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 analyzing 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 κ index for the Fe xvi 262.976 ...
Context. Remote observations of solar flare ion acceleration are rather limited. Theoretical predict...
Context. Remote observations of solar flare ion acceleration are rather limited. Theoretical predict...
Context. Observation of coronal extreme ultra-violet (EUV) spectral lines sensitive to different tem...
In a solar flare, a large fraction of the magnetic energy released is converted rapidly to the kinet...
In a solar flare, a large fraction of the magnetic energy released is converted rapidly to the kinet...
In a solar flare, a large fraction of the magnetic energy released is converted rapidly to the kinet...
Context. The properties of solar flare plasma can be determined from the observation of optically th...
Context: The properties of solar flare plasma can be determined from the observation of optically th...
Context. The properties of solar flare plasma can be determined from the observation of optically th...
Context. The properties of solar flare plasma can be determined from the observation of optically th...
Context. The properties of solar flare plasma can be determined from the observation of optically th...
Context: The properties of solar flare plasma can be determined from the observation of optically th...
Magnetohydrodynamic plasma turbulence is believed to play a vital role in the production of energeti...
This paper presents a detailed study of excess line broadening in EUV emission lines during the impu...
Context. Remote observations of solar flare ion acceleration are rather limited. Theoretical predict...
Context. Remote observations of solar flare ion acceleration are rather limited. Theoretical predict...
Context. Remote observations of solar flare ion acceleration are rather limited. Theoretical predict...
Context. Observation of coronal extreme ultra-violet (EUV) spectral lines sensitive to different tem...
In a solar flare, a large fraction of the magnetic energy released is converted rapidly to the kinet...
In a solar flare, a large fraction of the magnetic energy released is converted rapidly to the kinet...
In a solar flare, a large fraction of the magnetic energy released is converted rapidly to the kinet...
Context. The properties of solar flare plasma can be determined from the observation of optically th...
Context: The properties of solar flare plasma can be determined from the observation of optically th...
Context. The properties of solar flare plasma can be determined from the observation of optically th...
Context. The properties of solar flare plasma can be determined from the observation of optically th...
Context. The properties of solar flare plasma can be determined from the observation of optically th...
Context: The properties of solar flare plasma can be determined from the observation of optically th...
Magnetohydrodynamic plasma turbulence is believed to play a vital role in the production of energeti...
This paper presents a detailed study of excess line broadening in EUV emission lines during the impu...
Context. Remote observations of solar flare ion acceleration are rather limited. Theoretical predict...
Context. Remote observations of solar flare ion acceleration are rather limited. Theoretical predict...
Context. Remote observations of solar flare ion acceleration are rather limited. Theoretical predict...
Context. Observation of coronal extreme ultra-violet (EUV) spectral lines sensitive to different tem...