Well-defined EUV wave associated with a CME-driven shock

Cunha-Silva, R. D.; Selhorst, C. L.; Fernandes, Francisco Carlos; Silva, A. J. Oliveira e

doi:10.1051/0004-6361/201630358

Cited by 9 publications

(5 citation statements)

References 55 publications

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“…Further, we found that the EUV wave propagates ahead of the CME leading edge using the STEREO-A and LASCO data sets. This supports the earlier findings and models that the EUV wave is driven by CME (Ma et al, 2011;Vourlidas, 2009, 2012;Cunha-Silva, Fernandes, and Selhorst, 2015;Cunha-Silva et al, 2018).…”

Section: Discussionsupporting

confidence: 91%

Extreme-ultraviolet wave and accompanying loop oscillations

Devi

Chandra

Awasthi

et al. 2022

Preprint

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In this article, we present the observations of an Extreme-Ultraviolet (EUV) wave, which originated from the active region (AR) NOAA 12887 on 28 October 2021 and its impact on neighbouring loops. The event was observed by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) satellite at various wavebands and by the Solar TErrestrial RElationsObservatory-Ahead (STEREO–A), EUVI and COR1 instruments with a different view angle than SDO. We show that the EUV wave consists of severalwaves as well as non-wave phenomena. The wave–nature component includes:fast–mode part of the EUV wave, creation of oscillations in nearby loops andthe appearance of wave trains. The non-wave component consists of stationary fronts. We perform the analysis of selected oscillating loops and find the periods of these oscillation ranges from 230 – 549 s. Further, we compute the density ratio inside and outside the loops and the magnetic field strength. The computed density ratio and magnetic field are found in the range of 1.08 – 2.92 and 5.75 –8.79 G, respectively. Finally using the 3D point of view of the satellites we found that the EUV wave propagates ahead of the CME leading edge.

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Section: Discussionsupporting

confidence: 91%

Extreme-ultraviolet wave and accompanying loop oscillations

Devi

Chandra

Awasthi

et al. 2022

Preprint

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“…Because chromospheric Moreton waves were believed to be driven by the flare pressure pulses for a long time since Uchida (1968), solar physicists naturally thought at the beginning that EUV waves also have the same driving mechanism (e.g., Khan & Aurass 2002;Hudson et al 2003;Warmuth et al 2004). However, more and more recent high-resolution observational studies have shown that EUV waves are in fact bow shocks driven by CMEs instead of flare pressure pulses (e.g., Patsourakos & Vourlidas 2009;Kienreich et al 2009;Patsourakos et al 2010;Chen 2006;Shen & Liu 2012a,c;Shen et al 2017a;Xue et al 2013;Long et al 2017b;Cunha-Silva et al 2018;Liu et al 2011b). Further investigations indicated that EUV waves can also be excited by other kinds of slightly different processes, such as newly-formed expanding loops, coronal jets, and mini-filament eruptions in small scales (e.g., Podladchikova et al 2010;Zheng et al 2012Zheng et al , 2013Su et al 2015;Shen et al 2017a), and the sudden expansion of transequatorial loops driven by coronal jets in large scales (Shen et al 2018e,d) .…”

Section: Introductionmentioning

confidence: 99%

First Unambiguous Imaging of Large-scale Quasi-periodic Extreme-ultraviolet Wave or Shock

Shen

Chen

Liu

et al. 2019

ApJ

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We report the first unambiguous quasi-periodic large-scale extreme-ultraviolet (EUV) wave or shock that was detected by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory. During the whip-like unwinding eruption of a small filament on 2012 April 24, multiple consecutive large-scale wavefronts emanating from AR11467 were observed simultaneously along the solar surface and a closed transequatorial loop system. In the meantime, an upward propagating dome-shaped wavefront was also observed, whose initial speed and deceleration are about 1392 km s −1 and 1.78 km s −2 , respectively. Along the solar surface, the quasi-peridoic wavefronts had a period of about 163±21 seconds and propagated at a nearly constant speed of 747±26 km s −1 ; they interacted with active region AR11469 and launched a sympathetic upward propagating secondary EUV wave. The wavefronts along the loop system propagated at a speed of 897 km s −1 , and they were reflected back at the southern end of the loop system at a similar speed. In addition to the propagating waves, a standing kink wave was also present in the loop system simultaneously. Periodicity analysis reveals that the period of the wavefronts was consistent with that of the unwinding helical structures of the erupting filament. Based on these observational facts, we propose that the observed quasi-periodic EUV wavefronts were most likely excited by the periodic unwinding motion of the filament helical structures. In addition, two different seismological methods are applied to derive the magnetic field strength of the loop system, and for the first time the reliability of these inversion techniques are tested with the same magnetic structure.

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“…In the past decade, the Atmospheric Imaging Assembly (AIA) on board Solar Dynamics Observatory (SDO) allowed to acquire observation data with unprecedented high spatial and temporal resolutions, revealing more detailed features of EUV waves. Events with both wave and non-wave components are found to be very common (Chen & Wu 2011;Asai et al 2012;Liu et al 2013;Cunha-Silva et al 2018;Fulara et al 2019). Such observations are also supported by three-dimensional (3D) models (Cohen et al 2009;Downs et al 2012).…”

Section: Introductionmentioning

confidence: 61%

Exploring the Nature of EUV Waves in a Radiative Magnetohydrodynamic Simulation

Wang,

Chen,

Ding

2021

Preprint

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Coronal extreme-ultraviolet (EUV) waves are large-scale disturbances propagating in the corona, whose physical nature and origin have been discussed for decades. We report the first three dimensional (3D) radiative magneto-hydrodynamic (RMHD) simulation of a coronal EUV wave and the accompanying quasi-periodic wave trains. The numerical experiment is conducted with the MURaM code and simulates the formation of solar active regions through magnetic flux emergence from the convection zone to the corona. The coronal EUV wave is driven by the eruption of a magnetic flux rope that also gives rise to a C-class flare. It propagates in a semi-circular shape with an initial speed ranging from about 550 to 700 km s −1 , which corresponds to an average Mach number (relative to fast magnetoacoustic waves) of about 1.2. Furthermore, the abrupt increase of the plasma density, pressure and tangential magnetic field at the wavefront confirms fast-mode shock nature of the coronal EUV wave. Quasi-periodic wave trains with a period of about 30 s are found as multiple secondary wavefronts propagating behind the leading wavefront and ahead of the erupting magnetic flux rope. We also note that the true wavefront in the 3D space can be very inhomogeneous, however, the lineof-sight integration of EUV emission significantly smoothes the sharp structures in 3D and leads to a more diffuse wavefront.

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Well-defined EUV wave associated with a CME-driven shock

Cited by 9 publications

References 55 publications

Extreme-ultraviolet wave and accompanying loop oscillations

Extreme-ultraviolet wave and accompanying loop oscillations

First Unambiguous Imaging of Large-scale Quasi-periodic Extreme-ultraviolet Wave or Shock

Exploring the Nature of EUV Waves in a Radiative Magnetohydrodynamic Simulation

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