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Electron acceleration in the solar corona is often associated with flares andthe eruption of twisted magnetic structures known as flux ropes. However, thelocations and mechanisms of such particle acceleration during the flare anderuption are still subject to much investigation. Observing the exact sites ofparticle acceleration can help confirm how the flare and eruption are initiatedand how they evolve. Here we use the Atmospheric Imaging Assembly to analyse aflare and erupting flux rope on 2014-April-18, while observations from theNancay Radio Astronomy Facility allows us to diagnose the sites of electronacceleration during the eruption. Our analysis shows evidence for a pre-formedflux rope which slowly rises and becomes destabilised at the time of a C-classflare, plasma jet and the escape of >75 keV electrons from rope center into thecorona. As the eruption proceeds, continued acceleration of electrons withenergies of ~5 keV occurs above the flux rope for a period over 5 minutes. Atflare peak, one site of electron acceleration is located close to the flaresite while another is driven by the erupting flux rope into the corona atspeeds of up to 400 km/s. Energetic electrons then fill the erupting volume,eventually allowing the flux rope legs to be clearly imaged from radio sourcesat 150-445MHz. Following the analysis of Joshi et al. (2015), we conclude thatthe sites of energetic electrons are consistent with flux rope eruption via atether-cutting or flux cancellation scenario inside a magnetic fan-spinestructure. In total, our radio observations allow us to better understand theevolution of a flux rope eruption and its associated electron accelerationsites, from eruption initiation to propagation into the corona.

Radio Diagnostics of Electron Acceleration Sites During the Eruption of a Flux Rope in the Solar Corona