Chirality and magnetic configuration associated with two-ribbon solar flares: AR 10930 versus AR 11158
arXiv:1810.13124 · doi:10.1016/j.asr.2020.03.034
Abstract
The structural property of the magnetic field in flare-bearing solar active regions (ARs) is one of the key aspects for understanding and forecasting solar flares. In this paper, we make a comparative analysis on the chirality and magnetic configurations associated with two X-class two-ribbon flares happening in AR 10930 and AR 11158. The photospheric magnetic fields of the two ARs were observed by space-based instruments, and the corresponding coronal magnetic fields were calculated based on the nonlinear force-free field model. The analysis shows that the electric current in the two ARs was distributed mostly around the main polarity inversion lines (PILs) where the flares happened, and the magnetic chirality (indicated by the signs of force-free factor ) along the main PILs is opposite for the two ARs, i.e., left-handed () for AR 10930 and right-handed () for AR 11158. It is found that, for both the flare events, a prominent magnetic connectivity (featured by co-localized strong and strong current density distributions) was formed along the main PIL before flare and was totally broken after flare eruption. The two branches of the broken magnetic connectivity, combined with the prominent magnetic connectivity before flare, compose the opposite magnetic configurations in the two ARs owing to their opposite chirality, i.e., Z-shaped configuration in AR 10930 with left-handed chirality and inverse Z-shaped configuration in AR 11158 with right-handed chirality. It is speculated that two-ribbon flares can be generally classified to these two magnetic configurations by chirality in the flare source regions of ARs.
arXiv comment24 pages, 9 figures, 2 tables, AdSpR(2020)65:2828, doi:10.1016/j.asr.2020.03.034
References in corpus (51)
- Astropy: A Community Python Package for Astronomy
- The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package
- The Solar Optical Telescope for the Hinode Mission: An Overview
- An Observational Overview of Solar Flares
- The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: SHARPs -- Space-weather HMI Active Region Patches
- The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Overview and Performance
- Superflares on Solar Type Stars Observed with Kepler I. Statistical Properties of Superflares
- Evolution of Magnetic Field and Energy in A Major Eruptive Active Region Based on SDO/HMI Observation
- The Kepler Catalog of Stellar Flares
- Observation of An Evolving Magnetic Flux Rope Prior To and During A Solar Eruption
- Non-linear force-free field modeling of a solar active region around the time of a major flare and coronal mass ejection
- Superflares on Ordinary Solar-Type Stars
- The standard flare model in three dimensions III. Slip-running reconnection properties
- The standard flare model in three dimensions. II. Upper limit on solar flare energy
- Modelling Quasi-Periodic Pulsations in Solar and Stellar Flares
- Superflares on Solar-Type Stars Observed with Kepler II. Photometric Variability of Superflare-Generating Stars : A Signature of Stellar Rotation and Starspots
- Electric current in flares ribbons: observations and 3D standard model
- Global Properties of Solar Flares
- History and Development of Coronal Mass Ejections as a Key Player in Solar Terrestrial Relationship
- Response of the Photospheric Magnetic Field to the X2.2 Flare on 2011 February 15
- Interaction between a fast rotating sunspot and ephemeral regions as the origin of the major solar event on 2006 December 13
- Observational Evidence of Back-reaction on the Solar Surface Associated with Coronal Magnetic Restructuring in Solar Eruptions
- Origin and Structures of Solar Eruptions I: Magnetic Flux Rope (Invited Review)
- SunPy - Python for Solar Physics
- Chirality and Magnetic Configurations of Solar Filaments
- The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: Optimization of the Spectral Line Inversion Code
- Rapid Changes of Photospheric Magnetic Field after Tether-Cutting Reconnection and Magnetic Implosion
- Hinode Observations of Vector Magnetic Field Change Associated with a Flare on 2006 December 13
- Magnetohydrodynamic Simulation of the X9.3 Flare on 2017 September 6: Evolving Magnetic Topology
- Extreme Ultraviolet Imaging of Three-dimensional Magnetic Reconnection in a Solar Eruption
- Magnetic Field Extrapolations in the Corona: Success and Future Improvements
- Magnetohydrodynamic Modeling of a Solar Eruption Associated with X9.3 Flare Observed in Active Region 12673
- Buildup and Release of Magnetic Twist during the X3.4 Solar Flare of December 13, 2006
- Magnetic Activity of F-, G-, and K-type Stars in the LAMOST-Kepler Field
- A Circular White-Light Flare with Impulsive and Gradual White-Light Kernels
- Activity Analyses for Solar-Type Stars Observed With Kepler. I. Proxies of Magnetic Activity
- On flare predictability based on sunspot group evolution
- Starspots, Stellar Cycles and Stellar Flares: Lessons from Solar Dynamo Models
- Investigating Energetic X-Shaped Flares on the Outskirts of A Solar Active Region
- The nonpotentiality of coronae of solar active regions, the dynamics of the surface magnetic field, and the potential for large flares
- Activity Analyses for Solar-type Stars Observed with Kepler. II. Magnetic Feature Versus Flare Activity
- Torsional Alfven wave embedded ICME magnetic cloud and corresponding geomagnetic storm
- Nonlinear force-free coronal magnetic field extrapolation scheme based on the direct boundary integral formulation
- Magnetic activity analysis for a sample of G-type main sequence \emph{Kepler} targets
- A Statistical Comparison between Photospheric Vector Magnetograms Obtained by SDO/HMI and Hinode/SP
- Disintegration of an Eruptive Filament via Interactions with Quasi-Separatrix Layers
- 3-D nonlinear force-free field reconstruction of solar active region 11158 by direct boundary integral equation
- Variations of the 3-D coronal magnetic field associated with the X3.4-class solar flare event of AR 10930
- Where do flare ribbons stop?
- Flare Activity and Magnetic Feature Analysis of the Flare Stars
- Sunstardb: a database for the study of stellar magnetism and the solar-stellar connection