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Flare kernels are compact features located in the solar chromosphere that arethe sites of rapid heating and plasma upflow during the rise phase of flares.An example is presented from a M1.1 class flare observed on 2011 February 1607:44 UT for which the location of the upflow region seen by EIS can beprecisely aligned to high spatial resolution images obtained by the AtmosphericImaging Assembly (AIA) and Heliospheric Magnetic Imager (HMI) on board theSolar Dynamics Observatory (SDO). A string of bright flare kernels is found tobe aligned with a ridge of strong magnetic field, and one kernel site ishighlighted for which an upflow speed of 400 km/s is measured in lines formedat 10-30 MK. The line-of-sight magnetic field strength at this location is 1000G. Emission over a continuous range of temperatures down to the chromosphere isfound, and the kernels have a similar morphology at all temperatures and arespatially coincident with sizes at the resolution limit of the AIA instrument(< 400 km). For temperatures of 0.3-3.0 MK the EIS emission lines show multiplevelocity components, with the dominant component becoming more blue-shiftedwith temperature from a redshift of 35 km/s at 0.3 MK to a blueshift of 60 km/sat 3.0 MK. Emission lines from 1.5-3.0 MK show a weak redshifted component ataround 60-70 km/s implying multi-directional flows at the kernel site.Significant non-thermal broadening corresponding to velocities of 120 km/s isfound at 10-30MK, and the electron density in the kernel, measured at 2 MK, is3.4 x 10^10 cm-3. Finally, the Fe XXIV 192.03/255.11 ratio suggests that theEIS calibration has changed since launch, with the long wavelength channel lesssensitive than the short wavelength channel by around a factor two.

Properties of a solar flare kernel observed by Hinode and SDO