Structural evolution of a magnetic flux rope associated with a major flare in the solar active region 12205

Duan, Aiying; Jiang, Chaowei; Guo, Yilin; Feng, Xueshang; Cui, Jun

doi:10.1051/0004-6361/202142061

Cited by 5 publications

(2 citation statements)

References 97 publications

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“…No signature common to earlier twisted flux emergence simulations (e.g., Fan 2001;Magara & Longcope 2001;Manchester et al 2004;Archontis & Török 2008) can be identified. In addition, we cannot find any large-scale twisting motion (as modeled in Török & Kliem 2003;Aulanier et al 2005b;Jiang et al 2021), nor any systematic and well-aligned series of converging motions and photospheric flux cancellations (e.g., van Ballegooijen & Martens 1989;Forbes & Priest 1995;Aulanier et al 2010;Amari et al 2011;Zuccarello et al 2015;Duan et al 2022). Therefore, despite the pre-reconnecting lines organizing into the aforementioned arcade and flux rope at the onset of reconnection (Figures 7d and 7e), they do not begin as these coherent structures beforehand (Figures 7a-7c).…”

Section: Deviations From Previous Studiesmentioning

confidence: 71%

From incoherent field to coherent reconnection

Robinson

Carlsson

Aulanier

2022

A&A

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Context. Magnetic reconnection in the quiet Sun is a phenomenon that is consistently observed, however, its conditions of occurrence are not as well known as for more energetic events. It has recently become feasible to address this issue with 3D numerical simulations of realistically stratified and convection-driven reconnection. Aims. We aim to illustrate ways by which quiet Sun fields may contribute to solar atmospheric heating via magnetic reconnection that is driven by convective motion. We also aim to compare our complex stratified model to earlier idealized coronal models in terms of reconnection drivers and topological conditions. Methods. We analyzed a simulation of the quiet Sun in which a complex coronal magnetic field is self-consistently driven by the underlying convection. We employed a selection of Lagrangian markers to trace the spatiotemporal behavior of specific magnetic features that are relevant to magnetic reconnection and atmospheric heating. Results. A relatively large-scale reconnection-driven heating event occurs in the simulated corona, in a flattened X-shaped feature characterized by a weak field and high current. It is reminiscent of a hyperbolic flux tube (HFT), which is located at the interface between multiple flux systems. One of these is a smooth overlying horizontal field and the two most relevant others are located below the HFT. They consist of an arcade and a horizontal flux rope which eventually reconnect with the overlying field, raising coronal plasma temperatures up to 1.47 MK. Conclusions. We have identified a reconnection-driven coronal heating event in a quiet Sun simulation. We find that our results are in good phenomenological agreement with idealized coronal flare models, which demonstrates that the same general physical concepts are valid. However, we also find that the reconnecting flux rope and arcade are neither formed by any obvious coherent flux emergence, nor by any ordered photospheric motion or flux cancellation. Instead, they seem to develop merely from the selfconsistent convective driving of pre-existing tangled field lines. This gradual and smooth ordering suggests an inverse cascade of magnetic helicity via smaller reconnection events, located at or above slowly-moving photospheric flux concentrations. We suggest that this case is representative of many heating events that may be ubiquitous in the real quiet Sun.

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Section: Deviations From Previous Studiesmentioning

confidence: 71%

From incoherent field to coherent reconnection

Robinson

Carlsson

Aulanier

2022

A&A

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“…the integral follows the path of a magnetic field line from one footpoint to the other. Following [30], we estimate the averaged twist number corresponding to the MFR volume with |T w | 1 and found the maximum values of averaged twist number to be 1.98 and 2 for the MHD and HMMD cases, respectively. Previous studies regarding the threshold value for kink-instability (see [30] and the references therein) suggest that if the averaged twist number ranges between 1.5 to 2.5, the MFR is stable against kink.…”

Section: Simulation Resultsmentioning

confidence: 99%

Hall effect on the magnetic reconnections during the evolution of a three-dimensional magnetic flux rope

et al. 2023

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We present a novel Hall magnetohydrodynamics (HMHD) numerical simulation of a three-dimensional (3D) magnetic flux rope (MFR)---generated by magnetic reconnections from an initial 3D bipolar sheared field. Magnetic reconnections during the HMHD evolution are compared with the MHD. In both simulations, the MFRs generate as a consequence of the magnetic reconnection at null points which has not been realized in contemporary simulations. Interestingly, the evolution is faster and more intricate in the HMHD simulation. Repetitive development of the twisted magnetic field lines (MFL) in the vicinity of 3D nulls (reconnection site) is unique to the HMHD evolution of the MFR. The dynamical evolution of magnetic field lines around the reconnection site being affected by the Hall forcing, correspondingly affects the large-scale structures.

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Initiation mechanism of the first on-disk X-class flare of solar cycle 25

Duan¹,

Jiang²,

Zhou³

et al. 2023

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In this paper we study the initiation mechanism of the first on-disk X-class eruptive flare in solar cycle 25. Coronal magnetic field reconstructions reveal a magnetic flux rope (MFR) whose configuration is highly consistent with a filament existing for a long period before the flare; the eruption of the whole filament indicates that the MFR erupted during the flare. However, quantitative analysis shows that the pre-flare MFR resides too low to trigger a torus instability (TI). The filament experienced a slow rise before the flare onset, for which we estimated evolution of the filament height using a triangulation method by combining the SDO and STEREO observations, and find it is also much lower than the critical height for triggering TI. On the other hand, the pre-flare evolution of the current density shows progressive thinning of a vertical current layer on top of the flare polarity inversion line (PIL), which suggests that a vertical current sheet forms before the eruption. Meanwhile, there is continuous shearing motion along the PIL under the main branch of the filament, which can drive the coronal field to form such a current sheet. We thus suggest that the event follows a reconnection-based initiation mechanism as recently established using a high-accuracy magnetohydrodynamics simulation, in which an eruption is initiated by reconnection in a current sheet that forms gradually within a continuously sheared magnetic arcade. The eruption should be further driven by TI as the filament quickly rises into the TI domain during the eruption.

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Structural evolution of a magnetic flux rope associated with a major flare in the solar active region 12205

Cited by 5 publications

References 97 publications

From incoherent field to coherent reconnection

From incoherent field to coherent reconnection

Hall effect on the magnetic reconnections during the evolution of a three-dimensional magnetic flux rope

Initiation mechanism of the first on-disk X-class flare of solar cycle 25

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