Volume 590, June 2016
|Number of page(s)||15|
|Published online||31 May 2016|
Coronal mass ejection-related particle acceleration regions during a simple eruptive event
1 LESIA-UMR 8109 – Observatoire de Paris, PSL Research. Univ., CNRS, Univ. P & M Curie and Paris-Diderot, 92190 Meudon, France
2 Station de radioastronomie – Observatoire de Paris, PSL Research Univ., CNRS, University Orléans, OSUC, 18330 Nançay, France
3 Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse (UPS), 31028 Toulouse Cedex 4, France
4 Centre National de la Recherche Scientifique, UMR 5277, 31300 Toulouse, France
5 Space Research Center, University of Costa Rica, 2060 San Jose, Costa Rica
Received: 20 December 2015
Accepted: 23 March 2016
An intriguing feature of many solar energetic particle (SEP) events is the detection of particles over a very extended range of longitudes in the heliosphere. This may be due to peculiarities of the magnetic field in the corona, to a broad accelerator, to cross-field transport of the particles, or to a combination of these processes. The eruptive flare on 26 April 2008 provided an opportunity to study relevant processes under particularly favourable conditions since it occurred in a very quiet solar and interplanetary environment. This enabled us to investigate the physical link between a single well-identified coronal mass ejection (CME), electron acceleration as traced by radio emission, and the production of SEPs. We conduct a detailed analysis, which combines radio observations (Nançay Radio Heliograph and Nançay Decametre Array, Wind/Waves spectrograph) with remote-sensing observations of the corona in extreme ultraviolet (EUV) and white light, as well as in situ measurements of energetic particles near 1AU (SoHO and STEREO spacecraft). By combining images taken from multiple vantage points, we were able to derive the time-dependent evolution of the 3D pressure front that was developing around the erupting CME. Magnetic reconnection in the post-CME current sheet accelerated electrons, which remained confined in closed magnetic fields in the corona, while the acceleration of escaping particles can be attributed to the pressure front ahead of the expanding CME. The CME accelerated electrons remotely from the parent active region, owing to the interaction of its laterally expanding flank, which was traced by an EUV wave, with the ambient corona. SEPs detected at one STEREO spacecraft and SoHO were accelerated later, when the frontal shock of the CME intercepted the spacecraft-connected interplanetary magnetic field line. The injection regions into the heliosphere inferred from the radio and SEP observations are separated in longitude by about 140°. The observations for this event show that it is misleading to interpret multi-spacecraft SEP measurements in terms of one acceleration region in the corona. The different acceleration regions are linked to different vantage points in the interplanetary space.
Key words: acceleration of particles / Sun: coronal mass ejections (CMEs) / Sun: particle emission / Sun: radio radiation / solar-terrestrial relations / Sun: flares
© ESO, 2016
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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