Data-driven magnetohydrodynamic modelling of a flux-emerging active region leading to solar eruption

Jiang, Chaowei; Wu, S. T.; Feng, Xiaoying; Hu, Qiang

doi:10.1038/ncomms11522

Cited by 160 publications

(144 citation statements)

References 75 publications

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“…These semi-realistic simulations vary widely in complexity, depending on the physics included, the phases of the CME/ICME evolution modeled, and the extent of observational constraints and real data included. Many models use observed magnetograms as boundary condition for the magnetic field at the lower boundary, and recently observed surface flows have been included as well (Jiang et al 2016). Some simulations restrict the calculation to the evolution in the corona (e.g., Zuccarello et al 2012b;Amari et al 2014;Fan 2016), while others model the propagation of the ejecta to 1 AU but do not include the coronal evolution.…”

Section: Modeling Cmes From Sun To Earth: the Bastille Day Eventmentioning

confidence: 99%

The Physical Processes of CME/ICME Evolution

et al. 2017

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As observed in Thomson-scattered white light, coronal mass ejections (CMEs) are manifest as large-scale expulsions of plasma magnetically driven from the corona in the most energetic eruptions from the Sun. It remains a tantalizing mystery as to how these erupting magnetic fields evolve to form the complex structures we observe in the solar wind at Earth. Here, we strive to provide a fresh perspective on the post-eruption and interplanetary evolution of CMEs, focusing on the physical processes that define the many complex interactions of the ejected plasma with its surroundings as it departs the corona and propagates through the heliosphere. We summarize the ways CMEs and their interplanetary CMEs (ICMEs) are rotated, reconfigured, deformed, deflected, decelerated and disguised during their journey through the solar wind. This study then leads to consideration of how structures originating in coronal eruptions can be connected to their far removed interplanetary counterparts. Given that ICMEs are the drivers of most geomagnetic storms (and the sole driver of extreme storms), this work provides a guide to the processes that must be considered in making space weather forecasts from remote observations of the corona.

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Section: Modeling Cmes From Sun To Earth: the Bastille Day Eventmentioning

confidence: 99%

The Physical Processes of CME/ICME Evolution

et al. 2017

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“…One way to produce equilibrium FR configurations is by mimicking the slow formation of pre-eruptive FRs using a boundary-driven MHD evolution (e.g., Lionello et al 2002;Bisi et al 2010;Zuccarello et al 2012;Jiang et al 2016). This requires the development of photospheric boundary conditions that will lead to the formation of an FR, subject to the constraints of the observed photospheric field.…”

Section: Introductionmentioning

confidence: 99%

Regularized Biot–Savart Laws for Modeling Magnetic Flux Ropes

Titov

Downs

Mikić

et al. 2018

ApJL

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Many existing models assume that magnetic flux ropes play a key role in solar flares and coronal mass ejections (CMEs). It is therefore important to develop efficient methods for constructing fluxrope configurations constrained by observed magnetic data and the morphology of the pre-eruptive source region. For this purpose, we have derived and implemented a compact analytical form that represents the magnetic field of a thin flux rope with an axis of arbitrary shape and circular crosssections. This form implies that the flux rope carries axial current I and axial flux F , so that the respective magnetic field is the curl of the sum of axial and azimuthal vector potentials proportional to I and F , respectively. We expressed the vector potentials in terms of modified Biot-Savart laws whose kernels are regularized at the axis in such a way that, when the axis is straight, these laws define a cylindrical force-free flux rope with a parabolic profile for the axial current density. For the cases we have studied so far, we determined the shape of the rope axis by following the polarity inversion line of the eruptions' source region, using observed magnetograms. The height variation along the axis and other flux-rope parameters are estimated by means of potential field extrapolations. Using this heuristic approach, we were able to construct pre-eruption configurations for the 2009 February 13 and 2011 October 1 CME events. These applications demonstrate the flexibility and efficiency of our new method for energizing pre-eruptive configurations in simulations of CMEs.

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“…Kumar et al (2017) found that the reconnection between the cool Hα loops in the chromosphere during the flares can form an unstable flux rope using highresolution observations from the 1.6 m New Solar Telescope (NST) at BBSO. Some indirect evidence of the existence of flux ropes can be deduced by using a nonlinear force-free field (NLFFF) extrapolation (Cheng et al 2010;Jiang et al 2014Jiang et al , 2016aJiang et al , 2016b.…”

Section: Introductionmentioning

confidence: 99%

The Eruption of a Small-scale Emerging Flux Rope as the Driver of an M-class Flare and of a Coronal Mass Ejection

Yan

Jiang

Xue

et al. 2017

ApJ

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Solar flares and coronal mass ejections are the most powerful explosions in the Sun. They are major sources of potentially destructive space weather conditions. However, the possible causes of their initiation remain controversial. Using high-resolution data observed by the New Solar Telescope of Big Bear Solar Observaotry, supplemented by Solar Dynamics Observatory observations, we present unusual observations of a small-scale emerging flux rope near a large sunspot, whose eruption produced an M-class flare and a coronal mass ejection. The presence of the small-scale flux rope was indicated by static nonlinear force-free field extrapolation as well as data-driven magnetohydrodynamics modeling of the dynamic evolution of the coronal three-dimensional magnetic field. During the emergence of the flux rope, rotation of satellite sunspots at the footpoints of the flux rope was observed. Meanwhile, the Lorentz force, magnetic energy, vertical current, and transverse fields were increasing during this phase. The free energy from the magnetic flux emergence and twisting magnetic fields is sufficient to power the M-class flare. These observations present, for the first time, the complete process, from the emergence of the small-scale flux rope, to the production of solar eruptions.

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Data-driven magnetohydrodynamic modelling of a flux-emerging active region leading to solar eruption

Cited by 160 publications

References 75 publications

The Physical Processes of CME/ICME Evolution

The Physical Processes of CME/ICME Evolution

Regularized Biot–Savart Laws for Modeling Magnetic Flux Ropes

The Eruption of a Small-scale Emerging Flux Rope as the Driver of an M-class Flare and of a Coronal Mass Ejection

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