Transverse oscillations of a double-structured solar filament

Jelínek, Petr; Karlický, M.; Smirnova, V. V.; Соловьев, А. А.

doi:10.1051/0004-6361/201936836

Cited by 6 publications

(4 citation statements)

References 25 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In these two cases, however, the two branches possess opposite rather than same signs of helicity, which makes the tilt instability relevant (see Sect. 3.2.3); but without the HFT in between (see also Jelínek et al 2020), the configuration is more stable in this aspect than that originally envisaged in Liu et al (2012a). Double-decker filaments display a wide range of eruptive behavior.…”

Section: Double-decker Structurementioning

confidence: 74%

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

2020

Res. Astron. Astrophys.

View full text Add to dashboard Cite

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.

show abstract

Section: Double-decker Structurementioning

confidence: 74%

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

2020

Res. Astron. Astrophys.

View full text Add to dashboard Cite

show abstract

“…The other configuration, a flux rope atop a sheared arcade, is also found in NLFFF modeling (Régnier & Amari 2004) and inferred from dynamic motions i.e., rotations about the spine and longitudinal oscillations along the spine in a filament disturbed by a flare surge . In these two cases, however, the two branches possess opposite rather than same signs of helicity, which makes the tilt instability relevant (see Section 3.2.3); but without the HFT in between (see also Jelínek et al 2020), the configuration is more stable in this aspect than that originally envisaged in Liu et al (2012a). Double-decker filaments display a wide range of eruptive behavior.…”

Section: Double-decker Structurementioning

confidence: 95%

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

Liu

2020

Preprint

View full text Add to dashboard Cite

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

“…When an EUV jet from a remote AR arrives and collides with a filament, transverse oscillation of the filament may be generated (Zhang et al 2017b). Sophisticated numerical simulations have shed light on the triggering mechanism, restoring force, and damping mechanism of filament oscillations (e.g., Luna & Karpen 2012;Zhang et al 2013;Zhou et al 2018;Adrover-González & Terradas 2020;Fan 2020;Jelínek et al 2020;Liakh et al 2020). Several damping mechanisms have been proposed to interpret the observed attenuation of filament oscillations, such as thermal effects, resonant absorption in nonuniform media, and partial ionization effects (see Arregui & Ballester 2011, and references therein).…”

Section: Introductionmentioning

confidence: 99%

Simultaneous transverse oscillations of a coronal loop and a filament excited by a circular-ribbon flare

Zhang

2020

A&A

View full text Add to dashboard Cite

Aims. The aim of this study is to investigate the excitation of kink oscillations in coronal loops and filaments, by analyzing a C3.4 circular-ribbon flare associated with a blowout jet in active region 12434 on 2015 October 16. Methods. The flare was observed in ultraviolet and extreme-ultraviolet wavelengths by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory (SDO) spacecraft. The line-of-sight (LOS) magnetograms of the photosphere were observed by the Helioseismic and Magnetic Imager on board SDO. Soft X-ray fluxes of the flares in 0.5−4 and 1−8 Å were recorded by the GOES spacecraft. Results. The flare excited small-amplitude kink oscillation of a remote coronal loop. The oscillation lasted for ≥4 cycles without significant damping. The amplitude and period are 0.3 ± 0.1 Mm and 207 ± 12 s. Interestingly, the flare also excited transverse oscillation of a remote filament. The oscillation lasted for ∼3.5 cycles with decaying amplitudes. The initial amplitude is 1.7−2.2 Mm. The period and damping time are 437−475 s and 1142−1600 s. The starting times of simultaneous oscillations of coronal loop and filament were concurrent with the hard X-ray peak time. Though small in size and short in lifetime, the flare set off a chain reaction. It generated a bright secondary flare ribbon (SFR) in the chromosphere, remote brightening (RB) that was cospatial with the filament, and intermittent, jet-like flow propagating in the northeast direction. Conclusions. The loop oscillation is most probably excited by the flare-induced blast wave at a speed of ≥1300 km s−1. The excitation of the filament oscillation is more complicated. The blast wave triggers secondary magnetic reconnection far from the main flare, which not only heats the local plasma to higher temperatures (SFR and RB), but produces jet-like flow (i.e., reconnection outflow) as well. The filament is disturbed by the secondary magnetic reconnection and experiences transverse oscillation. These findings provide new insight into the excitation of transverse oscillations of coronal loops and filaments.

show abstract

Transverse oscillations of a double-structured solar filament

Cited by 6 publications

References 25 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

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

Simultaneous transverse oscillations of a coronal loop and a filament excited by a circular-ribbon flare

Contact Info

Product

Resources

About