paper

Magnetorotationally-Driven Galactic Turbulence and the Formation of Giant Molecular Clouds

arXiv:astro-ph/0309080 · doi:10.1086/379367

Abstract

Using local 3D MHD simulations, we investigate ways in which galactic turbulence associated with the magnetorotational instability (MRI) may influence the formation and properties of GMCs. Our disk models are vertically stratified and subject to uniform shear. Initial magnetic fields are weak and purely vertical. For simplicity, we adopt an isothermal equation of state. We find that MRI-driven turbulence develops rapidly, with the saturated-state Shakura & Sunyaev parameter alpha~(0.15-0.3) dominated by Maxwell stresses. Many of the dimensionless characteristics of the turbulence (e.g. the ratio of the Maxwell to Reynolds stresses) are similar to results from previous MRI studies of accretion disks, hence insensitive to the degree of vertical disk compression, shear rate, and the presence of self-gravity. The density-weighted velocity dispersions in non- or weakly self-gravitating disks are sigma_x ~ sigma_y ~ (0.4-0.6)c_s and sigma_z~(0.2-0.3)c_s, suggesting that MRI can contribute significantly to the observed level of galactic turbulence. The saturated-state magnetic field strength B ~ 2 μG is similar to typical galactic values. When self-gravity is strong enough, MRI-driven high-amplitude density perturbations are swing-amplified to form Jeans-mass (~10^7 Msun) bound clouds. Compared to previous unmagnetized or strongly-magnetized disk models, the threshold for nonlinear instability in the present models occurs for surface densities at least 50% lower, corresponding to the Toomre parameter Q_th~1.6. We present evidence that self-gravitating clouds like GMCs formed under conditions similar to our models can lose much of their original spin angular momenta by magnetic braking, preferentially via fields threading near-perpendicularly to their spin axes.

39 pages, 8 figures, to appear in ApJ, vol. 599, Dec. 20, 2003; For better postscript figures and mpeg animations, see http://cfa-www.harvard.edu/~wkim/FIGURE4/

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