Coronal loop hydrodynamics - The solar flare observed on November 12, 1980 revisited: The UV line emission

We revisit a well-studied solar are whose X-ray emission originating from a simple loop structure was observed by most of the instruments on board SMM on November 12, 1980. The X-ray emission of this are, as observed with the XRP, was successfully modeled previously. Here we include a detailed modeling of the transition region and we compare the hydrodynamic results with the UVSP observations in two EUV lines, measured in areas smaller than the XRP rasters, covering only some portions of the flaring loop (the top and the foot-points). The single loop hydrodynamic model, which fits well the evolution of coronal lines (those observed with the XRP and the Fe XXI 1354.1 Angstrom line observed with the UVSP) fails to model the flux level and evolution of the OV 1371.3 Angstrom line.