Pre-eruptive Magnetic Reconnection within a Multi-flux-rope System in the Solar Corona

Awasthi, Arun Kumar; Liu, Rui; Wang, Haimin; Wang, Yuming; Shen, Chenglong

doi:10.3847/1538-4357/aab7fb

Cited by 49 publications

(68 citation statements)

References 54 publications

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“…Hence, the geoeffectiveness of a CME arriving at Earth depends very much on the orientation and helicity of its magnetic structure (e.g., Yurchyshyn et al 2001;Awasthi et al 2018) .…”

Section: Introductionmentioning

confidence: 99%

The Relationship between Chirality, Sense of Rotation, and Hemispheric Preference of Solar Eruptive Filaments

Zhou

Cheng

et al. 2020

ApJ

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The orientation, chirality, and dynamics of solar eruptive filaments is a key to understanding the magnetic field of coronal mass ejections (CMEs) and therefore to predicting the geoeffectiveness of CMEs arriving at Earth. However, confusion and contention remain over the relationship between the filament chirality, magnetic helicity, and sense of rotation during eruption. To resolve the ambiguity in observations, in this paper, we used stereoscopic observations to determine the rotation direction of filament apex and the method proposed by Chen et al. (2014) to determine the filament chirality. Our sample of 12 eruptive active-region filaments establishes a strong one-to-one relationship, i.e., during the eruption, sinistral/dextral filaments (located in the southern/northern hemisphere) rotate clockwise/counterclockwise when viewed from above, and corroborates a weak hemispheric preference, i.e., a filament and related sigmoid both exhibit a forward (reverse) S shape in the southern (northern) hemisphere, which suggests that the sigmoidal filament is associated with a low-lying magnetic flux rope with its axis dipped in the middle. As a result of rotation, the projected S shape of a filament is anticipated to be reversed during eruption.

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“…Hence, the geoeffectiveness of a CME arriving at Earth depends very much on the orientation and helicity of its magnetic structure (e.g., Yurchyshyn et al 2001;Awasthi et al 2018) .…”

Section: Introductionmentioning

confidence: 99%

The Relationship between Chirality, Sense of Rotation, and Hemispheric Preference of Solar Eruptive Filaments

Zhou

Cheng

et al. 2020

ApJ

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“…Its pre-eruptive structure consists of multiple-braided flux ropes with different degrees of coherency, and the individual flux-rope branches manifest reconnection with each other. Awasthi et al (2018) excluded that the complex ICME can result from the merging of successive CMEs and the spacecraft they used only made a glancing encounter with Earth-directed CME. Awasthi et al (2018) considered that a non-MC event inherently disrupts magnetic fields.…”

Section: Introductionmentioning

confidence: 99%

“…Awasthi et al (2018) excluded that the complex ICME can result from the merging of successive CMEs and the spacecraft they used only made a glancing encounter with Earth-directed CME. Awasthi et al (2018) considered that a non-MC event inherently disrupts magnetic fields.…”

Section: Introductionmentioning

confidence: 99%

Comparison of counterstreaming suprathermal electron signatures of ICMEs with and without magnetic cloud: are all ICMEs flux ropes?

Wang

Zhao

Feng

et al. 2019

A&A

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Context. Magnetic clouds (MCs), as large-scale interplanetary magnetic flux ropes, are usually still connected to the sun at both ends near 1 AU. Many researchers believe that all non-MC interplanetary coronal mass ejections (ICMEs) also have magnetic flux rope structures, which are inconspicuous because the observing spacecraft crosses the flanks of the rope structures. If so, the field lines of non-MC ICMEs should also be usually connected to the Sun on both ends. Aims. Then we want to know whether the field lines of most non-MC ICMEs are still connected to the sun at both ends or not. Methods. This study examined the counterstreaming suprathermal electron (CSE) signatures of 266 ICMEs observed by the Advanced Composition Explorer (ACE) spacecraft from 1998 to 2008 and compared the CSE signatures of MCs and non-MC ICMEs.Results. Results show that only 10 of the 101 MC events (9.9% ) and 75 of the 171 non-MC events (43.9%) have no CSEs. Moreover, 21 of the non-MC ICMEs have high CSE percentages (more than 70%) and show relatively stable magnetic field components with slight rotations, which are in line with the expectations that spacecraft passes through the flank of magnetic flux ropes. So the 21 events may be magnetic flux ropes but the ACE spacecraft passes through their flanks of magnetic flux ropes. Conclusions.Considering that most other non-MC events have disordered magnetic fields, we suggest that some non-MC ICMEs inherently have disordered magnetic fields, namely have no magnetic flux rope structures.

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“…The way forward will be to exploit all models in some data-driven way. As a promising example, NLFFF modeling of the source region of a complex CME [4], not fully fitting the single flux rope scenario when observed further out in the heliosphere, found evidence for a multi-flux-rope system acting as its source region, characterized by reconnection and plasma flaring. A challenge for future (multi-scale) modeling efforts, is to use such NLFFF quantifications of multi-rope systems as initial conditions for full MHD evolutions.…”

Section: Discussionmentioning

confidence: 99%

Ideal MHD instabilities for coronal mass ejections: interacting current channels and particle acceleration

Keppens¹,

Guo²,

Makwana³

et al. 2019

Rev. Mod. Plasma Phys.

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We review and discuss insights on ideal magnetohydrodynamic (MHD) instabilities that can play a role in destabilizing solar coronal flux rope structures. For single flux ropes, failed or actual eruptions may result from internal or external kink evolutions, or from torus unstable configurations. We highlight recent findings from 3D magnetic field reconstructions and simulations where kink and torus instabilities play a prominent role.For interacting current systems, we critically discuss different routes to coronal dynamics and global eruptions, due to current channel coalescence or to tilt-kink scenarios. These scenarios involve the presence of two nearby current channels and are clearly distinct from the popular kink or torus instability. Since the solar corona is pervaded with myriads of magnetic loops -creating 2 Rony Keppens * et al.interacting flux ropes typified by parallel or antiparallel current channels as exemplified in various recent observational studies -coalescence or tilt-kink evolutions must be very common for destabilizing adjacent flux rope systems. Since they also evolve on ideal MHD timescales, they may well drive many sympathetic eruptions witnessed in the solar corona. Moreover, they necessarily lead to thin current sheets that are liable to reconnection. We review findings from 2D and 3D MHD simulations for tilt and coalescence evolutions, as well as on particle acceleration aspects derived from computed charged particle motions in tilt-kink disruptions and coalescing flux ropes. The latter were recently studied in two-way coupled kinetic-fluid models, where the complete phase-space information of reconnection is incorporated.

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Pre-eruptive Magnetic Reconnection within a Multi-flux-rope System in the Solar Corona

Cited by 49 publications

References 54 publications

The Relationship between Chirality, Sense of Rotation, and Hemispheric Preference of Solar Eruptive Filaments

The Relationship between Chirality, Sense of Rotation, and Hemispheric Preference of Solar Eruptive Filaments

Comparison of counterstreaming suprathermal electron signatures of ICMEs with and without magnetic cloud: are all ICMEs flux ropes?

Ideal MHD instabilities for coronal mass ejections: interacting current channels and particle acceleration

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