Authors: Yuhong Fan (NSF NCAR)

We present a magnetohydrodynamic simulation of the evolution of a prominence-forming coronal flux rope from quasi-equilibrium to eruption beneath a coronal streamer. The simulation produces a prominence-cavity system that qualitatively reproduces several observed features, including the coronal cavity, prominence horns, the central hot core (the so-called X-ray “chewy nougat”), filament barbs, and the development of the slow-rise phase preceding eruption onset. We discuss the physical nature of these observed features as natural consequences of a prominence-forming coronal flux rope. Using the MHD model, we further carry out forward modeling of the Doppler and spectropolarimetric signatures expected from the future COronal Solar Magnetism Observatory (COSMO) Large Coronagraph (LC), and demonstrate how such observations can be used to diagnose the non-potentiality of the coronal magnetic field within cavities.