  With the observations from the Atmospheric Imaging Assembly and the
Helioseismic and Magnetic Imager aboard the \emph{Solar Dynamics Observatory},
we statistically investigate the emerging dimmings (EDs) of 24 isolated active
regions (IARs) from June 2010 to May 2011. All the IARs present EDs in lower
temperature lines (e.g., 171 {\AA}) at their early emerging stages, meanwhile
in higher temperature lines (e.g., 211 {\AA}), the ED regions brighten
continuously. There are two type of EDs: fan-shaped and halo-shaped. There are
19 fan-shaped EDs and 5 halo-shaped ones. The EDs appear several to more than
ten hours delay to the first emergence of the IARs. The shortest delay is 3.6
hr and the longest 19.0 hr. The EDs last from 3.3 hr to 14.2 hr, with a mean
duration of 8.3 hr. Before the appearance of the EDs, the emergence rate of the
magnetic flux of the IARs is from 1.2 $\times$ 10$^{19}$ Mx hr$^{-1}$ to 1.4
$\times$ 10$^{20}$ Mx hr$^{-1}$. The larger the emergence rate is, the shorter
the delay time is. While the dimmings appear, the magnetic flux of the IARs
ranges from 8.8 $\times$ 10$^{19}$ Mx to 1.3 $\times$ 10$^{21}$ Mx. These
observations imply that the reconfiguration of the coronal magnetic fields due
to reconnection between the newly-emerging flux and the surrounding existing
fields results in a new thermal distribution which leads to a dimming for the
cooler channel (171 {\AA}) and brightnening in the warmer channels.
