One-second variations in non-thermal X-ray source morphologies in an X-class solar flare

Modelling in recent decades suggests that electron acceleration in solar flares occurs on timescales of łeq1,s. Timeseries analyses of spatially integrated hard X-ray (HXR) emission from these electrons has shown similarly rapid variations. Further probing the acceleration process requires characterising the spatial and spectral evolution of the electrons with HXR imaging spectroscopy. However, this has not previously been available on such fast timescales. We provide the first HXR spectroscopic imaging of accelerated electrons in a solar flare on timescales of 1,s. We examined the evolution of non-thermal HXR source morphologies and their spatially averaged spectra in the solar flare SOL2024-05-20T05:14L171C109 (estimated-X16.5) with The non-thermal component of this flare was one of the most intense ever observed, and was the first solar HXR spectroscopic imager capable of 1,s (and sub-second) imaging. These observations are therefore the best so far for high-cadence non-thermal X-ray imaging spectroscopy. We observed physical changes in the non-thermal HXR source morphologies on timescales of 1,s, which is consistent with predictions for the acceleration process. The evolution of the the spatially averaged electron spectral index was slower, however. This may suggest a coherent driver between different acceleration events and/or pathways whose spectrum varies on timescales $>$1,s. Alternatively, it may be an illusion of the spatial averaging in the spectral analysis. Either way, these results show that sub-second electron acceleration in solar flares can be associated with morphological dynamics on similar timescales. This highlights the importance of high spatial resolution sub-second HXR imaging spectroscopy for elucidating this process.