  We present the results from analyzing the physical and morphological
properties of 154 dimmings (transient coronal holes) and the associated flares
and coronal mass ejections (CMEs). Each dimming in our 2013 catalog was
processed with the semi-automated Coronal Dimming Tracker using Solar Dynamics
Observatory AIA 193 A observations and HMI magnetograms. Instead of the
typically used difference images, we used our coronal hole detection algorithm
to detect transient dark regions "directly" in extreme ultraviolet (EUV)
images. This allowed us to study dimmings as the footpoints of CMEs - in
contrast with the larger, diffuse dimmings seen in difference images that
represent the projected view of the rising, expanding plasma. Studying the
footpoint-dimming morphology allowed us to better understand the CME structure
in the low corona. While comparing the physical properties of dimmings, flares,
and CMEs we were also able to identify relationships between the different
parts of this complex eruptive phenomenon. We found that larger dimmings are
longer-lived, suggesting that it takes longer to "close down" large open
magnetic regions. Also, during their growth phase, smaller dimmings acquire a
higher magnetic flux imbalance (i. e., become more unipolar) than larger
dimmings. Furthermore, we found that the EUV intensity of dimmings (indicative
of local electron density) correlates with how much plasma was removed and how
energetic the eruption was. Studying the morphology of dimmings (single,
double, fragmented) also helped us identify different configurations of the
quasi-open magnetic field.
