  In a solar flare, a large fraction of the magnetic energy released is
converted rapidly to the kinetic energy of non-thermal particles and bulk
plasma motion. This will likely result in non-equilibrium particle
distributions and turbulent plasma conditions. We investigate this by analysing
the profiles of high-temperature extreme ultraviolet emission lines from a
major flare (SOL2014-03-29T17:44) observed by the EUV Imaging Spectrometer
(EIS) on Hinode. We find that in many locations the line profiles are
non-Gaussian, consistent with a kappa-distribution of emitting ions with
properties that vary in space and time. At the flare footpoints, close to sites
of hard X-ray emission from non-thermal electrons, the kappa-index for the Fe
XVI 262.976 angstrom line at 3 MK takes values of 3-5. In the corona, close to
a low-energy HXR source, the Fe XXIII 263.760 angstrom line at 15 MK shows
kappa values of typically 4-7. The observed trends in the kappa parameter show
that we are most likely detecting the properties of the ion population rather
than any instrumental effects. We calculate that a non-thermal ion population
could exist if locally accelerated on timescales < 0.1 s. However, observations
of net redshifts in the lines also imply the presence of plasma downflows which
could lead to bulk turbulence, with increased non-Gaussianity in cooler
regions. Both interpretations have important implications for theories of solar
flare particle acceleration.
