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Coronal condensation and rain are a crucial part of the mass cycle betweenthe corona and chromosphere. In some cases, condensation and subsequent rainoriginate in the magnetic dips formed during magnetic reconnection. Thisprovides a new and alternative formation mechanism for coronal rain. Until now,only off-limb, rather than on-disk, condensation events during reconnectionhave been reported. In this paper, employing extreme-ultraviolet (EUV) imagesof the Solar Terrestrial Relations Observatory (STEREO) and Solar DynamicsObservatory (SDO), we investigate the condensations facilitated by reconnectionfrom 2011 July 14 to 15, when STEREO was in quadrature with respect to theSun-Earth line. Above the limb, in STEREO/EUV Imager (EUVI) 171 \AA~images,higher-lying open structures move downward, reconnect with the lower-lyingclosed loops, and form dips. Two sets of newly reconnected structures thenform. In the dips, bright condensations occur in EUVI 304 \AA~images repeatedlywhich then flow downward to the surface. In the on-disk observations bySDO/Atmospheric Imaging Assembly (AIA) in the 171 \AA~channel, these magneticstructures are difficult to identify. Dark condensations appear in AIA 304\AA~images, and then move to the surface as on-disk coronal rain. The coolingand condensation of coronal plasma is revealed by the EUV light curves. If onlythe on-disk observations would be available, the relation between thecondensations and reconnection, shown clearly by the off-limb observations,would not be identified. Thus, we suggest that some on-disk condensation eventsseen in transition region and chromospheric lines may be facilitated byreconnection.

On-disk solar coronal condensations facilitated by magnetic reconnection between open and closed magnetic structures