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Current sheets are important signatures of magnetic reconnection in theeruption of confined solar magnetic structures. Models of Coronal MassEjections (CMEs) involve formation of a current sheet connecting the ejectedflux rope with the post eruption magnetic loops. Current sheets have beenidentified in white light images of CMEs as narrow rays trailing the outwardmoving CME core, and in ultraviolet spectra as narrow bright features emittingthe Fe XVIII line. In this work samples of rays detected in white light imagesor in ultraviolet spectra have been analyzed. Temperatures, widths, and lineintensities of the rays have been measured, and their correlation to the CMEproperties has been studied. The samples show a wide range of temperatures withhot, coronal and cool rays. In some cases, the UV spectra support theidentification of rays as current sheets, but they show that some white lightrays are cool material from the CME core. In many cases, both hot and coolmaterial are present, but offset from each other along the UltraVioletCoronagraph Spectrometer (UVCS) slit. We find that about 18% of the white lightrays show very hot gas consistent with the current sheet interpretation, whileabout 23% show cold gas that we attribute to cool prominence material drainingback from the CME core. The remaining events have ordinary coronaltemperatures, perhaps because they have relaxed back to a quiescent state.

Bright Ray-like Features in the Aftermath of CMEs: White Light vs UV Spectra