Evolution of the Toroidal Flux of CME Flux Ropes during Eruption

Xing, C.; Cheng, Xin; Ding, M. D.

doi:10.1016/j.xinn.2020.100059

Cited by 35 publications

(31 citation statements)

References 54 publications

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“…Such an evolution pattern also applies to that of the MFR foot area. This increase-todecrease pattern of toroidal flux reproduces the observed variations of magnetic flux in erupting MFR's foot as identified by flare ribbons and transient coronal dimming [40]. On the other hand, the mean twist number shows a systematic increase to a value close to 3.5 at the end of simulation.…”

Section: Evolution Of Mfr's Toroidal Fluxsupporting

confidence: 80%

“…The footprints of this QSL at the bottom surface, i.e., the photosphere, forms two thin strips of J shape on each side of the main polarity inversion line (PIL), and the legs of the MFR are anchored within the hooked parts of the J-shaped strips. Thus, the observed flare ribbons usually exhibit double-J pattern, and the transient coronal holes [37], i.e., post-eruptive twin coronal dimmings, are naturally suggested to map the feet of erupting MFRs, along which mass leakage into interplanetary space could take place [38][39][40], and the boundaries of such twin coronal dimmings are outlined by the hooks of flare ribbons. With the ongoing of reconnection, the arms of the double-J ribbons separate, and their hooks gradually extends outwards.…”

Section: Introductionmentioning

confidence: 99%

“…It is predicted by theoretical models [35] that if the MFR grows to sufficiently twisted, the hooks of the double-J shaped footprints of the QSL can indeed close onto themselves, becoming two closed rings, although this is not reproduced by the numerical model of [20], possibly because their simulation run is stopped before the MFR grows to such a high degree of twist. Very recently, a few papers reported that there is a systematic decrease of the toroidal flux of erupting MFR after its fast increase (e.g., [40,42,43]). In particular, Xing et al [40] developed a practical method for estimation of the toroidal flux of MFR during eruption by combining twin coronal dimmings and the hooks of flare ribbons.…”

Section: Introductionmentioning

confidence: 99%

“…Very recently, a few papers reported that there is a systematic decrease of the toroidal flux of erupting MFR after its fast increase (e.g., [40,42,43]). In particular, Xing et al [40] developed a practical method for estimation of the toroidal flux of MFR during eruption by combining twin coronal dimmings and the hooks of flare ribbons. They found that the toroidal flux of the CME flux rope for all four studied events shows a two-phase evolution: a rapid increasing phase followed by a decreasing phase, and moreover, the evolution is well synchronous in time with that of the flare soft X-ray flux.…”

Section: Introductionmentioning

confidence: 99%

“…The increase of MFR's toroidal flux can be easily understood by the aa-rf reconnection while the subsequent decrease remains unclear. Although Xing et al [40] invoked the rr-rf reconnection as the mechanism responsible for such decrease, it is still unknown whether the increase-to-decrease evolution of toroidal flux can self-consistently be reproduced in any MHD simulation.…”

Section: Introductionmentioning

confidence: 99%

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Formation of Magnetic Flux Rope During Solar Eruption. I. Evolution of Toroidal Flux and Reconnection Flux

et al. 2021

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Magnetic flux ropes (MFRs) constitute the core structure of coronal mass ejections (CMEs), but hot debates remain on whether the MFR forms before or during solar eruptions. Furthermore, how flare reconnection shapes the erupting MFR is still elusive in three dimensions. Here we studied a new MHD simulation of CME initiation by tether-cutting magnetic reconnection in a single magnetic arcade. The simulation follows the whole life, including the birth and subsequent evolution, of an MFR during eruption. In the early phase, the MFR is partially separated from its ambient field by a magnetic quasi-separatrix layer (QSL) that has a double-J shaped footprint on the bottom surface. With the ongoing of the reconnection, the arms of the two J-shaped footprints continually separate from each other, and the hooks of the J shaped footprints expand and eventually become closed almost at the eruption peak time, and thereafter the MFR is fully separated from the un-reconnected field by the QSL. We further studied the evolution of the toroidal flux in the MFR and compared it with that of the reconnected flux. Our simulation reproduced an evolution pattern of increase-to-decrease of the toroidal flux, which is reported recently in observations of variations in flare ribbons and transient coronal dimming. The increase of toroidal flux is owing to the flare reconnection in the early phase that transforms the sheared arcade to twisted field lines, while its decrease is a result of reconnection between field lines in the interior of the MFR in the later phase.

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Section: Evolution Of Mfr's Toroidal Fluxsupporting

confidence: 80%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Formation of Magnetic Flux Rope During Solar Eruption. I. Evolution of Toroidal Flux and Reconnection Flux

et al. 2021

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Upflows in the Upper Solar Atmosphere

et al. 2021

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Spectroscopic observations at extreme-and far-ultraviolet wavelengths have revealed systematic upflows in the solar transition region and corona. These upflows are best seen in the network structures of the quiet Sun and coronal holes, boundaries of active regions, and dimming regions associated with coronal mass ejections. They have been intensively studied in the past two decades because they are likely to be closely related to the formation of the solar wind and heating of the upper solar atmosphere. We present an overview of the characteristics of these upflows, introduce their possible formation mechanisms, and discuss their potential roles in the mass and energy transport in the solar atmosphere. Although past investigations have greatly improved our understanding of these upflows, they have left us with several outstanding questions and unresolved issues that should be addressed in the future. New observations from the Solar Orbiter mission, the Daniel K. Inouye Solar Telescope and the Parker Solar Probe will likely provide critical information to advance our understanding of the generation, propagation, and energization of these upflows.

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