Gravitational Collapse in Turbulent Molecular Clouds. II. Magnetohydrodynamical Turbulence

Details Gravitational Collapse in Turbulent Molecular Clouds. II. Magnetohydrodynamical Turbulence Gravitational Collapse in Turbulent Molecular Clouds. II. Magnetohydrodynamical Turbulence

2000-09-14

arxiv.org/abs/astro-ph/0009227v1

Astrophys.J.547:280-291,2001

Astronomy and Astrophysics

Astrophysics

32 pages, 14 figures, accepted by ApJ

Scientific paper

10.1086/318335

Hydrodynamic supersonic turbulence can only prevent local gravitational collapse if the turbulence is driven on scales smaller than the local Jeans lengths in the densest regions, a very severe requirement (Paper I). Magnetic fields have been suggested to support molecular clouds either magnetostatically or via magnetohydrodynamic (MHD) waves. Whereas the first mechanism would form sheet-like clouds, the second mechanism not only could exert a pressure onto the gas counteracting the gravitational forces, but could lead to a transfer of turbulent kinetic energy down to smaller spatial scales via MHD wave interactions. This turbulent magnetic cascade might provide sufficient energy at small scales to halt local collapse. We test this hypothesis with MHD simulations at resolutions up to 256^3 zones, done with ZEUS-3D. We first derive a resolution criterion for self-gravitating, magnetized gas: in order to prevent collapse of magnetostatically supported regions due to numerical diffusion, the minimum Jeans length must be resolved by four zones. Resolution of MHD waves increases this requirement to roughly six zones. We then find that magnetic fields cannot prevent local collapse unless they provide magnetostatic support. Weaker magnetic fields do somewhat delay collapse and cause it to occur more uniformly across the supported region in comparison to the hydrodynamical case. However, they still cannot prevent local collapse for much longer than a global free-fall time.

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