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Magnetic Helicity, Dynamo Action, Reconnection, and Particle Acceleration
Published online by Cambridge University Press: 25 May 2016
Abstract
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Blackman & Field have shown that a working α-Ω 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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- Part II: Posters
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- Copyright © Astronomical Society of the Pacific 2000
References
Field, G.
1986, in AIP Conf. Proc., 144, Magnetospheric Phenomena in Astrophysics, eds. Epstein, R. & Feldman, W. (New York: AIP), 324.Google Scholar
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