Data-driven modeling of solar coronal magnetic field evolution and eruptions

Jiang, Chaowei; Feng, Xueshang; Guo, Yang; Hu, Qiang

doi:10.1016/j.xinn.2022.100236

Cited by 32 publications

(28 citation statements)

References 194 publications

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“…Even though so many theoretical models exist, it is not easy to determine which one operates in realistic events since the coronal magnetic fields and their evolutions associated with eruptions are often much more complex than described in the models. In recent years, numerical models that are constrained or directly driven by observed data have been developed and proven to be a powerful tool in probing the mechanisms of realistic solar eruptions (e.g., Inoue et al 2014;Prasad et al 2017;Jiang et al 2018aJiang et al , 2018bGuo et al 2021); the progress has been reviewed by Jiang et al (2022a).…”

Section: Introductionmentioning

confidence: 99%

MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation

Wang

Jiang

Feng

et al. 2022

ApJ

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The relationship between solar eruption and sunspot rotation has been widely reported, and the underlying mechanism needs to be studied. Here we performed a full 3D MHD simulation using a data-constrained approach to study the mechanism of flare eruptions in active region (AR) NOAA 10930, which is characterized by continuous sunspot rotation and homologous eruptions. We reconstructed the potential magnetic field from the magnetogram of Hinode/SOT as the initial condition and drove the MHD system by applying continuous sunspot rotation at the bottom boundary. The key magnetic structure before the major eruptions and the preformed current sheet were derived, which is responsible for the complex MHD evolution with multiple stages. The major eruptions were triggered directly by fast reconnection in the preformed current sheet above the main polarity inversion line between the two major magnetic polarities of the AR. Furthermore, our simulation shows the homologous eruption successfully. It has reasonable consistency with observations in relative strength, energy release, X-ray and Hα features, and time interval of eruptions. In addition, the rotation angle of the sunspot before the first eruption in the simulation is also close to the observed value. Our simulation offers a scenario different from many previous studies based on ideal instabilities of a twisted magnetic flux rope and shows the importance of sunspot rotation and magnetic reconnection in efficiently producing homologous eruptions by continuous energy injection and impulsive energy release in a recurrent way.

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Section: Introductionmentioning

confidence: 99%

MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation

Wang

Jiang

Feng

et al. 2022

ApJ

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“…With continuous rotation, such confined flares might occur multiple times and jointly build up an ideal unstable MFR that eventually erupts, as suggested by recent observations 5 . This will need further investigations with future data-driven MHD simulations 34 .…”

Section: Discussionmentioning

confidence: 99%

“…Here through a comprehensive MHD simulation, with both data-constrained and datadriven approaches 34 , for a realistic event in solar AR NOAA 12158, we show that sunspot rotation can directly produce eruption, but the mechanism is different from any of the aforementioned ones. Our simulation shows that by applying surface rotation flow to the major sunspot, the nonpotentiality of the coronal magnetic field, as measured by the ratio of the total magnetic energy to the corresponding potential field energy, increases monotonically while the kinetic energy keeps a small value, as the MHD system evolves quasi-statically.…”

Section: Introductionmentioning

confidence: 88%

Sunspot Rotation Leading to Coronal Mass Ejection

Jiang

Feng²,

Bian

et al. 2022

Preprint

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The rotation of sunspots around their umbral center has long been considered as an important process in driving coronal mass ejections (CMEs), but the specific mechanism remains unclear. Here with numerical magnetohydrodynamic simulations of both data-inspired and data-driven approaches, we show that the rotation of a large sunspot leads to a CME actually in a way distinct from the conventional view based on ideal instabilities of twisted flux rope. It is found that through the successive rotation of the sunspot the coronal magnetic field is sheared with a vertical current sheet created progressively, and once fast reconnection sets in the current sheet, the eruption is instantly triggered, with a highly twisted flux rope originating from the eruption. The simulations also revealed a slow-rise evolution phase sandwiched between the quasi-static energy-storage phase and the impulsive eruption-acceleration phase, and it enhances building up of the current sheet.

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“…In this section, we briefly describe the utility of STITCH to event modeling of solar eruptions (for reviews see, e.g., Toriumi & Wang 2019;Jiang et al 2022). A full discussion of the topic is beyond the scope of our paper and ambition.…”

Section: Utility For Event Modelingmentioning

confidence: 99%

STITCH: A Subgrid-scale Model for Energy Buildup in the Solar Corona

Dahlin

DeVore

Antiochos

2022

ApJ

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The solar corona routinely exhibits explosive activity, in particular coronal mass ejections and their accompanying eruptive flares, which have global-scale consequences. These events and their smaller counterparts, coronal jets, originate in narrow, sinuous filament channels. The key processes that form and evolve the channels operate on still smaller spatial scales and much longer timescales, culminating in a vast separation of characteristic lengths and times that govern these explosive phenomena. In this article, we describe implementation and tests of an efficient subgrid-scale model for generating eruptive structures in magnetohydrodynamics (MHD) coronal simulations. STITCH—STatistical InjecTion of Condensed Helicity—is a physics-based, reduced representation of helicity condensation: a process wherein small-scale vortical surface convection forms ubiquitous current sheets and pervasive reconnection across the sheets mediates an inverse cascade of magnetic helicity and free energy, thereby forming the filament channels. We have developed a formalism, STITCH, that abstracts these complex processes into a single term in Ohm’s law and the induction equation that directly injects tangential magnetic flux into the low corona. We show that our approach is in very good agreement with a full helicity condensation calculation that treats all of the dynamics explicitly, while enabling substantial reductions in temporal duration and spatial resolution. In addition, we illustrate the flexibility of STITCH at forming localized filament channels and at energizing complex surface flux distributions that have sinuous boundaries. STITCH is simple to implement and computationally efficient, making it a powerful technique for physics-based modeling of solar eruptive events.

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Data-driven modeling of solar coronal magnetic field evolution and eruptions

Cited by 32 publications

References 194 publications

MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation

MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation

Sunspot Rotation Leading to Coronal Mass Ejection

STITCH: A Subgrid-scale Model for Energy Buildup in the Solar Corona

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