Density Structure of a Preeruption Coronal Flux Rope

Abstract

A density model is developed for a coronal flux rope with a specified magnetic field configuration in the noninteracting limit, for which transverse pressure forces can be neglected and flows are rapid enough (>1 km s^-1) to invalidate a hydrostatic solution. In the coronal portion of the flux rope, we find that the plasma density is depleted on-axis, where the magnetic field lines are least twisted.