The Hydromagnetic Origin of the Two Dynamical Types of Solar Coronal Mass Ejections

Abstract

We propose a qualitative theory relating flux rope coronal mass ejections (CMEs) to initial states, represented by inverse or normal quiescent prominences corresponding to whether the flux rope magnetic field circulates in the same or opposite sense relative to the surrounding coronal magnetic field. Our theory explains the observed dual character of CME speed-height profiles in terms of the interplays between flux rope expulsion and magnetic reconnection in topologically different magnetic environments and relates CMEs, prominences, and flares to coronal magnetic field reversal during activity maximum.