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

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dc.contributor.author Morosan, D. E.
dc.contributor.author Palmerio, E.
dc.contributor.author Lynch, B. J.
dc.contributor.author Kilpua, E. K. J.
dc.date.accessioned 2020-10-30T13:40:02Z
dc.date.available 2020-10-30T13:40:02Z
dc.date.issued 2020-01-24
dc.identifier.citation 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
dc.identifier.other PURE: 132717219
dc.identifier.other PURE UUID: d1c0a745-b5e5-47e2-aeea-ec8456ad3634
dc.identifier.other WOS: 000509314100001
dc.identifier.other ORCID: /0000-0002-4489-8073/work/70951176
dc.identifier.other ORCID: /0000-0001-6590-3479/work/70952330
dc.identifier.other ORCID: /0000-0002-8416-1375/work/70952450
dc.identifier.uri http://hdl.handle.net/10138/320862
dc.description.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. en
dc.format.extent 7
dc.language.iso eng
dc.relation.ispartof Astronomy & Astrophysics
dc.rights unspecified
dc.rights.uri info:eu-repo/semantics/openAccess
dc.subject Sun
dc.subject corona
dc.subject radio radiation
dc.subject coronal mass ejections (CMEs)
dc.subject particle emission
dc.subject SOLAR
dc.subject SHOCK
dc.subject EVOLUTION
dc.subject REGIONS
dc.subject MISSION
dc.subject BURSTS
dc.subject BAND
dc.subject CME
dc.subject 115 Astronomy, Space science
dc.title Extended radio emission associated with a breakout eruption from the back side of the Sun en
dc.type Article
dc.contributor.organization Space Physics Research Group
dc.contributor.organization Particle Physics and Astrophysics
dc.contributor.organization Department of Physics
dc.description.reviewstatus Peer reviewed
dc.relation.doi https://doi.org/10.1051/0004-6361/201936878
dc.relation.issn 0004-6361
dc.rights.accesslevel openAccess
dc.type.version publishedVersion

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