On the compatibility of Alfven wave heating of the chromosphere, transition region and corona

Details On the compatibility of Alfven wave heating of the chromosphere, transition region and corona On the compatibility of Alfven wave heating of the chromosphere, transition region and corona

Oct 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.276.1041c&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 276, Issue 4, pp. 1041-1051.

Astronomy and Astrophysics

Astronomy

12

Sun: Chromosphere, Sun: Corona, Sun: General, Sun: Magnetic Fields

Scientific paper

The heating of the solar atmosphere by Alfven waves has been discussed on the basis of two types of theory: (type I) takes into account dissipation by viscosity and electrical resistance, but neglects the variation of diffusivities and Alfven speed with altitude; (type II) takes into account the variation of Alfven speed with altitude, but neglects dissipation. We present a model based on a combined theory (type III), including Alfven speed, viscous and resistive diffusivities which can vary with altitude, and also allowing for the existence of a horizontal wavenumber and oblique magnetic field. We retain the modelling of the atmosphere by isothermal layers, under a uniform magnetic field. It is shown that, when values of the initial velocity perturbation at the chromosphere, wave period, viscosity and resistivity are consistent with observation, the empirical VAL III-F heating rates (Vernazza, Avrett & Loeser) in the chromosphere and corona can only be attained for propagation in oblique magnetic fields or shorter horizontal wavelengths, or both: the reason is that waveform gradients are better preserved by horizontal propagation than by vertical propagation, and an oblique magnetic field also increases propagation time through a given altitude range.

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