A Study of Pre-flare Solar Coronal Magnetic Fields: Magnetic Flux Ropes

Magnetic flux ropes (MFRs) are thought to be the central structures of solar eruptions, and their ideal MHD instabilities can trigger the eruption. Here we performed a study of all the MFR configurations that lead to major solar flares, either eruptive or confined, from 2011 to 2017 near the solar d...

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Vydáno v:The Astrophysical journal Ročník 884; číslo 1; s. 73 - 88
Hlavní autoři: Duan, Aiying, Jiang, Chaowei, He, Wen, Feng, Xueshang, Zou, Peng, Cui, Jun
Médium: Journal Article
Jazyk:angličtina
Vydáno: Philadelphia The American Astronomical Society 10.10.2019
IOP Publishing
Témata:
Astrophysics
Control stability
Coronal magnetic fields
Magnetic fields
Magnetic flux
Magnetic reconnection
Magnetism
Magnetohydrodynamics
Parameters
Solar active region magnetic fields
Solar corona
Solar coronal mass ejections
Solar filament eruptions
Solar flares
Solar magnetic field
Solar magnetic fields
Solar prominences
Three dimensional models
Toruses
ISSN:0004-637X, 1538-4357
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Abstract Magnetic flux ropes (MFRs) are thought to be the central structures of solar eruptions, and their ideal MHD instabilities can trigger the eruption. Here we performed a study of all the MFR configurations that lead to major solar flares, either eruptive or confined, from 2011 to 2017 near the solar disk center. The coronal magnetic field is reconstructed from observed magnetograms, and based on magnetic twist distribution, we identified the MFR, which is defined as a coherent group of magnetic field lines winding an axis with more than one turn. It is found that 90% of the events possess pre-flare MFRs, and their three-dimensional structures are much more complex in details than theoretical MFR models. We further constructed a diagram based on two parameters, the magnetic twist number which controls the kink instability (KI), and the decay index which controls the torus instability (TI). It clearly shows lower limits for TI and KI thresholds, which are ncrit = 1.3 and , respectively, as all the events above ncrit and nearly 90% of the events above erupted. Furthermore, by such criterion, over 70% of the events can be discriminated between eruptive and confined flares, and KI seems to play a nearly equally important role as TI in discriminating between the two types of flares. More than half of the events with both parameters are below the lower limits, and 29% are eruptive. These events might be triggered by magnetic reconnection rather than MHD instabilities.
AbstractList Magnetic flux ropes (MFRs) are thought to be the central structures of solar eruptions, and their ideal MHD instabilities can trigger the eruption. Here we performed a study of all the MFR configurations that lead to major solar flares, either eruptive or confined, from 2011 to 2017 near the solar disk center. The coronal magnetic field is reconstructed from observed magnetograms, and based on magnetic twist distribution, we identified the MFR, which is defined as a coherent group of magnetic field lines winding an axis with more than one turn. It is found that 90% of the events possess pre-flare MFRs, and their three-dimensional structures are much more complex in details than theoretical MFR models. We further constructed a diagram based on two parameters, the magnetic twist number which controls the kink instability (KI), and the decay index which controls the torus instability (TI). It clearly shows lower limits for TI and KI thresholds, which are n crit  = 1.3 and , respectively, as all the events above n crit and nearly 90% of the events above erupted. Furthermore, by such criterion, over 70% of the events can be discriminated between eruptive and confined flares, and KI seems to play a nearly equally important role as TI in discriminating between the two types of flares. More than half of the events with both parameters are below the lower limits, and 29% are eruptive. These events might be triggered by magnetic reconnection rather than MHD instabilities.
