Magnetohydrodynamic Modeling of a Solar Eruption Associated with an X9.3 Flare Observed in the Active Region 12673

Inoue, Satoshi; Shiota, Daikou; Bamba, Yumi; Park, Sung-Hong

doi:10.3847/1538-4357/aae079

Cited by 56 publications

(72 citation statements)

References 68 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We suggest that the recent 3D data driven studies of eruptive phenomena, based on the initialization of resistive 3D MHD codes with Non-Linear Force Free Extrapolations of the observed magnetograms of specific active regions, driven by the turbulent photospheric activity [55,99,113], is clearly closer to reality.…”

Section: Discussionmentioning

confidence: 70%

“…It is important to connect the sketch in Fig. 3 with the evolution of eruptive magnetic Inoue et al [55] performed a magnetohydrodynamic (MHD) simulation in order to reveal the three-dimensional dynamics of the magnetic fields associated with a X9.3 solar flare. They first performed an extrapolation of the 3D magnetic field based on the observed photospheric magnetic field prior to the flare and then used this as the initial condition for the MHD simulation, which revealed a dramatic eruption, see Fig.…”

Section: The Evolution Of Magnetic Topologies and Eruptive Phenomenamentioning

confidence: 99%

See 1 more Smart Citation

Sources of solar energetic particles

Vlahos

Anastasiadis

Papaioannou

et al. 2019

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

Solar Energetic Particles (SEP) are an integral part of the physical processes related with Space Weather. We present a review for the acceleration mechanisms related to the explosive phenomena (flares and/or CMEs) inside the solar corona. For more than 40 years, the main 2D cartoon representing our understanding of the explosive phenomena inside the solar corona remained almost unchanged. The acceleration mechanisms related to solar flares and CMEs also remained unchanged and were part of the same cartoon. In this review, we revise the standard cartoon and present evidence from recent global MHD simulations that supports the argument that explosive phenomena will lead to the spontaneous formation of current sheets in different parts of the erupting magnetic structure. The evolution of the large scale current sheets and their fragmentation will lead to strong turbulence and turbulent reconnection during solar flares and turbulent shocks. In other words, the acceleration mechanism in flares and CME-driven shocks may be the same, and their difference will be the overall magnetic topology, the ambient plasma parameters, and the duration of the unstable driver.

show abstract

Section: Discussionmentioning

confidence: 70%

Section: The Evolution Of Magnetic Topologies and Eruptive Phenomenamentioning

confidence: 99%

Sources of solar energetic particles

Vlahos

Anastasiadis

Papaioannou

et al. 2019

Phil. Trans. R. Soc. A.

View full text Add to dashboard Cite

show abstract

“…These studies thus emphasise the complex evolution of this AR and most of them feature several flux rope systems. In addition, Inoue et al (2018) found, using an MHD simulation initiated by NLFFF reconstruction, that the eruption of these flares initially included several small flux ropes and that magnetic reconnection played an important role. Similarly, Jiang et al (2018) presented a detailed study of the magnetic topology surrounding the X9.3 flare using an NLFFF initiated MHD simulation.…”

Section: Introductionmentioning

confidence: 99%

“…This active region and its eruptions have been the subject of a number of studies (e.g. Yang et al 2017;Chertok et al 2018;Hou et al 2018;Inoue et al 2018;Liu et al 2018;Verma 2018;Yan et al 2018;Morosan et al 2019;Romano et al 2019;Zou et al 2019). During its transit across the solar disc, this AR produced four GOES X-class flares and numerous weaker flares.…”

Section: Introductionmentioning

confidence: 99%

Time-dependent data-driven coronal simulations of AR 12673 from emergence to eruption

