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The Extreme-ultraviolet Imaging Spectrometer (EIS) on the Hinode spacecraftobserved flare footpoint regions coincident with a surge for a M3.7 flareobserved on 25 September 2011 at N12 E33 in active region 11302. The flare wasobserved in spectral lines of O VI, Fe X, Fe XII, Fe XIV, Fe XV, Fe XVI, FeXVII, Fe XXIII and Fe XXIV. The EIS observations were made coincident with hardX-ray bursts observed by the Reuven Ramaty High Energy Solar SpectroscopicImager (RHESSI). Overlays of the RHESSI images on the EIS raster images atdifferent wavelengths show a spatial coincidence of features in the RHESSIimages with the EIS upflow and downflow regions, as well as loop-top ornear-loop-top regions. A complex array of phenomena was observed includingmultiple evaporation regions and the surge, which was also observed by theSolar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) telescopes.The slit of the EIS spectrometer covered several flare footpoint regions fromwhich evaporative upflows in Fe XXIII and Fe XXIV lines were observed withDoppler speeds greater than 500 km s$^{-1}$. For ions such as Fe XV bothevaporative outflows (~200 km s$^{-1}$) and downflows (~30-50 km s$^{-1}$) wereobserved. Non-thermal motions from 120 to 300 km s$^{-1}$ were measured inflare lines. In the surge, Doppler speeds are found from about 0 to over 250 kms$^{-1}$ in lines from ions such as Fe XIV. The non-thermal motions could bedue to multiple sources slightly Doppler-shifted from each other or turbulencein the evaporating plasma. We estimate the energetics of the hard X-ray burstand obtain a total flare energy in accelerated electrons of$\geq7\times10^{28}$ ergs. This is a lower limit because only an upper limitcan be determined for the low energy cutoff to the electron spectrum. We findthat detailed modeling of this event would require a multi-threaded model dueto its complexity.

Flare Footpoint Regions and a Surge Observed by the Hinode/EUV Imaging Spectrometer (EIS), RHESSI, and SDO/AIA