Investigation of Solar Coronal Heating Using a Time Dependent MHD Model with Full Conductivity Tensor

Details Investigation of Solar Coronal Heating Using a Time Dependent MHD Model with Full Conductivity Tensor Investigation of Solar Coronal Heating Using a Time Dependent MHD Model with Full Conductivity Tensor

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp41a..07k&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SP41A-07

Astronomy and Astrophysics

Astrophysics

7500 Solar Physics, Astrophysics, And Astronomy, 7507 Chromosphere, 7509 Corona, 7546 Transition Region

Scientific paper

The transition region and lower corona is investigated using a newly developed time dependent MHD model that includes gravity and a self consistently computed conductivity tensor that depends on temperature, magnetic field, and density. The model is tested by its ability to preserve FAL equilibrium profiles, and to generate MHD waves with dispersion relations similar to those predicted by linear theory for the general types of MHD waves. The model is then used to examine solar atmospheric heating by Pedersen and magnetic field aligned current dissipation. Numerical experiments are conducted in which MHD waves are launched from either the transition region upward, or from the lower corona downward. Results from parametric studies of the evolution of these waves as a function of wavelength and amplitude are presented. In particular, the heating rate due to wave dissipation is compared with the FAL cooling rate, and with analytic results presented in M. Goodman [1,2]. % . The relative importance of physical dissipation due to the conductivity tensor, and numerical dissipation is estimated using Von Neumann stability analysis (VNSA) and numerical experiments with and without physical dissipation. It is then attempted to extrapolate from the simulation data the waves which could potentially lead to the correct heating rate, assumed to be the FAL net radiative loss rate. Realistic solar atmospheric data is used throughout the numerical investigations. This work was supported in part by NSF grant ATM-0242820 to the Institute for Scientific Research.

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