Extreme-Ultraviolet Wave and Accompanying Loop Oscillations

Devi, Pooja; Chandra, Ramesh; Cristiani, Germán D.; Schmieder, B.; Joshi, Reetika

doi:10.1007/s11207-022-02082-6

Cited by 5 publications

(6 citation statements)

References 111 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The slow-component EUV wave is three times slower than the fast-component EUV wave only when the magnetic field lines are concentric semicircles (Chen et al 2002). It is noted that the recent observational analysis for this event performed by Devi et al (2022) distinguished two components of EUV waves in this event, including the leading fast-mode wave and the following slow nonwave component, verifying the field-line stretching model of EUV waves. Moreover, they found that the ratio between the speeds of these two components ranged from 2.0 to 2.5, which is fairly closer to our simulation result.…”

Section: Relationship Between Cme Fronts and Euv Wavessupporting

confidence: 67%

“…The event we select is the second GOES X-class flare in solar cycle 25, hosted in NOAA active region 12887, occurring around 15:35 UT on 2021 October 28. This event has been reported by other papers, which focused on some observational features, such as observations of EUV waves and the corresponding CME (Devi et al 2022;Hou et al 2022), the CME three-part structure (Devi et al 2022), the eruption mechanism (Yamasaki et al 2022), the Sun-as-a-star spectroscopic characteristics (Xu et al 2022), the solar energetic particles (Li et al 2022), and the geomagnetic effects (Papaioannou et al 2022). It would be of great interest to check in what degree such a geoeffective solar eruption can be reproduced with a data-driven radiative MHD model.…”

Section: Event Overview and Numerical Setupsupporting

confidence: 65%

See 1 more Smart Citation

Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model

Guo

Zhong

et al. 2023

ApJS

Self Cite

View full text Add to dashboard Cite

Solar filament eruptions, flares, and coronal mass ejections (CMEs) are manifestations of drastic releases of energy in the magnetic field, which are related to many eruptive phenomena, from the Earth’s magnetosphere to black hole accretion disks. With the availability of high-resolution magnetograms on the solar surface, observational data-based modeling is a promising way to quantitatively study the underlying physical mechanisms behind observations. By incorporating thermal conduction and radiation losses in the energy equation, we develop a new data-driven radiative magnetohydrodynamic model, which has the capability of capturing the thermodynamic evolution compared to our previous zero-β model. Our numerical results reproduce the major observational characteristics of the X1.0 flare on 2021 October 28 in NOAA active region 12887, including the morphology of the eruption, the kinematics of the flare ribbons, extreme ultraviolet (EUV) radiations, and the two components of the EUV waves predicted by the magnetic stretching model, i.e., a fast-mode shock wave and a slower apparent wave, due to successive stretching of the magnetic field lines. Moreover, some intriguing phenomena are revealed in the simulation. We find that flare ribbons separate initially and ultimately stop at the outer stationary quasi-separatrix layers (QSLs). Such outer QSLs correspond to the border of the filament channel and determine the final positions of flare ribbons, which can be used to predict the size and the lifetime of a flare before it occurs. In addition, the side views of the synthesized EUV and white-light images exhibit typical three-part structures of CMEs, where the bright leading front is roughly cospatial with the nonwave component of the EUV wave, reinforcing the use of the magnetic stretching model for the slow component of EUV waves.

show abstract

Section: Relationship Between Cme Fronts and Euv Wavessupporting

confidence: 67%

Section: Event Overview and Numerical Setupsupporting

confidence: 65%

Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model

Guo

Zhong

et al. 2023

ApJS

Self Cite

View full text Add to dashboard Cite

show abstract

“…Successive stretching of the overlying magnetic field lines generates a bright, expanding front from the source region observed in extreme ultraviolet (EUV) wavelengths, which is named "EIT wave" (Thompson et al 1998;Chen et al 2002Chen et al , 2005Ballai et al 2005). Meanwhile, a faster coronal Moreton wave is frequently observed to propagate ahead of the EIT wave (Chen & Wu 2011;Kumar et al 2013;Devi et al 2022). It is generally accepted that an EUV wave consists of a wave-like component moving at fast magnetosonic speed (Wills-Davey & Thompson 1999;Zheng et al 2023) and a coherent driven compression front related to the eruption (Downs et al 2011).…”

