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Author Zuccarello, F. P. ♦ Aulanier, G. ♦ Démoulin, P. ♦ Schmieder, B. ♦ Dudík, J. ♦ Gilchrist, S. A.
Source United States Department of Energy Office of Scientific and Technical Information
Content type Text
Language English
Subject Keyword ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ♦ EXPANSION ♦ IMPLOSIONS ♦ MAGNETIC FLUX ♦ MAGNETOHYDRODYNAMICS ♦ PRESSURE GRADIENTS ♦ ROTATION ♦ SIMULATION ♦ SINKS ♦ SUN ♦ VORTEX FLOW
Abstract Eruptive flares are sudden releases of magnetic energy that involve many phenomena, several of which can be explained by the standard 2D flare model and its realizations in 3D. We analyze a 3D magnetohydrodynamics simulation, in the framework of this model, that naturally explains the contraction of coronal loops in the proximity of the flare sites, as well as the inflow toward the region above the cusp-shaped loops. We find that two vorticity arcs located along the flanks of the erupting magnetic flux rope are generated as soon as the eruption begins. The magnetic arcades above the flux rope legs are then subjected to expansion, rotation, or contraction depending on which part of the vortex flow advects them. In addition to the vortices, an inward-directed magnetic pressure gradient exists in the current sheet below the magnetic flux rope. It results in the formation of a sink that is maintained by reconnection. We conclude that coronal loop apparent implosions observed during eruptive flares are the result of hydromagnetic effects related to the generation of vortex and sink flows when a flux rope moves in a magnetized environment.
ISSN 0004637X
Educational Use Research
Learning Resource Type Article
Publisher Date 2017-03-10
Publisher Place United States
Journal Astrophysical Journal
Volume Number 837
Issue Number 2


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