An Incoherent alpha -Omega Dynamo Mechanism for Accretion Disks

Details An Incoherent alpha -Omega Dynamo Mechanism for Accretion Disks An Incoherent alpha -Omega Dynamo Mechanism for Accretion Disks

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...18710409v&link_type=abstract

American Astronomical Society, 187th AAS Meeting, #104.09; Bulletin of the American Astronomical Society, Vol. 27, p.1435

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We use the mean-field dynamo equations to show that an incoherent alpha effect in mirror-symmetric turbulence in a shearing flow can generate a large scale, coherent magnetic field. In other words, a shearing environment can create an organized magnetic field even if the time averaged helicity is zero. We illustrate this effect with simulations of a few simple systems. In accretion disks, this process can lead to axisymmetric magnetic domains whose radial and vertical dimensions will be comparable to the disk height. This process may be responsible for observations of dynamo activity seen in simulations of dynamo-generated turbulence involving, for example, the Balbus-Hawley instability. In this case the magnetic field strength will saturate at ~ (h/r)(2) times the ambient pressure in real accretion disks. The resultant dimensionless viscosity will be of the same order. In numerical simulations the azimuthal extent of the simulated annulus should be substituted for r. We compare the predictions of this model to numerical simulations previously reported by Brandenburg et al. (1995). In a radiation pressure dominated environment this estimate for viscosity should be reduced by a factor of (Pgas/Pradiation)(6) due to magnetic buoyancy.

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