3D MHD Modeling of Prominence Formation and Eruption
Abstract
The formation of prominences in the solar corona is widely thought to be caused by plasma evaporation and condensation via thermal non-equilibrium. This process has been previously modeled by one-dimensional hydrodynamic simulations along individual field lines within static magnetic fields. A more realistic modeling of prominence formation can be achieved through the use of three-dimensional thermodynamic MHD simulations with time-dependent magnetic fields, which has only become feasible within the last few years. In this talk I will describe recent three-dimensional simulations that display the formation and eruption of prominence-like structures. The capabilities and limitations of these simulations will be discussed, along with the next steps that lie ahead.
- Publication:
-
42nd COSPAR Scientific Assembly
- Pub Date:
- July 2018
- Bibcode:
- 2018cosp...42E3414T