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

Abstract

Electron acceleration in the solar corona is often associated with flares and the eruption of twisted magnetic structures known as flux ropes. However, the locations and mechanisms of such particle acceleration during the flare and eruption are still subject to much investigation. Observing the exact sites of particle acceleration can help confirm how the flare and eruption are initiated and how they evolve. Here we use the Atmospheric Imaging Assembly to analyse a flare and erupting flux rope on 2014-April-18, while observations from the Nancay Radio Astronomy Facility allows us to diagnose the sites of electron acceleration during the eruption. Our analysis shows evidence for a pre-formed flux rope which slowly rises and becomes destabilised at the time of a C-class flare, plasma jet and the escape of >75 keV electrons from rope center into the corona. As the eruption proceeds, continued acceleration of electrons with energies of ~5 keV occurs above the flux rope for a period over 5 minutes. At flare peak, one site of electron acceleration is located close to the flare site while another is driven by the erupting flux rope into the corona at speeds 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 sources at 150-445MHz. Following the analysis of Joshi et al. (2015), we conclude that the sites of energetic electrons are consistent with flux rope eruption via a tether-cutting or flux cancellation scenario inside a magnetic fan-spine structure. In total, our radio observations allow us to better understand the evolution of a flux rope eruption and its associated electron acceleration sites, from eruption initiation to propagation into the corona.

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• Observation of An Evolving Magnetic Flux Rope Prior To and During A Solar Eruption
• Quasi-periodic Fast-mode Wave Trains Within a Global EUV Wave and Sequential Transverse Oscillations Detected by SDO/AIA
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• Onset of a Large Ejective Solar Eruption from a Typical Coronal-Jet-Base Field Configuration
• Homologous Accelerated Electron Beams, Quasi-periodic fast-propagating Wave and CME Observed in one Fan-spine Jet
• Using radio triangulation to understand the origin of two subsequent type II radio bursts
• Evolutionary stages and triggering process of a complex eruptive flare with circular and parallel ribbons
• Deriving Large Coronal Magnetic Loop Parameters Using LOFAR J burst Observations
• Oscillations in the 45-5000 MHz Radio Spectrum of the 18 April 2014 Flare
• Bursty acceleration and 3D trajectories of electrons in a solar flare
• Observations of shock propagation through turbulent plasma in the solar corona