An Extreme-ultraviolet Wave Generating Upward Secondary Waves in a Streamer-like Solar Structure

Zheng, Ruisheng; Chen, Yao; Feng, Shiwei; Wang, Bing; Song, Hongqiang

doi:10.3847/2041-8213/aabe87

Cited by 12 publications

(8 citation statements)

References 50 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Along with the occurrence of the reflection and refraction of the EUV wave near the magnetic separatrix, a secondary wave 2ND might be further produced and propagate outward. Similar situations can be found in some other studies (e.g., Ofman and Thompson, 2002;Shen and Liu, 2012;Chandra et al, 2016;Zheng et al, 2018). In addition, some studies have shown a close relationship between Type II radio bursts and such interactions (e.g., Feng et al, 2012;Kong et al, 2012;Shen et al, 2019).…”

Section: Sba and The Secondary Wavesupporting

confidence: 87%

“…Since the first discovery of Type II bursts, they have been found to be closely related to both flares (e.g., Wild et al, 1954;Maxwell and Thompson, 1962;Dodge, 1975) and high-velocity ejections (e.g., Dodson et al, 1953;Giovanelli and Roberts, 1958;Swarup et al, 1960). The blast wave initiated by flares and piston-driven mechanism associated with coronal mass ejections (CMEs) have become the two main competitors of the triggering mechanism of the Type II bursts as reviewed by the papers (e.g., Cliver et al, 1999;Vršnak and Cliver, 2008;Nindos et al, 2011) and also suggested by some recent studies (e.g., Zheng et al, 2018;Eselevich et al, 2019;Frassati et al, 2019). In the piston-driven mechanism, besides CME front, some other triggers, such as soft X-ray jet, erupting coronal loop and eruptive magnetic flux rope are also proposed to explain the production of shock or Type II burst (e.g., Klein et al, 1999;Klassen et al, 2003;Dauphin et al, 2006;Su et al, 2015;Eselevich et al, 2017;Grechnev et al, 2018).…”

Section: Introductionmentioning

confidence: 90%

See 1 more Smart Citation

Two Successive Type II Radio Bursts Associated With B-Class Flares and Slow CMEs

Chen

2020

Front. Astron. Space Sci.

View full text Add to dashboard Cite

From 2018 Oct 12 to 13, three successive solar eruptions (E1-E3) with B-class flares and poor white light coronal mass ejections (CMEs) occurred from the same active region NOAA AR 12724. Interestingly, the first two eruptions are associated with Type II radio bursts but the third is not. Using the soft X-ray flux data, radio dynamic spectra and dual perspective EUV intensity images, we comparatively investigate the three events. Our results show that their relevant flares are weak (B2.1, B7.9, and B2.3) and short-lived (13, 9, and 14 min). The main eruption directions of E1 and E2 are along ∼45 • north of their radial directions, while E3 primarily propagated along the radial direction. In the EUV channels, the early speeds of the first two CMEs have apparent speeds of ∼320 and ∼380 km s −1 , which could exceed their respective local Alfvén speeds of ∼300 and ∼350 km s −1 . However, the CME in the third eruption possesses a much lower speed of ∼160 km s −1 . These results suggest that the observed Type II radio bursts in the eruptions E1 and E2 are likely triggered by their associated CMEs and the direction of eruption and the ambient plasma and magnetic environments may take an important place in producing Type II radio burst or shock as well.

show abstract

Section: Sba and The Secondary Wavesupporting

confidence: 87%

Section: Introductionmentioning

confidence: 90%

Two Successive Type II Radio Bursts Associated With B-Class Flares and Slow CMEs

Chen

2020

Front. Astron. Space Sci.

View full text Add to dashboard Cite

show abstract

“…More detailed features of EUV waves revealed by recent observations pose new challenges to numerical models. Our simulation self-consistently reproduces quasi-periodic wave trains within a large-scale EUV wave, as found in the AIA observations (e.g., Liu et al 2012;Yuan et al 2013;Nisticò et al 2014;Zheng et al 2018;Shen et al 2019).…”

Section: Quasi-periodic Wave Trainssupporting

confidence: 73%

Exploring the Nature of EUV Waves in a Radiative Magnetohydrodynamic Simulation

Wang,

Chen,

Ding

2021

Preprint

View full text Add to dashboard Cite

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.

show abstract

“…EUV waves are associated with various of solar successful eruptions, such as CMEs, solar flares, filament eruptions, and and their launch strongly depends on the rapid lateral expansion of the CME flank (Nitta et al 2013;Liu & Ofman 2014). In addition, it has been reported that the EUV wave can be generated by the failed eruption or the filament activation without any eruption (Zheng et al 2012(Zheng et al , 2018(Zheng et al , 2020. Hence, the formation of EUV waves is subject to the rapid expansion of the loops covering the erupting cores, no matter if associated CMEs happen.…”

Section: Introductionmentioning

confidence: 99%

Birth places of extreme ultraviolet waves driven by impingement of solar jets upon coronal loops

Zhang,

Zheng,

Chen

et al. 2022

Preprint

Self Cite

View full text Add to dashboard Cite

Solar extreme ultraviolet (EUV) waves are large-scale propagating disturbances in the corona. It is generally believed that the vital key for the formation of EUV waves is the rapid expansion of the loops that overlie erupting cores in solar eruptions, such as coronal mass ejections (CMEs) and solar jets. However, the details of the interaction between the erupting cores and overlying loops are not clear, because that the overlying loops are always instantly opened after the energetic eruptions. Here, we present three typical jet-driven EUV waves without CME to study the interaction between the jets and the overlying loops that remained closed during the events. All three jets emanated from magnetic flux cancelation sites in source regions. Interestingly, after the interactions between jets and overlying loops, three EUV waves respectively formed ahead of the top, the near end (close to the jet source), and the far (another) end of the overlying loops. According to the magnetic field distribution of the loops extrapolated from Potential Field Source Surface method, it is confirmed that the birth places of three jet-driven EUV waves were around the weakest magnetic field strength part of the overlying loops. We suggest that the jet-driven EUV waves preferentially occur at the weakest part of the overlying loops, and the location can be subject to the magnetic field intensity around the ends of the loops.

show abstract

An Extreme-ultraviolet Wave Generating Upward Secondary Waves in a Streamer-like Solar Structure

Cited by 12 publications

References 50 publications

Two Successive Type II Radio Bursts Associated With B-Class Flares and Slow CMEs

Two Successive Type II Radio Bursts Associated With B-Class Flares and Slow CMEs

Exploring the Nature of EUV Waves in a Radiative Magnetohydrodynamic Simulation

Birth places of extreme ultraviolet waves driven by impingement of solar jets upon coronal loops

Contact Info

Product

Resources

About