A model for quiescent solar prominences.
Abstract
A onedimensional model is computed for a quiescent prominence in both magnetohydrostatic equilibrium and thermal equilibrium (under a balance between the thermal condition, radiation, and wave heating). The effects of changing the coronal plasma pressure, the horizontal magnetic field strength, and the inclination of the horizontal magnetic field to the prominence normal are investigated. It is found that an equilibrium state is impossible when either the plasma beta or the magnetic field shear is too high. One feature of this model is that the magnetohydrostatics is coupled to the energetics, giving a fourthorder twopoint boundary value problem, with two symmetric conditions applied at the center of the structure and the coronal temperature and density specified at a fixed outer edge.
 Publication:

The Astrophysical Journal
 Pub Date:
 August 1979
 DOI:
 10.1086/157290
 Bibcode:
 1979ApJ...232..304M
 Keywords:

 Magnetic Effects;
 Magnetohydrostatics;
 Solar Prominences;
 Stellar Models;
 Boundary Value Problems;
 Graphs (Charts);
 Mathematical Models;
 Plasma Pressure;
 Shear Flow;
 Solar Corona;
 Solar Magnetic Field;
 Solar Temperature;
 Solar Wind;
 Solar Physics;
 Magnetohydrodynamics:Solar Prominences;
 Solar Prominences:Models