Simulation of a Solar Jet Formed from an Untwisting Flux Rope Interacting with a Null Point

Coronal jets are eruptions identified by a collimated, sometimes twisted spire. They are small-scale energetic events compared with flares. Using multiwavelength observations from the Solar Dynamics Observatory/Atmospheric Imaging Assembly and a magnetogram from Hinode/Spectro-Polarimeter (Hinode/SP...

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Main Authors: Jiahao Zhu, Yang Guo, Mingde Ding, Brigitte Schmieder
Format: Article
Language:English
Published: IOP Publishing 2023-01-01
Series:The Astrophysical Journal
Subjects:
Online Access:https://doi.org/10.3847/1538-4357/acc9a7
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author Jiahao Zhu
Yang Guo
Mingde Ding
Brigitte Schmieder
author_facet Jiahao Zhu
Yang Guo
Mingde Ding
Brigitte Schmieder
author_sort Jiahao Zhu
collection DOAJ
description Coronal jets are eruptions identified by a collimated, sometimes twisted spire. They are small-scale energetic events compared with flares. Using multiwavelength observations from the Solar Dynamics Observatory/Atmospheric Imaging Assembly and a magnetogram from Hinode/Spectro-Polarimeter (Hinode/SP), we study the formation and evolution of a jet occurring on 2019 March 22 in NOAA Active Region 12736. A zero- β magnetohydrodynamic simulation is conducted to probe the initiation mechanisms and appearance of helical motion during this jet event. As the simulation reveals, there are two pairs of field lines at the jet base, indicating two distinct magnetic structures. One structure outlines a flux rope lying low above the photosphere in the north of a bald patch region, and the other structure shows a null point high in the corona in the south. The untwisting motions of the observed flux rope were recovered by adding an anomalous (artificial) resistivity in the simulation. A reconnection occurs at the bald patch in the flux rope structure, which is moving upward and simultaneously encounters the field lines of the null point structure. The interaction of the two structures results in the jet, while the twist of the flux rope is transferred to the jet by the reconnected field lines. The rotational motion of the flux rope is proposed to be an underlying trigger of this process and responsible for helical motions in the jet spire.
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spelling doaj.art-f009e0e892cd466ebf07d79d0f9b4d662023-09-03T13:36:47ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-019491210.3847/1538-4357/acc9a7Simulation of a Solar Jet Formed from an Untwisting Flux Rope Interacting with a Null PointJiahao Zhu0https://orcid.org/0000-0003-4239-8101Yang Guo1https://orcid.org/0000-0002-9293-8439Mingde Ding2https://orcid.org/0000-0002-4978-4972Brigitte Schmieder3https://orcid.org/0000-0003-3364-9183School of Astronomy and Space Science and Key Laboratory for Modern Astronomy and Astrophysics, Nanjing University , Nanjing 210023, People's Republic of China ; guoyang@nju.edu.cnSchool of Astronomy and Space Science and Key Laboratory for Modern Astronomy and Astrophysics, Nanjing University , Nanjing 210023, People's Republic of China ; guoyang@nju.edu.cnSchool of Astronomy and Space Science and Key Laboratory for Modern Astronomy and Astrophysics, Nanjing University , Nanjing 210023, People's Republic of China ; guoyang@nju.edu.cnLESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris , 5 place Jules Janssen, F-92190 Meudon, France; Centre for Mathematical Plasma Astrophysics , Dept. of Mathematics, KU Leuven, B-3001 Leuven, Belgium; University of Glasgow , School of Physics and Astronomy, Glasgow, G128QQ, UKCoronal jets are eruptions identified by a collimated, sometimes twisted spire. They are small-scale energetic events compared with flares. Using multiwavelength observations from the Solar Dynamics Observatory/Atmospheric Imaging Assembly and a magnetogram from Hinode/Spectro-Polarimeter (Hinode/SP), we study the formation and evolution of a jet occurring on 2019 March 22 in NOAA Active Region 12736. A zero- β magnetohydrodynamic simulation is conducted to probe the initiation mechanisms and appearance of helical motion during this jet event. As the simulation reveals, there are two pairs of field lines at the jet base, indicating two distinct magnetic structures. One structure outlines a flux rope lying low above the photosphere in the north of a bald patch region, and the other structure shows a null point high in the corona in the south. The untwisting motions of the observed flux rope were recovered by adding an anomalous (artificial) resistivity in the simulation. A reconnection occurs at the bald patch in the flux rope structure, which is moving upward and simultaneously encounters the field lines of the null point structure. The interaction of the two structures results in the jet, while the twist of the flux rope is transferred to the jet by the reconnected field lines. The rotational motion of the flux rope is proposed to be an underlying trigger of this process and responsible for helical motions in the jet spire.https://doi.org/10.3847/1538-4357/acc9a7Solar magnetic fieldsSolar magnetic reconnectionMagnetohydrodynamicsSolar activitySolar active regions
spellingShingle Jiahao Zhu
Yang Guo
Mingde Ding
Brigitte Schmieder
Simulation of a Solar Jet Formed from an Untwisting Flux Rope Interacting with a Null Point
The Astrophysical Journal
Solar magnetic fields
Solar magnetic reconnection
Magnetohydrodynamics
Solar activity
Solar active regions
title Simulation of a Solar Jet Formed from an Untwisting Flux Rope Interacting with a Null Point
title_full Simulation of a Solar Jet Formed from an Untwisting Flux Rope Interacting with a Null Point
title_fullStr Simulation of a Solar Jet Formed from an Untwisting Flux Rope Interacting with a Null Point
title_full_unstemmed Simulation of a Solar Jet Formed from an Untwisting Flux Rope Interacting with a Null Point
title_short Simulation of a Solar Jet Formed from an Untwisting Flux Rope Interacting with a Null Point
title_sort simulation of a solar jet formed from an untwisting flux rope interacting with a null point
topic Solar magnetic fields
Solar magnetic reconnection
Magnetohydrodynamics
Solar activity
Solar active regions
url https://doi.org/10.3847/1538-4357/acc9a7
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AT yangguo simulationofasolarjetformedfromanuntwistingfluxropeinteractingwithanullpoint
AT mingdeding simulationofasolarjetformedfromanuntwistingfluxropeinteractingwithanullpoint
AT brigitteschmieder simulationofasolarjetformedfromanuntwistingfluxropeinteractingwithanullpoint