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Evidence for the magnetic breakout model in an equatorial coronal-hole jet.

Kumar, Pankaj and Karpen, Judith T. and Antiochos, Spiro K. and Wyper, Peter F. and DeVore, C. Richard and DeForest, Craig E. (2018) 'Evidence for the magnetic breakout model in an equatorial coronal-hole jet.', Astrophysical journal., 854 (2). p. 155.

Abstract

Small, impulsive jets commonly occur throughout the solar corona, but are especially visible in coronal holes. Evidence is mounting that jets are part of a continuum of eruptions that extends to much larger coronal mass ejections and eruptive flares. Because coronal-hole jets originate in relatively simple magnetic structures, they offer an ideal testbed for theories of energy buildup and release in the full range of solar eruptions. We analyzed an equatorial coronal-hole jet observed by the Solar Dynamics Observatory (SDO)/AIA on 2014 January 9 in which the magnetic-field structure was consistent with the embedded-bipole topology that we identified and modeled previously as an origin of coronal jets. In addition, this event contained a mini-filament, which led to important insights into the energy storage and release mechanisms. SDO/HMI magnetograms revealed footpoint motions in the primary minority-polarity region at the eruption site, but show negligible flux emergence or cancellation for at least 16 hr before the eruption. Therefore, the free energy powering this jet probably came from magnetic shear concentrated at the polarity inversion line within the embedded bipole. We find that the observed activity sequence and its interpretation closely match the predictions of the breakout jet model, strongly supporting the hypothesis that the breakout model can explain solar eruptions on a wide range of scales.

Item Type:Article
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Status:Peer-reviewed
Publisher Web site:https://doi.org/10.3847/1538-4357/aaab4f
Publisher statement:© 2018. The American Astronomical Society. All rights reserved.
Date accepted:25 January 2018
Date deposited:08 March 2018
Date of first online publication:21 February 2018
Date first made open access:08 March 2018

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