Stochastic perpendicular ion heating in Hall MHD

Abstract:

The mechanism of solar corona heating is a fundamental problem in heliosphere. One of the proposed models is based on the low-frequency Alfven waves(Omega << Omega_i). In the low-beta corona where a strong magnetic field domains, MHD studies show that Alfven waves turbulence primarily cascades to smaller scale perpendicular to the mean magnetic fields rather than the parallel direction. In our previous test-particle simulation, the inertial range MHD turbulence shows the existence of stochastic ion heating. However, most wave-particle interactions would be located near, or smaller than the transition region between the inertial scales and dissipation scales. Our Hall MHD simulation can provide this interesting background field including both Alfven wave and Kinetic Alfven wave. The new test particle simulation will provide more accurate stochastic heating rate. It will also reveal the difference of turbulence at different scales.