Abstract Electromagnetic wave lensing, a common physical phenomenon recognized in visible light for centuries, finds extensive applications manipulating optical systems such as telescopes and cameras. Magnetohydrodynamic is perturbation the corona. By using high spatio-temporal resolution observations from Solar Dynamics Observatory, here, we report observation of magnetohydrodynamic lensing highly ionized magnetized coronal plasma, where quasi-periodic wavefronts emanated flare converged at...

Abstract Ubiquitous solar jets or jet-like activities are generally regarded as an important source of energy and mass input to the upper atmosphere wind. However, their triggering driving mechanisms not completely understood. By taking advantage stereoscopic observations with high temporal spatial resolutions taken by Solar Dynamic Observatory ( SDO ) Terrestrial Relations STEREO ), we report intriguing two-sided-loop jet that occurred on 2013 June 02, was dynamically associated eruption a...

We report the first unambiguous quasi-periodic large-scale extreme-ultraviolet (EUV) wave or shock that was detected by Atmospheric Imaging Assembly on board Solar Dynamics Observatory. During whip-like unwinding eruption of a small filament 2012 April 24, multiple consecutive wavefronts emanating from AR11467 were observed simultaneously along solar surface and closed transequatorial loop system. In meantime, an upward propagating dome-shaped wavefront also observed, whose initial speed...

Using imaging and radio multi-wavelength observations, we studied the origin of two homologous accelerated electron beams a quasi-periodic fast-propagating (QFP) wave train associated with solar jet on 2012 July 14. The occurred in small-scale fan-spine magnetic system embedding large-scale pseudostreamer, which GOES C1.4 flare, jet-like coronal mass ejection (CME), type II burst, III burst. During initial stage, QFP fast moving on-disk source were detected succession ahead along outer spine...

Abstract Double-decker filaments and their eruptions have been widely observed in recent years, but physical formation mechanism is still unclear. Using high spatiotemporal resolution, multi-wavelength observations taken by the New Vacuum Solar Telescope Dynamics Observatory, we show of a double-decker pair flux rope system two successive tether-cutting bipolar active region. Due to combined effect photospheric shearing convergence motions around region’s polarity inversion line (PIL), arms...

The detailed observational analysis of a homologous Extreme-ultraviolet (EUV) wave event is presented to study the driving mechanism and physical property EUV waves, combining high resolution data taken by Solar Dynamics Observatory TErrestrial RElations Observatory. It observed that four waves originated from same active region AR11476 within about one hour, time separations between consecutive were 8 - 20 minutes. showed narrow arc-shaped wavefronts propagated in direction along...

The reflection, refraction, and transmission of large-scale extreme ultraviolet (EUV) waves (collectively, secondary waves) have been observed during their interactions with coronal structures such as active regions (ARs) holes (CHs). However, the effect total reflection EUV has not reported in literature. Here, we present first unambiguous observational evidence a quasi-periodic wave train its interaction polar CH. event occurred NOAA AR 12473, located close to southeast limb solar disk,...

Abstract This paper presents three distinct wave trains that occurred on 2023 April 21: a broad quasiperiodic fast-propagating (QFP) train and bidirectional narrow QFP trains. The expands outward in circular front, while propagate the northward southward directions, respectively. concurrent presence of offers remarkable opportunity to investigate their respective triggering mechanisms. Measurement shows speed is range 300–1100 km s −1 different propagating directions. There significant...

We present the observations of an extreme ultraviolet (EUV) wave, a quasi-periodic fast-propagating (QFP) magnetosonic and kink wave that were simultaneously associated with impingement coronal jet upon group loops. After interaction, loop showed obvious oscillation had period about 428 seconds. In meantime, large-scale EUV QFP are observed on west interaction position. It is interesting refraction effect during its passing through two strong magnetic regions. The angular extent, speed,...

Abstract 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 Atmospheric Imaging Assembly on board Solar Dynamics Observatory . Observational results indicate observed EUV were accompanied flares and jets, but CMEs regarded as drivers most in previous studies. In first case, it is a jet ejected along transequatorial loop system at plane-of-the-sky (POS)...

Large-scale Extreme-ultraviolet (EUV) waves are frequently observed as an accompanying phenomenon of flares and coronal mass ejections (CMEs). Previous studies mainly focus on EUV with single wavefronts that generally thought to be driven by the lateral expansion CMEs. Using high spatio-temporal resolution multi-angle imaging observations taken Solar Dynamic Observatory Terrestrial Relations Observatory, we present observation a broad quasi-periodic fast propagating (QFP) wave train composed...