Magnetic flux ropes (MFRs) are thought to be the central structures of solar eruptions, and their ideal MHD instabilities can trigger the eruption. Here we performed a study of all the MFR configurations that lead to major solar flares, either eruptive or confined, from 2011 to 2017 near the solar disk center. The coronal magnetic field is reconstructed from observed magnetograms, and based on magnetic twist distribution, we identified the MFR, which is defined as a coherent group of magnetic field lines winding an axis with more than one turn. It is found that 90% of the events possess pre-flare MFRs, and their three-dimensional structures are much more complex in details than theoretical MFR models. We further constructed a diagram based on two parameters, the magnetic twist number which controls the kink instability (KI), and the decay index which controls the torus instability (TI). It clearly shows lower limits for TI and KI thresholds, which are n crit = 1.3 and \(| {T}_{w}{| }_{\mathrm{crit}}=2\), respectively, as all the events above n crit and nearly 90% of the events above \(| {T}_{w}{| }_{\mathrm{crit}}\) erupted. Furthermore, by such criterion, over 70% of the events can be discriminated between eruptive and confined flares, and KI seems to play a nearly equally important role as TI in discriminating between the two types of flares. More than half of the events with both parameters are below the lower limits, and 29% are eruptive. These events might be triggered by magnetic reconnection rather than MHD instabilities.
Magnetic flux ropes (MFRs) are thought to be the central structures of solar eruptions, and their ideal MHD instabilities can trigger the eruption. Here we performed a study of all the MFR configurations that lead to major solar flares, either eruptive or confined, from 2011 to 2017 near the solar disk center. The coronal magnetic field is reconstructed from observed magnetograms, and based on magnetic twist distribution, we identified the MFR, which is defined as a coherent group of magnetic field lines winding an axis with more than one turn. It is found that 90% of the events possess pre-flare MFRs, and their three-dimensional structures are much more complex in details than theoretical MFR models. We further constructed a diagram based on two parameters, the magnetic twist number which controls the kink instability (KI), and the decay index which controls the torus instability (TI). It clearly shows lower limits for TI and KI thresholds, which are ncrit = 1.3 and , respectively, as all the events above ncrit and nearly 90% of the events above erupted. Furthermore, by such criterion, over 70% of the events can be discriminated between eruptive and confined flares, and KI seems to play a nearly equally important role as TI in discriminating between the two types of flares. More than half of the events with both parameters are below the lower limits, and 29% are eruptive. These events might be triggered by magnetic reconnection rather than MHD instabilities.
Author Cui, Jun
Jiang, Chaowei
He, Wen
Zou, Peng
Duan, Aiying
Feng, Xueshang
Author_xml – sequence: 1
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  orcidid: 0000-0002-1916-1053
  surname: Duan
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  organization: Sun Yat-sen University School of Atmospheric Sciences, Zhuhai 519000, People's Republic of China
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  surname: Jiang
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  organization: Institute of Space Science and Applied Technology , Harbin Institute of Technology, Shenzhen 518055, People's Republic of China
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  surname: He
  fullname: He, Wen
  organization: Institute of Space Science and Applied Technology , Harbin Institute of Technology, Shenzhen 518055, People's Republic of China
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  givenname: Xueshang
  orcidid: 0000-0001-8605-2159
  surname: Feng
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  organization: Chinese Academy of Sciences SIGMA Weather Group, State Key Laboratory for Space Weather, National Space Science Center, Beijing 100190, People's Republic of China
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  givenname: Peng
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  surname: Zou
  fullname: Zou, Peng
  organization: Institute of Space Science and Applied Technology , Harbin Institute of Technology, Shenzhen 518055, People's Republic of China
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  givenname: Jun
  orcidid: 0000-0002-4721-8184
  surname: Cui
  fullname: Cui, Jun
  organization: CAS Center for Excellence in Comparative Planetology, People's Republic of China
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Copyright 2019. The American Astronomical Society. All rights reserved.
Copyright IOP Publishing Oct 10, 2019
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Snippet Magnetic flux ropes (MFRs) are thought to be the central structures of solar eruptions, and their ideal MHD instabilities can trigger the eruption. Here we...
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StartPage 73
SubjectTerms Astrophysics
Control stability
Coronal magnetic fields
Magnetic fields
Magnetic flux
Magnetic reconnection
Magnetism
Magnetohydrodynamics
Parameters
Solar active region magnetic fields
Solar corona
Solar coronal mass ejections
Solar filament eruptions
Solar flares
Solar magnetic field
Solar magnetic fields
Solar prominences
Three dimensional models
Toruses
Title A Study of Pre-flare Solar Coronal Magnetic Fields: Magnetic Flux Ropes
URI https://iopscience.iop.org/article/10.3847/1538-4357/ab3e33
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