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Alfven-wave dissipation: A support mechanism for quiescent prominencesHigh resolution filtergrams or spectrograms of the main body of quiescent prominences often show a very vivid dynamical picture that cannot be reconciled with static models. Even if large differences exist between individual prominences in this respect, at least parts of the prominence are usually found to be in a 'choppy', turbulent state. Evidence for systematic flows are found in local regions in the prominence and also in the transition zone in the surroundings. These two regions are probably decoupled magnetically. Alfven waves are generally believed to be responsible for the heating in the upper chromosphere and corona (Hollweg 1986). Since evidence for the presence of Alfven-waves has also been found in the solar wind field, it is highly probable that such waves are generated in the convection zone of the sun and propagated outwards in the solar atmosphere wherever a proper magnetic field is present to carry the waves. The most basic magnetic formations in the solar atmosphere are simple loops. They occur all over the solar surface and cover a large range of magnetic field strengths. Loops with the strongest magnetic fields are found in active regions. It is to be expected that the Alfven-wave flux which is channelled into the loops from below, could show considerable variation both with heliocentric latitude, with time and locally between neighbouring loops. What happens when a magnetic loop is exposed to the appropriate Alfven-wave flux required to heat the upper solar atmosphere is examined.
Document ID
19870011448
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Jensen, Eberhart (Oslo Univ.)
Date Acquired
September 5, 2013
Publication Date
December 1, 1986
Publication Information
Publication: NASA. Goddard Space Flight Center Coronal and Prominence Plasmas
Subject Category
Solar Physics
Accession Number
87N20881
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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