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Theoretically, CME kinematics are related to magnetic reconnection processesin the solar corona. However, the current quantitative understanding of thisrelationship is based on the analysis of only a handful of events. Here wereport a statistical study of 60 CME-flare events from August 2010 to December2013. We investigate kinematic properties of CMEs and magnetic reconnection inthe low corona during the early phase of the eruptions, by combining limbobservations from STEREO with simultaneous on-disk views from SDO. For a subsetof 42 events with reconnection rate evaluated by the magnetic fluxes swept bythe flare ribbons on the solar disk observed from SDO, we find a strongcorrelation between the peak CME acceleration and the peak reconnection rate.Also, the maximum velocities of relatively fast CMEs (> 600 km/s) arepositively correlated with the reconnection flux, but no such correlation isfound for slow CMEs. A time-lagged correlation analysis suggests that thedistribution of the time lag of CME acceleration relative to reconnection rateexhibits three peaks, approximately 10 minutes apart, and on average,acceleration-lead events have smaller reconnection rates. We further comparethe CME total mechanical energy with the estimated energy in the current sheet.The comparison suggests that, for small-flare events, reconnection in thecurrent sheet alone is insufficient to fuel CMEs. Results from this studysuggest that flare reconnection may dominate the acceleration of fast CMEs, butfor events of slow CMEs and weak reconnection, other mechanisms may be moreimportant.

How Does Magnetic Reconnection Drive the Early Stage Evolution of Coronal Mass Ejections?