Local magnetohydrodynamic instabilities and the wave-driven dynamo in accretion disks

Details Local magnetohydrodynamic instabilities and the wave-driven dynamo in accretion disks Local magnetohydrodynamic instabilities and the wave-driven dynamo in accretion disks

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...398..561v&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 398, no. 2, p. 561-568.

Statistics

Computation

46

Accretion Disks, Dynamo Theory, Magnetohydrodynamic Stability, Stellar Physics, Buoyancy, Computational Astrophysics, Interstellar Magnetic Fields, Magnetohydrodynamic Turbulence, Propagation Modes, Viscosity

Scientific paper

We consider the consequences of magnetic buoyancy and the magnetic shearing instability (MSI) on the strength and organization of the magnetic field in a thin accretion disk. We discuss a model in which the wave-driven dynamo growth rate is balanced by the dissipative effects of the MSI. As in earlier work, the net helicity is due to small advective motions driven by nonlinear interactions between internal waves. Assuming a simple model of the internal wave spectrum generated from the primary m = 1 internal waves, we find that the magnetic energy density saturates at about (H/r) exp 4/3 times the local pressure (where H is the disk thickness and r is its radius). On very small scales the shearing instability will produce an isotropic fluctuating field. For a stationary disk this is equivalent to a dimensionless 'viscosity' of about (H/r) exp 4/3. The vertical and radial diffusion coefficients will be comparable to each other. Magnetic buoyancy will be largely suppressed by the turbulence due to the MSI. We present a rough estimate of its effects and find that it removes magnetic flux from the disk at a rate comparable to that caused by turbulent diffusion.

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