  Earlier studies using extreme-ultraviolet images and line-of-sight
magnetograms from the Solar Dynamics Observatory (SDO) have suggested that
active region (AR) plages and strong network concentrations often have small,
looplike features embedded within them, even though no minority-polarity flux
is visible in the corresponding magnetograms. Because of the unexpected nature
of these findings, we have searched the SDO database for examples of inverted-Y
structures rooted inside "unipolar" plages, with such jetlike structures being
interpreted as evidence for magnetic reconnection between small bipoles and the
dominant-polarity field. Several illustrative cases are presented from the
period 2013--2015, all of which are associated with transient outflows from AR
"moss." The triangular or dome-shaped bases have horizontal dimensions of
$\sim$2--4 Mm, corresponding to $\sim$1--3 granular diameters. We also note
that the spongy-textured Fe IX 17.1 nm moss is not confined to plages, but may
extend into regions where the photospheric field is relatively weak or even has
mixed polarity. We again find a tendency for bright coronal loops seen in the
17.1, 19.3, and 21.1 nm passbands to show looplike fine structure and compact
brightenings at their footpoints. These observations provide further
confirmation that present-day magnetograms are significantly underrepresenting
the amount of minority-polarity flux inside AR plages and again suggest that
footpoint reconnection and small-scale flux cancellation may play a major role
in coronal heating, both inside and outside ARs.
