A (The?) 3D standard model for eruptive flares

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Introduction

Eruptive flares, associated with coronal mass ejections, are important energetic events taking place in the solar corona. The intense magnetic energy release originates from magnetic reconnection, which is also responsible for newly formed magnetic structures that are ejected as CMEs. Solar corona observations reveal typical 3D magnetic structures during eruptive flares: flux ropes (twisted magnetic field lines structures), ultimately ejected in the interplanetary medium, and hot and dense flare loops. Magnetic reconnection takes place in regions of drastic changes in the magnetic connectivity: these are separatrices, defining different domains of connectivity, or quasi-separatrix layers (QSLs) that generalize in 3D regions of strong connectivity gradients.

With a MHD numerical simulation recreating the evolution of a flux rope expansion during an eruptive flare [Ref. 1], we propose a 3D-extended, more complete version of the standard model for eruptive flares. We present below new understandings offered by this model.

New elements of the 3D standard model

The 3D standard model cartoon is depicted in Figure 1, and shows the evolution of reconnecting magnetic field lines and associated current/flare ribbons. This cartoon summarizes several processes deduced from the comparisons between the 3D MHD simulation and the observations, listed as follows.

Figure 1: Cartoon of the 3D standard model for eruptive flares, showing four pre- and post-reconnected field lines. The pre-eruptive arcades undergo slipping reconnection and form flare loops (green and yellow lines) and the twisted envelope of the flux rope (blue and orange lines). The grey area represents parts of the 3D volume of the current layer and the QSL (restricted to strong currents location below the flux rope), while the J-shape red structures are their photospheric footprints.

Flare Loops

Observations of the formation and the evolution of flare loops usually show a strong-to-weak shear evolution (see Figure 2). This transition comes from the reconnection-driven transfer of the differential magnetic shear, from the pre- to the post-eruptive configuration (green and yellow lines in the cartoon), and also from the vertical straightening of the inner legs of the flux rope, which induces an outer shear weakening [Ref. 1].

Figure 2: Strong-to-weak shear evolution for post-flare loops, as seen in STEREO/EUVI observations (top) and as reproduced with the MHD simulation of an unstable flux rope (bottom).

The flux rope

A torus-unstable flux rope core (dashed purple lines in Figure 1), created by photospheric shearing motions/magnetic diffusion, can trigger eruptive flares [Ref. 2]. As field lines undergo reconnection, the flux rope is continuously fed by newly reconnected field lines (blue/green lines, Figure 3). These field lines create the outer envelope of the flux rope and lead to the continuous growth of the expanding flux rope.

Slipping reconnection

Slipping motion of field lines occurs naturally as a result of successive connectivity changes, and takes place in strong current density region where the magnetic field is strongly distorted (see Ref. 3). Both flare loop arcades and the erupting flux rope undergo slipping reconnection during their formation/evolution process. This intrinsic reconnection regime has recently been observed during an eruptive flare [Ref.4].

Figure 3: uild-up of the flux rope envelope during the flare, as reproduced with a 3D MHD simulation. As time passes by, newly field lines reconnecting at different times (blue and green lines) wrap around the torus-unstable flux rope core (pink lines).

Figure 4: (top) Apparent slipping motion of field lines and associated kernels during the SOL2012-12-07 flare, (bottom) Slipping mechanism for field lines building up the flux rope in the 3D MHD simulation.

Current / flare ribbons

Photospheric currents are the footprints of the coronal current layer. They are located in the same regions as the flare ribbons and the photospheric footprints of the 3D QSL volume [Ref. 5]. As time goes by, current ribbons move away from each other, while field lines being swiped by the coronal current layer further reconnect. During the impulsive flare phase, the currents are seen to increase in the very localized ribbons, due to the collapse of the coronal current sheet.

Figure 5: Evolution of the flare ribbons (left), and current ribbons (middle) during the SOL2011-02-15 X-class flare, and in the 3D MHD simulation (right). As time passes by, the straight parts of the J-shape ribbons move away from each other, while the hook becomes rounder as a result of a growing flux rope envelope. The currents increase during the impulsive phase of the flare in the localized ribbon region.

Conclusion

Our 3D standard model, built from a 3D MHD simulation and which cartoon is presented in Figure 1, extends our understanding of the observational characteristics, as well as the underlying physical mechanisms of eruptive flares. This model shows that both flare loops and flux rope are constructed by 3D reconnection, in the thin coronal current layer that maps as J-shaped current/flare ribbons onto the photosphere. Field lines entering this region reconnect successively, leading to an apparent slipping motion, as recently seen in coronal observations. This change of connectivity allows shear transfer from dynamically evolving pre- to post- reconnected field lines, and is often observed as a strong-to-weak shear transfer in flare loops observations. The flux rope, on the other hand, is constantly growing as reconnected twisted field lines construct its outer shell.

References

[1] G. Aulanier, M. Janvier and B. Schmieder, , Astronomy and Astrophysics, 543, A110 (2012) link "The standard model in three dimensions. I. Strong-to-weak shear transition in post-flare loops"

[2] G. Aulanier, T. Török, P. Démoulin and E. E. DeLuca, "Formation of torus-unstable flux ropes and electric currents in erupting sigmoids", 708, 314 (2010)

[3] M. Janvier, G. Aulanier, E. Pariat and P. Démoulin, "The standard model in three dimensions. III. Slip-running reconnection properties", Astronomy and Astrophysics, 555, A77 (2013)

[4] J. Dudìk et al., link title

[5]