ABSTRACT We report the first observations of simultaneous large-amplitude longitudinal and transverse oscillations a quiescent filament trigged by two-sided-loop jet formed magnetic reconnection between an emerging loop in channel, recorded Solar Dynamics Observatory TErrestrial RElations Observatory. The north arm firstly pushed mass moving northwardly along field lines consisting coronal cavity, then some elevated fell back started to oscillate longitudinally at bottom cavity (i.e. dip)....

Abstract A solar jet can often cause coronal mass ejections (CMEs) with different morphologies in the high corona, for example, jet-like CMEs, bubble-like and so-called twin CMEs that include a pair of simultaneous CMEs. However, what determines morphology jet-related CME is still an open question. Using spatiotemporal resolution stereoscopic observations taken by Solar Dynamics Observatory Terrestrial Relations from 2010 October to 2012 December, we performed statistical study potential...

It is unclear whether successive filament eruptions at different sites within a short time interval are physically connected or not. Here, we present the observations of small and large in tripolar magnetic field region whose coronal showed as fan-spine system. By analyzing multi-wavelength taken by Solar Dynamic Observatory (SDO) extrapolated three-dimensional field, find that two filaments resided respectively lobes make up inner fan structure In addition, system was also revealed...

Quasi-periodic fast-propagating (QFP) magnetosonic wave trains are commonly observed in the low corona at extreme ultraviolet wavelength bands. Here, we report first white-light imaging observation of a QFP train propagating outwardly outer ranging from 2 to 4 R ⊙ . The was recorded by Large Angle Spectroscopic Coronagraph on board Solar and Heliospheric Observatory (SOHO), associated with GOES M1.5 flare NOAA active region AR12172 southwest limb solar disk. Measurements show that speed...

Solar macrospicules are beam-like cool plasma ejections of size in-between spicules and coronal jets, which can elucidate potential connections between jetting activity at different scales. With high-resolution observations from the {\em New Vacuum Telescope} Dynamic Observatory, we investigate origin five groups recurrent active-region macrospicules. Before launch each macrospicule, detect a compact bright patch (BP) its base where newly emerging dipole contacts cancel with pre-existing...

A solar jet on 2014 July 31, which was accompanied by a GOES C1.3 flare and mini-filament eruption at the base, studied using observations taken New Vacuum Solar Telescope Dynamic Observatory. Magnetic field extrapolation revealed that confined in fan-spine magnetic system hosts null point height of about 9 Mm from surface. An inner ribbon surrounded an outer circular remote were observed to be associated with eruption, ribbons respectively located footprints spines, while one manifested...

The fine magnetic structure is vitally important to understanding the formation, stabilization and eruption of solar filaments, but so far, it still an open question yet be resolved. Using stereoscopic observations taken by Solar Dynamics Observatory TErrestrial RElations Obsevatory, we studied generation mechanism a two-sided-loop jet (TJ) ejection process plasma into overlying filament-cavity system. We find that was due reconnection between emerging flux loop filament. jet's two arms...

Abstract About the driven mechanisms of quasiperiodic fast-propagating (QFP) wave trains, there exist two dominant competing physical explanations: they are associated with flaring energy release or attributed to waveguide dispersion. Employing Solar Dynamics Observatory/Atmospheric Imaging Assembly 171 Å images, we investigated a series QFP trains composed multiple fronts propagating along loop system during accompanying flare on 2011 November 11. The showed high correlation in start times...

Abstract Large-scale extreme-ultraviolet waves commonly exhibit as single wave front and are believed to be caused by coronal mass ejections. Utilizing high spatiotemporal resolution imaging observations from the Solar Dynamics Observatory, we present two sequentially generated trains originating same active region: a narrow quasiperiodic fast-propagating (QFP) train that propagates along loop system above jet broad QFP travels solar surface beneath jet. The measurements indicate...

Abstract We present the sympathetic eruption of a standard and blowout coronal jet originating from two adjacent bright points (CBP1 CBP2) in polar hole, using soft X-ray extreme-ultraviolet observations respectively taken by Hinode Solar Dynamics Observatory. In event, collimated with obvious westward lateral motion first launched CBP1, during which small point appeared around CBP1's east end, magnetic flux cancellation was observed within source region. Based on these characteristics, we...

The excitation mechanism of coronal quasi-period fast-propagating (QFP) wave trains remains unresolved. Using Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory observations, we study a narrow and broad QFP train excited one after another during successive eruptions filaments hosted within fan-spine magnetic system on 2013 October 20. consecutive occurrence these two types in same event provides an excellent opportunity to explore their mechanisms compare physical...