RADIO DIAGNOSTICS OF ELECTRON ACCELERATION SITES DURING THE ERUPTION OF A FLUX ROPE IN THE SOLAR CORONA

• Published in: The Astrophysical journal Vol. 833; no. 1; pp. 87 - 102
• Main Authors: Carley, Eoin P., Vilmer, Nicole, Gallagher, Peter T.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 10.12.2016; IOP Publishing; American Astronomical Society
• Subjects: ACCELERATION; acceleration of particles; ASTRONOMY; Astrophysics; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BLOWERS; CANCELLATION; Corona; Electron acceleration; ERUPTION; Fluctuations; KEV RANGE; Magnetic flux; MASS; MHZ RANGE; Particle acceleration; Physics; PLASMA JETS; Radio astronomy; Radio observation; Radio sources (astronomy); Sciences of the Universe; Solar and Stellar Astrophysics; SOLAR CORONA; SOLAR FLARES; SOLAR PARTICLES; Spine; SUN; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: particle emission; Sun: radio radiation; TAIL ELECTRONS
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/833/1/87

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 analyze a flare and erupting flux rope on 2014 April 18, while observations from the Nançay Radio Astronomy Facility allow us to diagnose the sites of electron acceleration during the eruption. Our analysis shows evidence of a pre-formed flux rope that slowly rises and becomes destabilized at the time of a C-class flare, plasma jet, and the escape of 75 keV electrons from the 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 the 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−1. Energetic electrons then fill the erupting volume, eventually allowing the flux rope legs to be clearly imaged from radio sources at 150-445 MHz. 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.