basic properties of the relativistic
magnetohydrodynamical (RMHD) turbulence present in these systems, we present
results from numerical simulations of fully developed driven turbulence in a
relativistically warm, weakly magnetized and mildly compressible ideal fluid.
We have evolved the RMHD equations for many dynamical times on a uniform grid
with 1024^3 zones using a high order Godunov code. We observe the growth of
magnetic energy from a seed field through saturation at about 1% of the total
fluid energy. We compute the power spectrum of velocity and density-weighted
velocity and conclude that the inertial scaling is consistent with a slope of
-5/3. We compute the longitudinal and transverse velocity structure functions
of order p up to 11, and discuss their possible deviation from the expected
scaling for non-relativistic media. We also compute the scale-dependent
distortion of coherent velocity structures with respect to the local magnetic
field, finding a weaker scale dependence than is expected for incompressible
non-relativistic flows with a strong mean field.
