Comparison of Kinematics of Solar Eruptive Prominences and Spatial Distribution of the Magnetic Decay Index

Myshyakov, I. I.; Tsvetkov, Ts.

doi:10.3847/1538-4357/ab6334

Cited by 8 publications

(5 citation statements)

References 37 publications

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“…In a datadriven MHD simulation, Guo et al (2019a) computed the decay index along the eruption path of a flux rope, and found that the rope starts to rise rapidly at the same height as the decay index crosses the canonical critical value of 1.5. Similarly, recent studies on the heighttime profiles of eruptive filaments (Vasantharaju et al 2019;Zou et al 2019b;Myshyakov & Tsvetkov 2020;Cheng et al 2020) and of hot channels (Cheng et al 2020) generally concluded that the decay index at the height where the slow rise transitions to fast rise is close to the threshold of the torus instability.…”

Section: Torus Instabilitymentioning

confidence: 83%

Magnetic flux ropes in the solar corona: structure and evolution toward eruption

2020

Res. Astron. Astrophys.

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Magnetic flux ropes are characterized by coherently twisted magnetic field lines, which are ubiquitous in magnetized plasmas. As the core structure of various eruptive phenomena in the solar atmosphere, flux ropes hold the key to understanding the physical mechanisms of solar eruptions, which impact the heliosphere and planetary atmospheres. The strongést disturbances in the Earth’s space environments are often associated with large-scale flux ropes from the Sun colliding with the Earth’s magnetosphere, leading to adverse, sometimes catastrophic, space-weather effects. However, it remains elusive as to how a flux rope forms and evolves toward eruption, and how it is structured and embedded in the ambient field. The present paper addresses these important questions by reviewing current understandings of coronal flux ropes from an observer’s perspective, with an emphasis on their structures and nascent evolution toward solar eruptions, as achieved by combining observations of both remote sensing and in-situ detection with modeling and simulation. This paper highlights an initiation mechanism for coronal mass ejections (CMEs) in which plasmoids in current sheets coalesce into a ‘seed’ flux rope whose subsequent evolution into a CME is consistent with the standard model, thereby bridging the gap between microscale and macroscale dynamics.

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Section: Torus Instabilitymentioning

confidence: 83%

Magnetic flux ropes in the solar corona: structure and evolution toward eruption

2020

Res. Astron. Astrophys.

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“…A general method to get the kinematics of ascending filaments is making a slice to track its plane-of-sky (POS) apex and further fitting the trajectory with an exponential-pluspolynomial function (Myshyakov & Tsvetkov 2020;Qiu et al 2020). It is found that the filament eruptions usually comprise a preceding slow-rise phase and a following fast-rise phase.…”

Section: Introductionmentioning

confidence: 99%

Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE

Qiu,

Li,

Guo

et al. 2024

ApJL

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The eruption of solar filaments, also known as prominences appearing off limb, is a common phenomenon in the solar atmosphere. It ejects massive plasma and high-energy particles into interplanetary space, disturbing the solar-terrestrial environment. It is vital to obtain the three-dimensional velocity fields of erupting filaments for space-weather predictions. We derive the three-dimensional kinematics of an off-limb prominence and an on-disk filament, respectively, using the full-disk spectral and imaging data detected by the Chinese Hα Solar Explorer (CHASE). It is found that both the prominence and the filament experience a fast semicircle-shaped expansion at first. The prominence keeps propagating outward with an increasing velocity until escaping successfully, with the south leg of the prominence finally moving back to the Sun in a swirling manner. For the filament, the internal plasma falls back to the Sun in a counterclockwise rotation in the late ejection, matching the failed eruption without a coronal mass ejection. During the eruptions, both the prominence and the filament show material splitting along the line-of-sight direction, revealed by the bimodal Hα spectral profiles. For the prominence, the splitting begins at the top and gradually spreads to almost the whole prominence with a fast blueshift component and a slow redshift component. The material splitting in the filament is more fragmental. As shown by the present results, the CHASE full-disk spectroscopic observations make it possible to systematically study the three-dimensional kinematics of solar filament eruptions.

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“…In a data-driven MHD simulation, Guo et al (2019a) computed the decay index along the eruption path of a flux rope, and found that the rope starts to rise rapidly at the same height as the decay index crosses the canonical critical value of 1.5. Similarly, recent studies on the height-time profiles of eruptive filaments (Vasantharaju et al 2019;Zou et al 2019b;Myshyakov & Tsvetkov 2020;Cheng et al 2020) and of hot channels (Cheng et al 2020) generally concluded that the decay index at the height where the slow rise transitions to fast rise is close to the threshold of the torus instability.…”

Section: Torus Instabilitymentioning

confidence: 84%

Magnetic Flux Ropes in the Solar Corona: Structure and Evolution toward Eruption

Liu

2020

Preprint

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Magnetic flux ropes are characterized by coherently twisted magnetic field lines, which are ubiquitous in magnetized plasmas. As the core structure of various eruptive phenomena in the solar atmosphere, flux ropes hold the key to understanding the physical mechanisms of solar eruptions, which impact the heliosphere and planetary atmospheres. Strongest disturbances in the Earth's space environments are often associated with largescale flux ropes from the Sun colliding with the Earth's magnetosphere, leading to adverse, sometimes catastrophic, space-weather effects. However, it remains elusive as to how a flux rope forms and evolves toward eruption, and how it is structured and embedded in the ambient field. The present paper addresses these important questions by reviewing current understandings of coronal flux ropes from an observer's perspective, with emphasis on their structures and nascent evolution toward solar eruptions, as achieved by combining observations of both remote sensing and in-situ detection with modeling and simulation. It highlights an initiation mechanism for coronal mass ejections (CMEs) in which plasmoids in current sheets coalesce into a 'seed' flux rope whose subsequent evolution into a CME is consistent with the standard model, thereby bridging the gap between microscale and macroscale dynamics.

show abstract

Comparison of Kinematics of Solar Eruptive Prominences and Spatial Distribution of the Magnetic Decay Index

Cited by 8 publications

References 37 publications

Magnetic flux ropes in the solar corona: structure and evolution toward eruption

Magnetic flux ropes in the solar corona: structure and evolution toward eruption

Three-dimensional Velocity Fields of the Solar Filament Eruptions Detected by CHASE

Magnetic Flux Ropes in the Solar Corona: Structure and Evolution toward Eruption

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