The Nonuniform Magnetohydrodynamic Nature of the Solar Corona. II. Generalization of Basic Solutions
The method developed recently by Priest (1988) for modeling standing MHD disturbances in the solar corona is extended in several ways. Including inertial effects of the uniform plasma flow distorts the isobars and makes the flow and magnetic field vary with altitude in a manner that depends on the value of the flow speed relative to the cusp speed, the sound speed, and the Alfven speed. More general classes of solutions to the governing equation may be determined by seeking nonseparable solutions with a Green's function technique. Allowing magnetic flux to escape across the side boundaries leads to models which are relevant for coronal holes. The relation of this governing equation to the nonlinear MHD equations is indicated.