Heating of the solar corona by the resonant absorption of Alfven waves

Details Heating of the solar corona by the resonant absorption of Alfven waves Heating of the solar corona by the resonant absorption of Alfven waves

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...317..514d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 317, June 1, 1987, p. 514-521. NASA-supported research.

Statistics

Computation

185

Energy Dissipation, Magnetohydrodynamic Waves, Plasma Heating, Plasma Resonance, Solar Corona, Absorption, Computational Astrophysics, Coronal Loops, Fourier Transformation, Late Stars, Plasma Dynamics

Scientific paper

An improved method for calculating the resonance absorption heating rate is discussed and the results are compared with observations in the solar corona. To accomplish this, the wave equation for a dissipative, compressible plasma is derived from the linearized magnetohydrodynamic equations for a plasma with transverse Alfven speed gradients. For parameters representative of the solar corona, it is found that a two-scale description of the wave motion is appropriate. The large-scale motion, which can be approximated as nearly ideal, has a scale which is on the order of the width of the loop. The small-scale wave, however, has a transverse scale much smaller than the width of the loop, with a width of about 0.3-250 km, and is highly dissipative. These two wave motions are coupled in a narrow resonance region in the loop where the global wave frequency equals the local Alfven wave frequency. Formally, this coupling comes about from using the method of matched asymptotic expansions to match the inner and outer (small and large scale) solutions. The resultant heating rate can be calculated from either of these solutions. A formula derived using the outer (ideal) solution is presented, and shown to be consistent with observations of heating and line broadening in the solar corona.

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