Dissipating waves in a hot, compressible, magnetic, structured atmosphere

Details Dissipating waves in a hot, compressible, magnetic, structured atmosphere Dissipating waves in a hot, compressible, magnetic, structured atmosphere

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995soph..157..103l&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 157, no. 1-2, p. 103-119

Physics

8

Dissipation, Magnetohydrodynamic Waves, Magnetohydrodynamics, Solar Atmosphere, Solar Physics, Sun, Conductive Heat Transfer, Coronal Loops, Damping, Ducted Flow, Solar Magnetic Field, Viscosity

Scientific paper

The damping of ducted, fast, magnetohydrpodynamic (MHD) waves by ion viscosity and electron heat conduction in a radiating, optically thin, warm, structured atmosphere has been evaluated. Dissipation is more effective in a warm plasma than in a 'cold' one but, for waves ducted by solar coronal loops, dissipation is only efficient if the periods of the waves are shorter than a few tens of seconds and only if the background magnetic field is less than about 15 G. It appears that MHD waves of longer periods and in stronger magnetic fields will survive the dissipative mechanisms considered here and may be manifest as observable coronal oscillations.

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