Dynamos in Disks and Disk Coronae: The Role of the Magnetorotational Instability

Details Dynamos in Disks and Disk Coronae: The Role of the Magnetorotational Instability Dynamos in Disks and Disk Coronae: The Role of the Magnetorotational Instability

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...204.6222v&link_type=abstract

American Astronomical Society Meeting 204, #62.22; Bulletin of the American Astronomical Society, Vol. 36, p.776

Astronomy and Astrophysics

Astronomy

Scientific paper

The generation of strong large scale magnetic field depends on the generation of a magnetic helicity current by eddy scale turbulence. We give a quasilinear estimate of the magnetic helicity current driven by the magnetorotational instability in an accretion disk. We compare the fluid and kinetic limits of this process and show that in both cases a dynamo is expected. This implies that accretion disk coronae and advective accretion solutions can generate large scale magnetic fields, and release gravitational energy through the magnetorotational instability.

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