  Employing Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA)
multi-wavelength images, we report the coronal condensation during the magnetic
reconnection (MR) between a system of open and closed coronal loops.
Higher-lying magnetically open structures, observed in AIA 171 A images above
the solar limb, move downward and interact with the lower-lying closed loops,
resulting in the formation of dips in the former. An X-type structure forms at
the interface. The interacting loops reconnect and disappear. Two sets of
newly-reconnected loops then form and recede from the MR region. During the MR
process, bright emission appears sequentially in the AIA 131 A and 304 A
channels repeatedly in the dips of higher-lying open structures. This indicates
the cooling and condensation process of hotter plasma from ~0.9 MK down to ~0.6
MK, and then to ~0.05 MK, also supported by the light curves of the AIA 171 A,
131 A, and 304 A channels. The part of higher-lying open structures supporting
the condensations participate in the successive MR. The condensations without
support by underlying loops then rain back to the solar surface along the
newly-reconnected loops. Our results suggest that the MR between coronal loops
leads to the condensation of hotter coronal plasma and its downflows. MR thus
plays an active role in the mass cycle of coronal plasma because it can
initiate the catastrophic cooling and condensation. This underlines that the
magnetic and thermal evolution has to be treated together and cannot be
separated, even in the case of catastrophic cooling.