Price

Pomoell

Lumme

et al. 2019

A&A

View full text Add to dashboard Cite

Aims. We present a detailed study of the magnetic evolution of AR 12673 using a magnetofrictional modelling approach. Methods. The fully data-driven and time-dependent model was driven with maps of the photospheric electric field, inverted from vector magnetogram observations obtained from the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO). Our analysis was aided by studying the evolution of metrics such as the free magnetic energy and the current-carrying helicity budget of the domain, maps of the squashing factor and twist, and plots of the current density. These allowed us to better understand the dynamic nature of the magnetic topology. Results. Our simulation captured the time-dependent nature of the active region and the erupting flux rope associated with the X-class flares on 6 September 2017, including the largest of solar cycle 24. Additionally, our results suggest a possible threshold for eruptions in the ratio of current-carrying helicity to relative helicity. Conclusion. The flux rope was found to be a combination of two structures that partially combine during the eruption process. Our time-dependent data-driven magnetofrictional model is shown to be capable of generating magnetic fields consistent with extreme ultraviolet (EUV) observations.

show abstract

“…Flare activity was also discovered on the solar-type stars other than the Sun (Schaefer et al 2000;Benz & Güdel 2010;Shibata & Magara 2011;Maehara et al 2012;Notsu et al 2013;Shibayama et al 2013;Balona 2015;Davenport 2016). Solar flares commonly come from solar active regions (ARs), and the magnetic configuration of flare-bearing ARs is one key aspect for understanding the initiation and evolution of solar flares (e.g., Chen et al 2012;Sun et al 2015;Jiang et al 2016Jiang et al , 2018Liu et al 2016;Cheng et al 2017;Guo et al 2017;Hao et al 2017;Inoue et al 2018) and other related eruptive phenomena in the solar atmosphere (e.g., Zhang et al 2012;Ouyang et al 2017;Wang et al 2017;Liu et al 2018). The non-potential property of the magnetic fields with electric current permeating inside is believed to be the critical aspect related to the activity level of ARs (e.g., Wang et al 1996;Leka & Barnes 2003;Schrijver 2016).…”

Section: Introductionmentioning

confidence: 99%

Chirality and magnetic configuration associated with two-ribbon solar flares: AR 10930 versus AR 11158

Wang

Yan

et al. 2020

Advances in Space Research

View full text Add to dashboard Cite

The magnetic configuration of flare-bearing active regions (ARs) is one key aspect for understanding the initiation of solar flares. In this paper, we perform a comparative analysis on the chiral characteristics and the magnetic configurations of two X-class two-ribbon flares happening in AR 10930 and AR 11158, whose photospheric magnetic fields were observed by the Hinode and SDO satellites, respectively. The corresponding coronal magnetic fields were calculated based on the nonlinear forcefree field model. It is found that both the flares were initiated in local areas with extremely strong electric current density. The chirality of the magnetic field (indicated by the sign of force-free factor α) along the main polarity inversion line (PIL) is opposite for the two ARs, that is, left-handed (α < 0) for AR 10930 and right-handed (α > 0) for AR 11158. The analysis shows that, for both flare events, prominent magnetic connectivity (indicated by both high α and strong current distributions) was formed above the main PIL before the flare and was totally broken after the flare eruption. Yet the two branches of broken magnetic connectivity, combined with the isolated electric current at the magnetic connectivity breaking site, compose the opposite magnetic configurations for the two ARs owing to their opposite chiral characteristics. That is, Z-shaped configuration for AR 10930 with negative α and left-handed chirality, and inverse Z-shaped configuration for AR 11158 with positive α and right-handed chirality. We speculate that two-ribbon flares can be generally classified to these two magnetic configurations by chirality (α sign) of ARs.

show abstract

Magnetohydrodynamic Modeling of a Solar Eruption Associated with an X9.3 Flare Observed in the Active Region 12673

Cited by 56 publications

References 68 publications

Sources of solar energetic particles

Sources of solar energetic particles

Time-dependent data-driven coronal simulations of AR 12673 from emergence to eruption

Chirality and magnetic configuration associated with two-ribbon solar flares: AR 10930 versus AR 11158

Contact Info

Product

Resources

About