Modeling a Coronal Mass Ejection from an Extended Filament Channel. I. Eruption and Early Evolution

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Lynch , B J , Palmerio , E , DeVore , C R , Kazachenko , M D , Dahlin , J T , Pomoell , J & Kilpua , E K J 2021 , ' Modeling a Coronal Mass Ejection from an Extended Filament Channel. I. Eruption and Early Evolution ' , Astrophysical Journal , vol. 914 , no. 1 , 39 . https://doi.org/10.3847/1538-4357/abf9a9

Title: Modeling a Coronal Mass Ejection from an Extended Filament Channel. I. Eruption and Early Evolution
Author: Lynch, Benjamin J.; Palmerio, Erika; DeVore, C. Richard; Kazachenko, Maria D.; Dahlin, Joel T.; Pomoell, Jens; Kilpua, Emilia K. J.
Other contributor: University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics

Date: 2021-06
Language: eng
Number of pages: 17
Belongs to series: Astrophysical Journal
ISSN: 0004-637X
DOI: https://doi.org/10.3847/1538-4357/abf9a9
URI: http://hdl.handle.net/10138/331791
Abstract: We present observations and modeling of the magnetic field configuration, morphology, and dynamics of a large-scale, high-latitude filament eruption observed by the Solar Dynamics Observatory. We analyze the 2015 July 9-10 filament eruption and the evolution of the resulting coronal mass ejection (CME) through the solar corona. The slow streamer-blowout CME leaves behind an elongated post-eruption arcade above the extended polarity inversion line that is only poorly visible in extreme ultraviolet (EUV) disk observations and does not resemble a typical bright flare-loop system. Magnetohydrodynamic (MHD) simulation results from our data-inspired modeling of this eruption compare favorably with the EUV and white-light coronagraph observations. We estimate the reconnection flux from the simulation's flare-arcade growth and examine the magnetic-field orientation and evolution of the erupting prominence, highlighting the transition from an erupting sheared-arcade filament channel into a streamer-blowout flux-rope CME. Our results represent the first numerical modeling of a global-scale filament eruption where multiple ambiguous and complex observational signatures in EUV and white light can be fully understood and explained with the MHD simulation. In this context, our findings also suggest that the so-called stealth CME classification, as a driver of unexpected or "problem" geomagnetic storms, belongs more to a continuum of observable/nonobservable signatures than to separate or distinct eruption processes.
Subject: MAGNETIC-HELICITY
ENERGY BUILDUP
CURRENT SHEETS
SOLAR
RECONNECTION
DYNAMICS
PROMINENCE
CONDENSATION
ONSET
CMES
114 Physical sciences
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