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The near-Sun kinematics of coronal mass ejections (CMEs) determine theseverity and arrival time of associated geomagnetic storms. We investigate therelationship between the deprojected speed and kinetic energy of CMEs andmagnetic measures of their solar sources, reconnection flux of associatederuptive events and intrinsic flux rope characteristics. Our data covers theperiod 2010-2014 in solar cycle 24. Using vector magnetograms of source activeregions we estimate the size and nonpotentiality. We compute the total magneticreconnection flux at the source regions of CMEs using the post-eruption arcademethod. By forward modeling the CMEs we find their deprojected geometricparameters and constrain their kinematics and magnetic properties. Based on ananalysis of this database we report that the correlation between CME speed andtheir source active region size and global nonpotentiality is weak, but notnegligible. We find the near-Sun velocity and kinetic energy of CMEs to be wellcorrelated with the associated magnetic reconnection flux. We establish astatistically significant empirical relationship between the CME speed andreconnection flux that may be utilized for prediction purposes. Furthermore, wefind CME kinematics to be related with the axial magnetic field intensity andrelative magnetic helicity of their intrinsic flux ropes. The amount of coronalmagnetic helicity shed by CMEs is found to be well correlated with theirnear-Sun speeds. The kinetic energy of CMEs is well correlated with theirintrinsic magnetic energy density. Our results constrain processes related tothe origin and propagation of CMEs and may lead to better empirical forecastingof their arrival and geoeffectiveness.

Dependence of coronal mass ejection properties on their solar source active region characteristics and associated flare reconnection flux