  We present a statistical study of 62 coronal dimming events associated with
Earth-directed CMEs during the quasi-quadrature period of STEREO and SDO. This
unique setting allows us to study both phenomena in great detail and compare
characteristic quantities statistically. Coronal dimmings are observed on-disk
by SDO/AIA and HMI, while the CME kinematics during the impulsive acceleration
phase is studied close to the limb with STEREO/EUVI and COR, minimizing
projection effects. The dimming area, its total unsigned magnetic flux and its
total brightness, reflecting properties of the total dimming region at its
final extent, show the highest correlations with the CME mass ($c\sim0.6-0.7$).
Their corresponding time derivatives, describing the dynamics of the dimming
evolution, show the strongest correlations with the CME peak velocity ($c\sim
0.6$). The highest correlation of $c=0.68\pm0.08$ is found with the mean
intensity of dimmings, indicating that the lower the CME starts in the corona,
the faster it propagates. No significant correlation between dimming parameters
and the CME acceleration was found. However, for events where high-cadence
STEREO observations were available, the mean unsigned magnetic field density in
the dimming regions tends to be positively correlated with the CME peak
acceleration ($c=0.42\pm0.20$). This suggests that stronger magnetic fields
result in higher Lorentz forces providing stronger driving force for the CME
acceleration. Specific coronal dimming parameters correlate with both, CME and
flare quantities providing further evidence for the flare-CME feedback
relationship. For events in which the CME occurs together with a flare, coronal
dimmings statistically reflect the properties of both phenomena.
