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A Kopp-Pneuman-like Picture of Coronal Mass Ejections

A new coronal mass ejection (CME) picture is described that utilizes a number of attributes commonly found operating during magnetotail reconnection events. We first present key observational constraints any final model of CMEs must explain. We then describe how three-dimensional reconnection occurs in the magnetotail and how magnetotail reconnection helps explain a variety of observed CME attributes. We then argue why reconnection, as usually described in the literature, cannot explain the particle acceleration process that occurs during the CME/flare process. Instead we argue that it is the flow fields that are driven by the relaxation of the magnetic stresses due to reconnection that are ultimately the cause of particle acceleration. In particular, it is the electrons that make up the discharging field-aligned currents, which connect flow field-driven cross field inertial currents in the high corona with the chromosphere, that are in fact the high-energy electrons needed to explain flare ribbons and other high-energy emissions. We compute the expected electron fluxes from these current systems and find that they are of order those required. In addition, we discuss betatron acceleration during the dipolarization process that occurs when the flux rope/CME is ejected and how the hot particles generated during the dipolarization process can lead to traps in solar loops, thereby helping to explain long-duration events. Further, we examine whether particle acceleration by shocks can contribute to the mix. We also note that our new picture eliminates a number of paradoxes, specifically elimination of magnetic flux from the Sun and how the Aly conjecture is not of consequence in our picture. Finally, we examine what will be needed to numerically simulate our picture of a CME.