MHD Simulations of Chromospheric Dynamics Using a Complete Electrical Conductivity Tensor

Details MHD Simulations of Chromospheric Dynamics Using a Complete Electrical Conductivity Tensor MHD Simulations of Chromospheric Dynamics Using a Complete Electrical Conductivity Tensor

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0204k&link_type=abstract

American Astronomical Society, SPD meeting #37, #2.04; Bulletin of the American Astronomical Society, Vol. 38, p.221

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A 1.5 D MHD simulation that includes an energy equation and a complete space and timedependent electrical conductivity tensor valid for a variably ionized plasma is used tostudy Alfven, magnetoacoustic, and acoustic wave propagation in the chromosphere. Heatingrates due to dissipation of magnetic field aligned and Pedersen currents are computed andcompared with FAL values. The model includes a numerical method that reduces the numerical dissipationrate far below the physical dissipation rate determined by the conductivity tensor. Wavelengths of 80 - 220 km, and a spatial resolution of 10 km are used. The background state is the FAL equilibriumstate with a constant vertical magnetic field. For magnetic waves, the initial energy is converted intothermal energy, bulk flow kinetic energy, and a Poynting flux of energy with a non-zero divergence.It is verified that Poynting's theorem is satisfied. The waves are launched 10^3 km above the FAL photosphere. The magnetic waves are rapidly damped outnear this height, and produce heating rates close to the corresponding FAL value. It is the strong magnetization and weak ionization of the chromospherethat allows for the strong wave heating. This heating is duealmost entirely to Pedersen current dissipation.This distinguishes the chromospherefrom the weakly magnetized and weakly ionized photosphere, and the strongly magnetized and stronglyionized corona where Pedersen current dissipation is not a significant heating mechanism on the lengthand time scales simulated.

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