Extended radio emission associated with a breakout eruption from the back side of the Sun

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Morosan , D E , Palmerio , E , Lynch , B J & Kilpua , E K J 2020 , ' Extended radio emission associated with a breakout eruption from the back side of the Sun ' , Astronomy & Astrophysics , vol. 633 , A141 . https://doi.org/10.1051/0004-6361/201936878

Title: Extended radio emission associated with a breakout eruption from the back side of the Sun
Author: Morosan, D. E.; Palmerio, E.; Lynch, B. J.; Kilpua, E. K. J.
Contributor: University of Helsinki, Space Physics Research Group
University of Helsinki, Particle Physics and Astrophysics
University of Helsinki, Department of Physics
Date: 2020-01-24
Language: eng
Number of pages: 7
Belongs to series: Astronomy & Astrophysics
ISSN: 0004-6361
URI: http://hdl.handle.net/10138/320862
Abstract: Context. Coronal mass ejections (CMEs) on the Sun are the largest explosions in the Solar System that can drive powerful plasma shocks. The eruptions, shocks, and other processes associated to CMEs are efficient particle accelerators and the accelerated electrons in particular can produce radio bursts through the plasma emission mechanism. Aims. Coronal mass ejections and associated radio bursts have been well studied in cases where the CME originates close to the solar limb or within the frontside disc. Here, we study the radio emission associated with a CME eruption on the back side of the Sun on 22 July 2012. Methods. Using radio imaging from the Nancay Radioheliograph, spectroscopic data from the Nancay Decametric Array, and extreme-ultraviolet observations from the Solar Dynamics Observatory and Solar Terrestrial Relations Observatory spacecraft, we determine the nature of the observed radio emission as well as the location and propagation of the CME. Results. We show that the observed low-intensity radio emission corresponds to a type II radio burst or a short-duration type IV radio burst associated with a CME eruption due to breakout reconnection on the back side of the Sun, as suggested by the pre-eruptive magnetic field configuration. The radio emission consists of a large, extended structure, initially located ahead of the CME, that corresponds to various electron acceleration locations. Conclusions. The observations presented here are consistent with the breakout model of CME eruptions. The extended radio emission coincides with the location of the current sheet and quasi-separatrix boundary of the CME flux and the overlying helmet streamer and also with that of a large shock expected to form ahead of the CME in this configuration.
Subject: Sun
radio radiation
coronal mass ejections (CMEs)
particle emission
115 Astronomy, Space science

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