On-Disc Observations of Flux Rope Formation Prior to Its Eruption

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http://hdl.handle.net/10138/214808

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James , A W , Green , L M , Palmerio , E , Valori , G , Reid , H A S , Baker , D , Brooks , D H , van Driel-Gesztelyi , L & Kilpua , E K J 2017 , ' On-Disc Observations of Flux Rope Formation Prior to Its Eruption ' , Solar Physics , vol. 292 , no. 5 , 71 . https://doi.org/10.1007/s11207-017-1093-4

Title: On-Disc Observations of Flux Rope Formation Prior to Its Eruption
Author: James, A. W.; Green, L. M.; Palmerio, E.; Valori, G.; Reid, H. A. S.; Baker, D.; Brooks, D. H.; van Driel-Gesztelyi, L.; Kilpua, E. K. J.
Contributor: University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
Date: 2017-05
Language: eng
Number of pages: 24
Belongs to series: Solar Physics
ISSN: 0038-0938
URI: http://hdl.handle.net/10138/214808
Abstract: Coronal mass ejections (CMEs) are one of the primary manifestations of solar activity and can drive severe space weather effects. Therefore, it is vital to work towards being able to predict their occurrence. However, many aspects of CME formation and eruption remain unclear, including whether magnetic flux ropes are present before the onset of eruption and the key mechanisms that cause CMEs to occur. In this work, the pre-eruptive coronal configuration of an active region that produced an interplanetary CME with a clear magnetic flux rope structure at 1 AU is studied. A forward-S sigmoid appears in extremeultra-violet (EUV) data two hours before the onset of the eruption (SOL2012-06-14), which is interpreted as a signature of a right-handed flux rope that formed prior to the eruption. Flare ribbons and EUV dimmings are used to infer the locations of the flux rope footpoints. These locations, together with observations of the global magnetic flux distribution, indicate that an interaction between newly emerged magnetic flux and pre-existing sunspot field in the days prior to the eruption may have enabled the coronal flux rope to form via tethercutting-like reconnection. Composition analysis suggests that the flux rope had a coronal plasma composition, supporting our interpretation that the flux rope formed via magnetic reconnection in the corona. Once formed, the flux rope remained stable for two hours before erupting as a CME.
Subject: Corona: structures
Coronal mass ejections: initiation and propagation
Magnetic fields: photosphere
Radio emission: active regions
CORONAL MASS EJECTIONS
SOLAR ACTIVE-REGION
EUV IMAGING SPECTROMETER
III RADIO-BURSTS
MAGNETIC-FIELDS
SUNSPOT ROTATION
ATOMIC DATABASE
PLASMA
FLARES
MODEL
114 Physical sciences
115 Astronomy, Space science
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