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Formation and Dynamics of a Solar Eruptive Flux Tube View all abstracts by submitter

Satoshi Inoue   Submitted: 2018-01-25 08:43

Solar eruptions are well known drivers of extreme space weather, which can greatly disturb the Earth's magnetosphere and ionosphere. The triggering process and initial dynamics of these eruptions are still an area of intense study. Here we perform a magnetohydrodynamic simulation taking into account the observed photospheric magnetic field to reveal the dynamics of a solar eruption in a real magnetic environment. In our simulation we confirmed that tether-cutting reconnection occurring locally above the polarity inversion line creates a twisted flux tube which is lifted into a torus unstable area where it loses equilibrium, destroying the force-free state, driving the eruption. Consequently, a more highly twisted flux tube is buildup during this initial phase, can be further accelerated even when it returns to a stable area. We suggest that a nonlinear positive feedback process between the flux tube evolution and reconnection is the key to ensure this extra acceleration.

Authors: Satoshi Inoue, Kanya Kusano, Jörg Büchner, Jan Skála
Projects: None

Publication Status: Published in Nature Communications
Last Modified: 2018-01-29 14:04
Go to main E-Print page  Coronal hole evolution from multi-viewpoint data as input for a STEREO solar wind speed persistence model  The Instruments and Capabilities of the Miniature X-ray Solar Spectrometer (MinXSS) CubeSats  Edit Entry  Download Preprint  Delete Entry 

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