A post-CME current sheet ( CS ) is a common feature developed behind an erupting flux rope in CME models .
Observationally , white light observations have recorded many occurrences of a thin ray appearing behind a CME eruption that closely resembles a post-CME CS in its spatial correspondence and morphology .
UV and X-ray observations further strengthen this interpretation by the observations of high temperature emission at locations consistent with model predictions .
The next question then becomes whether the properties inside a post-CME current sheet predicted by a model agree with observed properties .
In this work , we assume that the post-CME CS is a consequence of Petschek-like reconnection and that the observed ray-like structure is bounded by a pair of slow mode shocks developed from the reconnection site .
We perform time-dependent ionization calculations and model the UV line emission .
We find that such a model is consistent with SOHO/UVCS observations of the post-CME CS .
The change of Fe XVIII emission in one event implies an inflow speed of \sim 10 km/s and a corresponding reconnection rate of M _ { A } \sim 0.01 .
We calculate the expected X-ray emission for comparison with X-ray observations by Hinode/XRT , as well as the ionic charge states as would be measured in-situ at 1 AU .
We find that the predicted count rate for Hinode/XRT agree with what was observed in a post-CME CS on April 9 , 2008 , and the predicted ionic charge states are consistent with high ionization states commonly measured in the interplanetary CMEs .
The model results depend strongly on the physical parameters in the ambient corona , namely the coronal magnetic field , the electron density and temperature during the CME event .
It is crucial to obtain these ambient coronal parameters and as many facets of the CS properties as possible by observational means so that the post-CME current sheet models can be scrutinized more effectively .