Section: Introductionmentioning

confidence: 99%

“…Fast-mode kink oscillations of coronal loops excited by flares were first observed by the Transition Region and Coronal Explorer (TRACE) spacecraft (Aschwanden et al 1999;Nakariakov et al 1999). Kink oscillations could also been induced by small-scale magnetic reconnection (He et al 2009), coronal jets (Dai et al 2021), prominence eruptions (Zimovets & Nakariakov 2015), and EUV waves (Shen & Liu 2012;Kumar et al 2013;Srivastava & Goossens 2013;Guo et al 2015;Su et al 2018;Devi et al 2022). Coronal seismology based on kink oscillations provides an effective way of determining the magnetic field strength, internal Alfvén speed, and density scale height of the oscillating loops (Nakariakov & Ofman 2001;Verwichte et al 2004;Verth & Erdélyi 2008;Li et al 2017;Yang et al 2020;Zhang et al 2020;Li & Long 2023).…”

Section: Introductionmentioning

confidence: 99%

First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops

Zhang

et al. 2022

ApJL

View full text Add to dashboard Cite

In this Letter, we perform a detailed analysis of the M5.5 class eruptive flare occurring in active region 12,929 on 2022 January 20. The eruption of a hot channel generates a fast coronal mass ejection (CME) and a dome-shaped extreme-ultraviolet (EUV) wave at speeds of 740–860 km s−1. The CME is associated with a type II radio burst, implying that the EUV wave is a fast-mode shock wave. During the impulsive phase, the flare shows quasi-periodic pulsations (QPPs) in EUV, hard X-ray, and radio wavelengths. The periods of QPPs range from 18 to 113 s, indicating that flare energy is released and nonthermal electrons are accelerated intermittently with multiple timescales. The interaction between the EUV wave and low-lying adjacent coronal loops (ACLs) results in contraction, expansion, and transverse vertical oscillation of ACLs. The speed of contraction in 171, 193, and 211 Å is higher than that in 304 Å. The periods of oscillation are 253 s and 275 s in 304 Å and 171 Å, respectively. A new scenario is proposed to explain the interaction. The equation that interprets the contraction and oscillation of the overlying coronal loops above a flare core can also interpret the expansion and oscillation of ACLs, suggesting that the two phenomena are the same in essence.

show abstract

“…Successive stretching of the overlying magnetic field lines generates a bright, expanding front from the source region observed in extreme-ultraviolet (EUV) wavelengths, which is named "EIT wave" (Thompson et al 1998;Chen et al 2002;Ballai et al 2005;Chen et al 2005). Meanwhile, a faster coronal Moreton wave is frequently observed to propagate ahead of the EIT wave (Chen & Wu 2011;Kumar et al 2013;Devi et al 2022). It is generally accepted that an EUV wave consists of a wave-like component moving at fast magnetosonic speed (Wills-Davey & Thompson 1999; Zheng et al 2023) and a coherently driven compression front related to the eruption (Downs et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Transverse Vertical Oscillations During the Contraction and Expansion of Coronal Loops

Zhang

Zhou

et al. 2023

ApJ

View full text Add to dashboard Cite

In this paper, we carry out a detailed analysis of the M1.6 class eruptive flare occurring in NOAA active region 13078 on 2022 August 19. The flare is associated with a fast coronal mass ejection (CME) propagating in the southwest direction with an apparent speed of ∼926 km s−1. Meanwhile, a shock wave is driven by the CME at the flank. The eruption of the CME generates an extreme-ultraviolet (EUV) wave expanding outward from the flare site with an apparent speed of ≥200 km s−1. As the EUV wave propagates eastward, it encounters and interacts with the low-lying adjacent coronal loops (ACLs), which are composed of two loops. The compression of the EUV wave results in contraction, expansion, and transverse vertical oscillations of ACLs. The commencements of contraction are sequential from western to eastern footpoints and the contraction lasts for ∼15 minutes. The speeds of contraction lie in the range of 13–40 km s−1 in 171 Å and 8–54 km s−1 in 193 Å. A long, gradual expansion follows the contraction at lower speeds. Concurrent vertical oscillations are superposed on the contraction and expansion of ACLs. The oscillations last for two to nine cycles and the amplitudes are ≤4 Mm. The periods are between 3 and 12 minutes with an average value of 6.7 minutes. The results show rich dynamics of coronal loops.

show abstract

Extreme-Ultraviolet Wave and Accompanying Loop Oscillations

Cited by 5 publications

References 111 publications

Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model

Thermodynamic and Magnetic Topology Evolution of the X1.0 Flare on 2021 October 28 Simulated by a Data-driven Radiative Magnetohydrodynamic Model

First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops

Transverse Vertical Oscillations During the Contraction and Expansion of Coronal Loops

Contact Info

Product

Resources

About