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Magnetic fields in the sunThe observed properties of solar magnetic fields are reviewed, with particular reference to the complexities imposed on the field by motions of the highly conducting gas. Turbulent interactions between gas and field lead to heating or cooling of the gas according to whether the field energy density is less or greater than the maximum kinetic energy density in the convection zone. The field strength above which cooling sets in is 700 gauss. A weak solar dipole field may be primeval, but dynamo action is also important in generating new flux. The dynamo is probably not confined to the convection zone, but extends throughout most of the volume of the sun. Planetary tides appear to play a role in driving the dynamo.
Document ID
19740015242
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Mullan, D. J. (Franklin Inst. Swarthmore, PA, United States)
Date Acquired
September 3, 2013
Publication Date
January 1, 1974
Subject Category
Space Radiation
Report/Patent Number
NASA-CR-138189
Meeting Information
Meeting: Ann. Symp. of BRF (expanded version)
Location: Swarthmore, PA
Country: United States
Start Date: May 10, 1974
End Date: May 11, 1974
Accession Number
74N23355
Funding Number(s)
CONTRACT_GRANT: NGR-39-005-066
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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