  We report multi-wavelength and multi-viewpoint observations of a solar
eruptive event which involves loop-loop interactions. During a C2.0 flare,
motions associated with inflowing and outflowing plasma provide evidence for
ongoing magnetic reconnection. The flare loop top and a rising "concave-up"
feature are connected by a current-sheet-like structure (CSLS). The physical
properties (thickness, length, temperature, and density) of the CSLS are
evaluated. In regions adjacent to the CSLS, the EUV emission (characteristic
temperature at 1.6 MK) begins to increase more than ten minutes prior to the
onset of the flare, and steeply decreases during the decay phase. The reduction
of the emission resembles that expected from coronal dimming. The dynamics of
this event imply a magnetic reconnection rate in the range 0.01 -- 0.05.
