Non-force-free solar magnetic fields in magnetohydrostatic equilibrium

The problem of a non--force-free magnetic field in magnetohydrostatic equilibrium with a plasma in a gravitational field is treated analytically. The most extensive development is for the spherical coordinate system, in which axisymmetry is assumed. Dependent variables to be determined are the plasma density, temperature, and pressure and the three components of the magnetic field; all are assumed factorable into their dependences on the independent variables to faciliate possible analytical solution by separation of variables. The governing equations are solved formally for the magnetic field components in terms of the plasma variables. Then a final equation, which must be satisfied by the plasma variables, is derived. Procedures are developed for analyzing this equation systematically and for obtaining sets of self-consistent, particular solutions to the governing equations; a number of such sets of solutions are presented. As an example, one solution set is examined in detail, illustrating the application of these results to the analysis of solar observational data. One of the useful features of these solutions is that they can permit magnetic fields to be inferred quantitatively from observations of the solar plasma properties