MHD Shock Heating in Solar Corona Holes

Summary form only given. We report on a one dimensional simulation of plane polarized, large amplitude, Alfven waves traveling upwards through a gravitationally stratified solar corona hole. In the low plasma beta region the waves develop into fast magnetic shocks that reach great heights with little heat dissipation, where they excite large amplitude slow hydrodynamic shocks that deposit sufficient energy to be a possible important mechanism of heating the corona. We also report on progress in doing a three dimensional simulation of the same problem using the FCTMHD3D code.