Physics
Scientific paper
Jan 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...95..119t&link_type=abstract
Solar Physics (ISSN 0038-0938), vol. 95, Jan. 1985, p. 119-140. NSF-NASA-supported research.
Physics
10
Compressibility Effects, Cosmic Plasma, Magnetohydrodynamic Flow, Solar Activity, Solar Magnetic Field, Viscous Flow, Eigenvectors, Force-Free Magnetic Fields, Solar Flares, Solar Prominences, Tearing Modes (Plasmas)
Scientific paper
Filaments and flares are prominent indicators of the magnetic fields of solar activity. These instability phenomena arise from the influence of weak transport effects (radiation and resistivity, respectively) on coronal magnetodynamics and energy flow. It has been shown that the filament and flare (tearing or reconnection) mechanisms are resistively coupled in sheared magnetic fields of the kind existing in active regions. The present paper expands this treatment to include the effects of compressibility and viscosity, which are most prominent at short wavelengths. The results show that compressibility affects the radiative mode, including a modest increase of its growth rate, and that viscosity modifies the tearing mode, partially through a decrease of its growth rate. A comprehensive discussion of the mode structures and flows is presented. The strongest effect found is a reversal, at very long wavelengths, of the radiative cooling of the resistive interior layer of the tearing mode, caused by compressional heating.
Steinolfson Richard S.
Tachi Tomohiro
van Hoven Gerard
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