Turbulence in Accretion Disks
An accretion disk is an inevitable part of the star forming process. Recent years have witnessed dramatic progress in our understanding of how turbulence arises and transports angular momentum in astrophysical accretion disks. The key conceptual point is that the combination of a subthermal magnetic field and outwardly decreasing differential rotation is subject to the magnetorotational instability. This rapidly generates magnetohydrodynamical (MHD) turbulence, leading to greatly enhanced angular momentum transport. Purely hydrodynamic disks, on the other hand, are stable. Disks that are too cool to couple effectively to the magnetic field will not be turbulent. Fully global three dimensional MHD simulations are now beginning to probe the properties of accretion disks from first principles.
KeywordsInstabilities MHD protostellar disks
Unable to display preview. Download preview PDF.
- Blaes, O.M. and Balbus, S.A.: 1994 ApJ 421 163.Google Scholar
- Brandenburg, A., Norlund, Â., Stein, R.F. and Torkelsson, U.: 1995, Api 446, 741.Google Scholar
- De Villiers, J.-P. and Hawley, J.F.: 2003, Api 592, 1060.Google Scholar
- Glassgold, A.E., Feigelson, E.D. and Montmerle, T.: 2000, in: V. Mannings, A.P. Boss and S.S. Russell (eds.), Protostars and Planets IV, Univ. Arizona, Tucson, 429.Google Scholar
- Nelson, R. and Papaloizou, J.C.B.: 2002a, MNRAS 339, 983.Google Scholar
- Shakura, N.I. and Sunyaev, R.A.: 1973, AandA 24, 337.Google Scholar
- Stone, J.M. and Fleming, T.: 2003, Api 585, 908.Google Scholar
- Stone, J. M., Gammie, C. F., Balbus, S. A. and Hawley, J.F.: 2000Google Scholar
- Transport Processes in Protostellar Disks, in: V. Manning, A. Boss and S. Russell (eds.), Protostars and Planets IV,Tuscon, Univ. Arizona Press, 589.Google Scholar
- Zahn, J.-P.: 1991, in: C. Bertout et al. (eds.), Structure and Emission Properties of Accretion Disks, Editions Frontières, Gif-sur-Yvette, 87.Google Scholar