  Current sheets are important signatures of magnetic reconnection in the
eruption of confined solar magnetic structures. Models of Coronal Mass
Ejections (CMEs) involve formation of a current sheet connecting the ejected
flux rope with the post eruption magnetic loops. Current sheets have been
identified in white light images of CMEs as narrow rays trailing the outward
moving CME core, and in ultraviolet spectra as narrow bright features emitting
the Fe XVIII line. In this work samples of rays detected in white light images
or in ultraviolet spectra have been analyzed. Temperatures, widths, and line
intensities of the rays have been measured, and their correlation to the CME
properties has been studied. The samples show a wide range of temperatures with
hot, coronal and cool rays. In some cases, the UV spectra support the
identification of rays as current sheets, but they show that some white light
rays are cool material from the CME core. In many cases, both hot and cool
material are present, but offset from each other along the UltraViolet
Coronagraph Spectrometer (UVCS) slit. We find that about 18% of the white light
rays show very hot gas consistent with the current sheet interpretation, while
about 23% show cold gas that we attribute to cool prominence material draining
back from the CME core. The remaining events have ordinary coronal
temperatures, perhaps because they have relaxed back to a quiescent state.
