The Magnetic Helicity Current in an Alpha-Omega Dynamo

Details The Magnetic Helicity Current in an Alpha-Omega Dynamo The Magnetic Helicity Current in an Alpha-Omega Dynamo

Jun 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005mpge.conf..177v&link_type=abstract

The Magnetized Plasma in Galaxy Evolution, Proceedings of the conference held in Kraków, Poland, Sept. 27th - Oct. 1st, 2004, Ed

Physics

Scientific paper

Conservation of magnetic helicity plays a critical role in suppressing mean-field dynamo action. Successful large scale dynamo action can occur if, and only if, the local turbulence is biased to drive a magnetic helicity current. In the case of a disk dynamo, the required magnetic helicity current is vertical and imposes a connection between the corona and the dynamo. The sign of the magnetic helicity current determines whether we get a dynamo or an anti-dynamo. The latter is more likely in systems in which angular momentum is driven outward by local turbulence. A successful galactic dynamo in an L* spiral disk will magnetize the surrounding intergalactic medium within several hundred kpc to ˜ 10-9 Gauss.

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