Physics
Scientific paper
Dec 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...89..275j&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 89, Dec. 1983, p. 275-285.
Physics
10
Magnetohydrodynamic Waves, Plasma Turbulence, Solar Physics, Solar Prominences, Astronomical Models, Field Strength, Flow Velocity, Solar Magnetic Field, Wave Attenuation
Scientific paper
In the dynamical model of quiescent prominences presented in this paper, it is assumed that the ever-changing velocity field and brightness of the fine structure is due to MHD turbulence driven by an Alfven-wave flux from below. It is shown that these waves become highly nonlinear and are dissipated over relatively short scales in prominence matter. For magnetic field strengths lower than those observed in quiescent prominences, no closed arch structure can exist with the physical parameters observed. For higher field strengths the conditions for the creation of turbulence are not fulfilled. The momentum gained by prominence matter in the dissipation process, is shown to be of the right order of magnitude to provide the supporting force against gravity. 'Edge' effects find a simple explanation within the framework of this hypothesis. In the upper regions of a prominence one result of the dissipation may be the formation of open magnetic configurations, in keeping with the presence of streamers connected with quiescent prominences. Observational tests are proposed and discussed.
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