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

Zhang, Q. M.

doi:10.1051/0004-6361/202038557

Cited by 20 publications

(13 citation statements)

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“…A bundle of magnetic field lines are involved in the reconnection process. For the field lines threading the filament, the jet directly hits the filament to oscillate longitudinally, as indicated by observations (Luna et al 2014;Zhang et al 2017;Zhang 2020) and illustrated by numerical simulations in this paper in 1D or in Luna & Moreno-Insertis (2021) in 2D. For the field lines encircling the filament, the jet plasma does not impact the filament material directly.…”

Section: How Filament Decayless Oscillations Are Maintainedmentioning

confidence: 54%

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Ni,

Guo,

Zhang

et al. 2022

Preprint

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Context. As a ubiquitous phenomenon, large-amplitude longitudinal filament oscillations usually decay in 1-4 periods. Recently, we observed a decayless case of such oscillations in the corona. Aims. We try to understand the physical process that maintains the decayless oscillation of the filament. Methods. Multi-wavelength imaging observations and magnetograms are collected to study the dynamics of the filament oscillation and its associated phenomena. To explain the decayless oscillations, we also perform one-dimensional hydrodynamic numerical simulations using the MPI-AMRVAC code. Results. In observations, the filament oscillates decaylessly with a period of 36.4 ± 0.3 min for almost 4 hours before eruption. During oscillations, four quasi-periodic jets emanate from a magnetic cancellation site near the filament. The time interval between neighboring jets is ∼ 68.9 ± 1.0 min. Numerical simulations constrained by the observations reproduced the decayless longitudinal oscillations. However, it is surprising to find that the period of the decayless oscillations is not consistent with the pendulum model. Conclusions. We propose that the decayless longitudinal oscillations of the filament are maintained by quasi-periodic jets, which is verified by the hydrodynamic simulations. More importantly, it is found that, when driven by quasi-periodic jets, the period of the filament longitudinal oscillations depends also on the driving period of the jets, not simply the pendulum period. With a parameter survey in simulations, we derived a formula, by which one can derive the pendulum oscillation period using the observed period of decayless filament oscillations and the driving periods of jets.

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Section: How Filament Decayless Oscillations Are Maintainedmentioning

confidence: 54%

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Ni,

Guo,

Zhang

et al. 2022

Preprint

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“…As mentioned in Section 1, CFs are frequently associated with hot coronal jets observed in EUV wavelengths Zhang & Ni 2019;Zhang 2020;Zhang et al 2021) or cool surges observed in Hα (Wang & Liu 2012;Xu et al 2017). In Figure 1, the C4.2 class flare is accompanied by a blowout jet (Zhang et al 2016a; Dai et al 2021).…”

Section: Relation With Coronal Jetsmentioning

confidence: 93%

“…CFs are usually triggered by filament eruptions (Joshi et al 2015;Xu et al 2017;Yang et al 2020a), which may also generate coronal jets (Wang & Liu 2012;Joshi et al 2018;Zhang et al 2016aZhang et al , 2021Zhang & Ni 2019;Zhang 2020;Dai et al 2021) or drive coronal mass ejections (CMEs; Sun et al 2013;Joshi et al 2015Joshi et al , 2017Liu et al 2019Liu et al , 2020. CFs show similar dynamics to that of two-ribbon flares.…”

Section: Introductionmentioning

confidence: 99%

Statistical analysis of circular-ribbon flares

Zhang,

Song

et al. 2022

Preprint

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Circular-ribbon flares (CFs) are a special type of solar flares owing to their particular magnetic topology. In this paper, we conducted a comprehensive statistical analysis of 134 CFs from 2011 September to 2017 June, including four B-class, 82 C-class, 40 M-class, and eight X-class flares, respectively. The flares were observed by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) spacecraft. The physical properties of CFs are derived, including the location, area (A CF ), equivalent radius (r CF ) assuming a semi-spherical fan dome, lifetime (τ CF ), and peak SXR flux in 1−8 Å. It is found that all CFs are located in active regions, with the latitudes between -30 • and 30 • . The distributions of areas and lifetimes could be fitted with a log-normal function. There is a positive correlation between the lifetime and area. The peak SXR flux in 1−8 Å is well in accord with a power-law distribution with an index of −1.42. For the 134 CFs, 57% of them are accompanied by remote brightenings or ribbons. A positive correlation exists between the total length (L RB ) and average distance (D RB ) of remote brightenings. About 47% and 51% of the 134 CFs are related to type III radio bursts and jets, respectively. The association rates are independent of flare energies. About 38% of CFs are related to mini-filament eruptions, and the association rates increase with flare classes. Only 28% of CFs are related to CMEs, meaning that a majority of them are confined rather than eruptive events. There is a positive correlation between the CME speed and peak SXR flux in 1−8 Å, and faster CMEs tend to be wider.

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“…Phase mixing with anomalously high viscosity is also important in the dissipation of energy during loop oscillations (Ofman & Aschwanden 2002). Small-amplitude, transverse oscillations of coronal loops without significant damping have been noticed (Anfinogentov et al 2013;Nisticò et al 2013;Li et al 2018a;Zhang 2020). The observed loop oscillations in combination with magnetohydrodynamics (MHD) A&A proofs: manuscript no.…”

Section: Introductionmentioning

confidence: 98%

Transverse oscillation of a coronal loop induced by a flare-related jet

Dai,

Zhang,

et al. 2020

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Context. Kink oscillations in coronal loops are ubiquitous, and the observed parameters of oscillations are applied to estimate the magnetic field strength of the loops. Aims. In this work, we report our multiwavelength observations of the transverse oscillation of a large-scale coronal loop with a length of ≥350 Mm. The oscillation was induced by a blowout coronal jet, which was related to a C4.2 circular-ribbon flare (CRF) in AR 12434 on 2015 October 16. We aim to determine the physical parameters in the coronal loop, including the Alfvén speed and magnetic field strength. Methods. The jet-induced kink oscillation was observed in extreme-ultraviolet (EUV) wavelengths by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). Line of sight magnetograms were observed by the Helioseismic and Magnetic Imager (HMI) on board SDO. We took several slices along the loop to assemble time-distance diagrams, and used an exponentially decaying sine function to fit the decaying oscillation. The initial amplitude, period, and damping time of kink oscillation were obtained. Coronal seismology of the kink mode was applied to estimate the Alfvén speed and magnetic field strength in the oscillating loop. In addition, we measured the magnetic field of the loop through non-linear force-free field (NLFFF) modeling using the flux rope insertion method. Results. The oscillation is most pronounced in AIA 171 and 131 Å. The oscillation is almost in phase along the loop with a peak initial amplitude of ∼13.6 Mm, meaning that the oscillation belong to the fast standing kink mode. The oscillation lasts for ∼3.5 cycles with an average period of ∼462 s and average damping time of ∼976 s. The values of τ/P lie in the range of 1.5−2.5. Based on coronal seismology, the Alfvén speed in the oscillating loop is estimated to be ∼1210 km s −1 . Two independent methods are applied to calculate the magnetic field strength of the loop, resulting in 30−43 G using the coronal seismology and 21−23 G using the NLFFF modeling, respectively. Conclusions. The magnetic field strength estimated using two different approaches are in the same order of magnitude, which confirms the reliability of coronal seismology by comparing with the NLFFF modeling.

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

Cited by 20 publications

References 72 publications

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Statistical analysis of circular-ribbon flares

Transverse oscillation of a coronal loop induced by a flare-related jet

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