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Magnetic reconnection plays an integral part in nearly all models of solarflares and coronal mass ejections (CMEs). The reconnection heats andaccelerates the plasma, produces energetic electrons and ions, and changes themagnetic topology to form magnetic flux ropes and allow CMEs to escape.Structures that appear between flare loops and CME cores in optical, UV, EUVand X-ray observations have been identified as current sheets and interpretedin terms of the nature of the reconnection process and the energetics of theevents. Many of these studies have used UV spectral observations of hightemperature emission features in the [Fe XVIII] and Si XII lines. In this paperwe discuss several surprising cases in which the [Fe XVIII] and Si XII emissionpeaks are spatially offset from each other. We discuss interpretations based onasymmetric reconnection, on a thin reconnection region within a broaderstreamer-like structure, and on projection effects. Some events seem to beeasily interpreted as projection of a sheet that is extended along the line ofsight that is viewed an angle, but a physical interpretation in terms ofasymmetric reconnection is also plausible. Other events favor an interpretationas a thin current sheet embedded in a streamer-like structure.

Spatial Offsets in Flare-CME Current Sheets