A numerical simulation of the formation of solar prominences.
Abstract
The radiative-resistive MHD equations are numerically solved in two-dimensions for a magnetic field configuration that starts with a vertical current sheet which is line-tied at its base and is in mechanical, but not radiative, equilibrium. The aim of the present study is to determine whether this initial configuration can achieve a prominence-like equilibrium in the presence of magnetic reconnection and tearing in the current-sheet.
- Publication:
-
ESA Special Publication
- Pub Date:
- November 1984
- Bibcode:
- 1984ESASP.220..119M
- Keywords:
-
- Magnetohydrodynamics:Solar Prominences;
- Solar Prominences:Magnetohydrodynamics;
- Solar Prominences:Models;
- Computerized Simulation;
- Magnetic Field Configurations;
- Magnetohydrodynamics;
- Radiative Transfer;
- Solar Prominences;
- Stellar Models;
- Coronal Loops;
- Current Sheets;
- Tearing Modes (Plasmas);
- Solar Physics