  The near-Sun kinematics of coronal mass ejections (CMEs) determine the
severity and arrival time of associated geomagnetic storms. We investigate the
relationship between the deprojected speed and kinetic energy of CMEs and
magnetic measures of their solar sources, reconnection flux of associated
eruptive events and intrinsic flux rope characteristics. Our data covers the
period 2010-2014 in solar cycle 24. Using vector magnetograms of source active
regions we estimate the size and nonpotentiality. We compute the total magnetic
reconnection flux at the source regions of CMEs using the post-eruption arcade
method. By forward modeling the CMEs we find their deprojected geometric
parameters and constrain their kinematics and magnetic properties. Based on an
analysis of this database we report that the correlation between CME speed and
their source active region size and global nonpotentiality is weak, but not
negligible. We find the near-Sun velocity and kinetic energy of CMEs to be well
correlated with the associated magnetic reconnection flux. We establish a
statistically significant empirical relationship between the CME speed and
reconnection flux that may be utilized for prediction purposes. Furthermore, we
find CME kinematics to be related with the axial magnetic field intensity and
relative magnetic helicity of their intrinsic flux ropes. The amount of coronal
magnetic helicity shed by CMEs is found to be well correlated with their
near-Sun speeds. The kinetic energy of CMEs is well correlated with their
intrinsic magnetic energy density. Our results constrain processes related to
the origin and propagation of CMEs and may lead to better empirical forecasting
of their arrival and geoeffectiveness.
