Magnetic Helicity, Dynamo Action, Reconnection, and Particle Acceleration

Details Magnetic Helicity, Dynamo Action, Reconnection, and Particle Acceleration Magnetic Helicity, Dynamo Action, Reconnection, and Particle Acceleration

May 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000iaus..195..389f&link_type=abstract

Highly Energetic Physical Processes and Mechanisms for Emission from Astrophysical Plasmas, Proceedings of IAU Symposium #195, h

Astronomy and Astrophysics

Astrophysics

Scientific paper

Blackman & Field have shown that a working "alpha-omega" dynamo requires finite but opposite flows of small- and large-scale magnetic helicity through a body's surface. The helicity is accompanied by magnetic energy available for dissipation. The observed solar coronal nonthermal power is consistent with the derived lower limit required. This link between dynamo field generation and nonthermal emission should generally apply to stars, spiral galaxies, and accretion disks.

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