Dissipation in Compressible MHD Turbulence
  We report results of a three dimensional, high resolution (up to 512^3) numerical investigation of supersonic compressible magnetohydrodynamic turbulence. We consider both forced and decaying turbulence. The model parameters are appropriate to conditions found in Galactic molecular clouds. We find that the dissipation time of turbulence is of order the flow crossing time or smaller, even in the presence of strong magnetic fields. About half the dissipation occurs in shocks. Weak magnetic fields are amplified and tangled by the turbulence, while strong fields remain well ordered. 
James M. Stone (1), Eve C. Ostriker (1), and Charles F. Gammie (2)   ((1) University of Maryland, (2) Center for Astrophysics)