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Coronal heating by stochastic magnetic pumpingRecent observational data cast serious doubt on the widely held view that the Sun's corona is heated by traveling waves (acoustic or magnetohydrodynamic). It is proposed that the energy responsible for heating the corona is derived from the free energy of the coronal magnetic field derived from motion of the 'feet' of magnetic field lines in the photosphere. Stochastic motion of the feet of magnetic field lines leads, on the average, to a linear increase of magnetic free energy with time. This rate of energy input is calculated for a simple model of a single thin flux tube. The model appears to agree well with observational data if the magnetic flux originates in small regions of high magnetic field strength. On combining this energy input with estimates of energy loss by radiation and of energy redistribution by thermal conduction, we obtain scaling laws for density and temperature in terms of length and coronal magnetic field strength.
Document ID
19800019786
Acquisition Source
Legacy CDMS
Document Type
Preprint (Draft being sent to journal)
Authors
Sturrock, P. A. (Stanford Univ. CA, United States)
Uchida, Y. (Tokyo Astronomical Observatory)
Date Acquired
September 4, 2013
Publication Date
June 1, 1980
Subject Category
Solar Physics
Report/Patent Number
SU-SUIPR-809
NASA-CR-163356
Report Number: SU-SUIPR-809
Report Number: NASA-CR-163356
Accession Number
80N28287
Funding Number(s)
CONTRACT_GRANT: N00014-75-C-0673
CONTRACT_GRANT: NGL-05-020-272
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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