Analysis of mass and energy flows in coronal loops using the Bifrost stellar atmosphere code
Abstract
Identifying and quantifying processes that lead to the regulation of the mass and energy supply from the chromosphere to the outer layers of the solar atmosphere is key to advancing our understanding of the coupling between the solar chromosphere and corona. The combination of large-scale numerical simulations of the rapidly evolving detailed physical processes occurring in the solar atmosphere and high-resolution observations from instruments like IRIS, Hinode and SDO makes this undertaking more and more feasible. Using the Bifrost stellar atmosphere code, we have performed 3D radiation MHD simulations of the solar atmosphere extending from the convection zone to the corona to study the evolution of magnetic field structures and the underlying dynamics. By adding tracer particles to the simulation, we are able to follow the magnetic field lines properly. A detailed analysis of the plasma properties along those field lines and of the generation and propagation of waves travelling into the corona will be presented. By tracking the evolution of the observed perturbations, we provide new insights on the physical processes driving them and on their role in the chromosphere-corona mass cycle.
- Publication:
-
40th COSPAR Scientific Assembly
- Pub Date:
- 2014
- Bibcode:
- 2014cosp...40E3750Z