Elemental abundances and post-coronal mass ejection current sheet in a very hot active region

A peculiar young active region was observed in 1998 March with the Ultraviolet Coronagraph Spectrometer ( UVCS) over the southwest limb. The spectra showed strong emission in the 974 line of fluorine-like iron, [Fe XVIII], which is brightest at an electron temperature of 10(6.8) K, and lines of Ne IX [Ca XIV], [Ca XV], Fe XVII [Ni xiv, and [Ni xv]. It is the only active region so far observed to show such high temperatures 0.5 R-. above the solar limb. We derive the emission measure and estimate elemental abundances. The active region produced a number of coronal mass ejections (CMEs). After one CME on March 23, a bright post-CME arcade was seen in EIT and Yohkoh/SXT images. Between the arcade and the CME core, UVCS detected a very narrow, very hot feature, most prominently in the [ Fe XVIII] line. This feature seems to be the reconnection current sheet predicted by flux rope models of CMEs. Its thickness, luminosity, and duration seem to be consistent with the expectations of the flux rope models for CME. The elemental abundances in the bright feature are enhanced by a factor of 2 compared to those in the surrounding active region, i.e., a first ionization potential enhancement of 7-8 compared to the usual factor of 3-4.