Simulating the Chromosphere
(Damien Przybylski, Rajees Uthayasegaram, Robert Cameron)
We have extended the MURaM radiative MHD code to incorporate these physical effects (improving our treatment will be an ongoing effort). We have now began our investigation of the dynamics and structure of the chromosphere using our first simulations.
The solar chromosphere is the layer of the solar atmosphere between the cool photosphere (approximately 6000 degrees K) and the corona where the temperature jumps to 1000000 degrees K. The chrosphere is extremely dynamic, full of jets, spicules, shocks, and explosive events. Our understanding of these dynamic features is hampered by the complexity of the physics: the plasma in the chromosphere is of sufficiently low density that collisions no longer dominate and local thermal equilibrium can not be assumed. Radiation in a number of lines become important for the energetics, as are various types of magneto-acoustic waves and magnetic reconnection. The driving of these events take place in the photosphere, and the events extend into the optically thin Corona through the transition region.