Solar-like convective and coronal layers in a single numerical model
Abstract
We investigate the coupling between turbulent magnetoconvection and an atmospheric layer on the sun using numerical simulations of compressible fluids. The model consists of a stratified MHD fluid spanning multiple scale heights, encompassing the transition of the plasma beta from high to low values. Although a heat flux is imposed at the lower boundary, only the lower portion of the domain where the beta is high is convectively unstable. The upper portions are stabilized by a parameterized heating function and the presence of a strong magnetic field and, similar to the solar chromosphere and corona. As a result, the dynamics associated with evolving magnetic features in the solar atmosphere can be modeled in a manner that is self-consistent with the convective motions that provide the driving. We present simulations of arcade-like reconnection in the presence of supergranular-scale flows and discuss possible observational consequences.
- Publication:
-
35th COSPAR Scientific Assembly
- Pub Date:
- 2004
- Bibcode:
- 2004cosp...35.3551H