1998/09/28 by James M. Stone, Eve C. Ostriker, Charles F. Gammie · 10 citations
Physics and Astronomy · #Astrophysics #Astrophysics and Star Formation Studies #Atomic and Molecular Physics #Classical mechanics #Compressibility #Dissipation #Dynamo #K-epsilon turbulence model #K-omega turbulence model #Magnetic field #Magnetohydrodynamic drive #Magnetohydrodynamic turbulence #Magnetohydrodynamics #Mechanics #Physics #Stellar, planetary, and galactic studies #Supersonic speed #Thermodynamics #Turbulence #astro-ph
paper · pdf · doi:10.1086/311718
published as Astrophys.J. 508 (1998) L99-L102 · 5 pages, 3 Postscript figures, LaTeX, accepted by Ap.J.Lett
arxiv created 1998/09/28 · openalex publication_date 1998/11/20 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
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 the order of the flow crossing time or smaller, even in the presence of strong magnetic fields. About half of the dissipation occurs in shocks. Weak magnetic fields are amplified and tangled by the turbulence, while strong fields remain well ordered.