Dispersively formed quasi-periodic fast magnetosonic wavefronts due to the eruption of a nearby mini-filament

Shen, Yuandeng; Song, Tengfei; Liu, Yu

doi:10.1093/mnrasl/sly044

Cited by 16 publications

(18 citation statements)

References 58 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…In addition, the detrended intensities (blue) are also plotted in the figure, which show the wavefronts more clearly. The percentage intensities also indicate that the intensity variations relative to the background is about 3%, consistent with those detected in quasi-periodic fast-propagating magnetosonic waves (e.g., Liu et al 2011;Shen & Liu 2012b;Shen et al 2013aShen et al , 2018b. With the method of wavelet analysis (Torrence & Compo 1998), the periods of these intensity curves are obtained, and the results are plotted in the right column of Figure 5.…”

Section: Resultssupporting

confidence: 71%

Coronal EUV, QFP, and kink waves simultaneously launched during the course of jet–loop interaction

Shen

Tang

et al. 2018

Monthly Notices of the Royal Astronomical Society: Letters

Self Cite

View full text Add to dashboard Cite

We present the observations of an extreme ultraviolet (EUV) wave, a quasi-periodic fast-propagating (QFP) magnetosonic wave, and a kink wave that were simultaneously associated with the impingement of a coronal jet upon a group of coronal loops. After the interaction, the coronal loop showed obvious kink oscillation that had a period of about 428 seconds. In the meantime, a large-scale EUV wave and a QFP wave are observed on the west of the interaction position. It is interesting that the QFP wave showed refraction effect during its passing through two strong magnetic regions. The angular extent, speed, and lifetime of the EUV (QFP) wave were about 140 • (40 • ), 423 (322) km s −1 , and 6 (26) minutes, respectively. It is measured that the period of the QFP wave was about 390 ± 100. Based on the observational analysis results, we propose that the kink wave was probably excited by the interaction of the jet; the EUV was probably launched by the sudden expansion of the loop system due to the impingement of the coronal jet; and the QFP wave was possibly formed through the dispersive evolution of the disturbance caused by the jet-loop interaction.

show abstract

Section: Resultssupporting

confidence: 71%

Coronal EUV, QFP, and kink waves simultaneously launched during the course of jet–loop interaction

Shen

Tang

et al. 2018

Monthly Notices of the Royal Astronomical Society: Letters

Self Cite

View full text Add to dashboard Cite

show abstract

“…Here, based on the close temporal and spatial relationship between the QFP wave and the EUV wave, it is obvious that the generation of the multiple wavefronts were associated with the interaction of the EUV wave. Therefore, the generation of this QFP wave was possibly due to the dispersive evolution of the disturbance caused by the interaction (Liu et al 2012;Shen et al 2018b). Here, we would like to point out that mode conversion of solar EUV wavefronts have been reported in recent observational and simulation studies, where fast-mode magnetosonic waves transformed into slow-mode magnetosonic waves during their interaction with other magnetic structures (Chandra et al 2016;Chen et al 2016;Zong & Dai 2017).…”

Section: The Event On 2011 February 15mentioning

confidence: 99%

EUV Waves Driven by the Sudden Expansion of Transequatorial Loops Caused by Coronal Jets

Shen

Tang

Miao

et al. 2018

ApJL

Self Cite

View full text Add to dashboard Cite

We present two events to study the driving mechanism of extreme-ultraviolet (EUV) waves that are not associated with coronal mass ejections (CMEs), by using high resolution observations taken by the Atmospheric Imaging Assembly (AIA) on board Solar Dynamics Observatory. Observational results indicate that the observed EUV waves were accompanied by flares and coronal jets, but without CMEs that were regarded as the driver of most EUV waves in previous studies. In the first case, it is observed that a coronal jet ejected along a transequatorial loop system at a plane-of-the-sky (POS) speed of 335 ± 22 km s −1 , in the meantime, an arc-shaped EUV wave appeared on the eastern side of the loop system. In addition, the EUV wave further interacted with another interconnecting loop system and launched a fast propagating (QFP) magnetosonic wave along the loop system, which had a period of 200 s and a speed of 388 ± 65 km s −1 , respectively. In the second case, we also observed a coronal jet ejected at a POS speed of 282 ± 44 km s −1 along a transequatorial loop system and the generation of bright EUV wave on the eastern side of the loop system. Based on the observational results, we propose that the observed EUV waves on the eastern side of the transequatorial loop systems are fast-mode magnetosonic waves, and they were driven by the sudden lateral expansion of the transequatorial loop systems due to the direct impingement of the associated coronal jets, while the QFP wave in the fist case formed due to the dispersive evolution of the disturbance caused by the interaction between the EUV wave and the interconnecting coronal loops. It is noted that EUV waves driven by sudden loop expansions have shorter lifetimes than those driven by CMEs.

show abstract

“…the regular and repeating variations in the Doppler velocity, line width and intensity of spectral lines (e.g., Wang et al 2015;Tian et al 2016;Brosius, & Inglis 2018). Finally, the QPPs in solar flares are found to share some main frequencies with the quasi-periodic fast-propagating (QFP) magnetosonic waves (e.g., Liu et al 2011;Nisticò et al 2014;Shen et al 2018a), indicating their common origin (Yuan et al 2013;Liu & Ofman 2014;Shen et al 2018b;Kumar et al 2017).…”

Section: Introductionmentioning

confidence: 93%

Quasi-periodic pulsation detected in Lyman-alpha emission during solar flares

Li,

Lu,

Ning

et al. 2020

Preprint

View full text Add to dashboard Cite

We investigated the quasi-periodic pulsation (QPP) in Ly-α, X-ray and extremeultraviolet (EUV) emissions during two solar flares, i.e., an X-class (SOL2012-01-27T) and a C-class (SOL2016-02-08T). The full-disk Ly-α and X-Ray flux during these solar flares were recorded by the EUV Sensor and X-Ray Sensor on board the Geostationary Operational Environmental Satellite. The flare regions were located from the EUV images measured by the Atmospheric Imaging Assembly. The QPP could be identified as a series of regular and periodic peaks in the light curves, and its quasi-periodicity was determined from the global wavelet and Fourier power spectra. A quasi-periodicity at about 3 minutes is detected during the impulsive phase of the X-class flare, which could be explained as the acoustic wave in the chromosphere (e.g., Milligan et al. 2017). Interestingly, a quasi-periodicity at roughly 1 minute is discovered during the entire evolutionary phases of solar flares, including the precursor, impulsive, and gradual phases. This is the first report of 1-minute QPP in the Ly-α emission during solar flares, in particular during the flare precursor. It may be interpreted as a self-oscillatory regime of the magnetic reconnection, such as magnetic dripping.

show abstract

Dispersively formed quasi-periodic fast magnetosonic wavefronts due to the eruption of a nearby mini-filament

Cited by 16 publications

References 58 publications

Coronal EUV, QFP, and kink waves simultaneously launched during the course of jet–loop interaction

Coronal EUV, QFP, and kink waves simultaneously launched during the course of jet–loop interaction

EUV Waves Driven by the Sudden Expansion of Transequatorial Loops Caused by Coronal Jets

Quasi-periodic pulsation detected in Lyman-alpha emission during solar flares

Contact Info

Product

Resources

About