On the nature of EIT waves, EUV dimmings and their link to CMEs

Zhukov, A. N.; Auchère, F.

doi:10.1051/0004-6361:20040351

Cited by 223 publications

(199 citation statements)

References 41 publications

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“…Then, the CME flank decelerates, while the coronal wave detaches and continues its propagation. This scenario is consistent with the bimodality observed in coronal EUV waves by Zhukov and Auchère (2004). It is additionally supported by 3D modelling based on tomographic reconstructions, which show that the CME is not cospatial with the coronal wavefront Temmer et al, 2011).…”

Section: Coronal Mass Ejections (Cmes)supporting

confidence: 85%

“…High-cadence observations have also confirmed the bimodality of coronal waves originally suggested by Zhukov and Auchère (2004). This means that many EUV wave show a fast bright front that appears to be wavelike in nature, and additionally trailing intensity enhancements that are associated with an erupting CME (Section 4.1.4).…”

supporting

confidence: 69%

“…However, other authors (Wills-Davey and Wills-Davey, 2006) interpreted the same event in terms of the single pulse EUV wave that is commonly observed. Based on limb observations of EIT waves, a general bimodality of coronal waves was suggested by Zhukov and Auchère (2004). They noted that some EIT waves actually consist of two distinct parts: a leading front that appears to be wave-like (diffuse, quasi-circular), and a slower trailing front that is followed by coronal dimmings.…”

Section: Propagation Heights and 3d Structurementioning

confidence: 99%

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Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

156

140

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Large-scale, globally propagating wave-like disturbances have been observed in the solar chromosphere and by inference in the corona since the 1960s. However, detailed analysis of these phenomena has only been conducted since the late 1990s. This was prompted by the availability of high-cadence coronal imaging data from numerous spaced-based instruments, which routinely show spectacular globally propagating bright fronts. Coronal waves, as these perturbations are usually referred to, have now been observed in a wide range of spectral channels, yielding a wealth of information. Many findings have supported the "classical" interpretation of the disturbances: fast-mode MHD waves or shocks that are propagating in the solar corona. However, observations that seemed inconsistent with this picture have stimulated the development of alternative models in which "pseudo waves" are generated by magnetic reconfiguration in the framework of an expanding coronal mass ejection. This has resulted in a vigorous debate on the physical nature of these disturbances. This review focuses on demonstrating how the numerous observational findings of the last one and a half decades can be used to constrain our models of large-scale coronal waves, and how a coherent physical understanding of these disturbances is finally emerging. Article RevisionsLiving Reviews supports two ways of keeping its articles up-to-date:Fast-track revision. A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here.Major update. A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number.For detailed documentation of an article's evolution, please refer to the history document of the article's online version at http://dx

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Section: Coronal Mass Ejections (Cmes)supporting

confidence: 85%

supporting

confidence: 69%

Section: Propagation Heights and 3d Structurementioning

confidence: 99%

See 1 more Smart Citation

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

156

140

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“…Since the coronal dimmings can be observed in different wavelengths, they are mainly due to the depletion of plasma density. Several authors quantitatively calculated the dimmings due to the plasma density depletion using Yohkoh/SXT (Sterling & Hudson 1997), SOHO/EIT (Zhukov & Auchère 2004) and STEREO data (Aschwanden 2009).…”

Section: Two Types Of Euv Waves and Stationary Euv Wave Frontsmentioning

confidence: 99%

“…They also concluded that EIT waves having S-shape signatures are always associated with both flares and CMEs. On the basis of SOHO/EIT observations, Zhukov & Auchère (2004) suggested a bimodal characteristic for EIT waves, i.e., including a wave mode and an eruptive mode component. The wave-mode component is a wavelike phenomenon and represented by pure MHD waves.…”

Section: Introductionmentioning

confidence: 99%

Peculiar Stationary Euv Wave Fronts in the Eruption on 2011 May 11

Chandra

Chen

Fulara

et al. 2016

ApJ

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We present and interpret the observations of extreme ultraviolet (EUV) waves associated with a filament eruption on 2011 May 11. The filament eruption also produces a small B-class two ribbon flare and a coronal mass ejection. The event is observed by the Solar Dynamic Observatory with high spatio-temporal resolution data recorded by the Atmospheric Imaging Assembly. As the filament erupts, we observe two types of EUV waves (slow and fast) propagating outwards. The faster EUV wave has a propagation velocity of ∼500 km s −1 and the slower EUV wave has an initial velocity of ∼120 km s −1 . We report, for the first time, that not only does the slower EUV wave stop at a magnetic separatrix to form bright stationary fronts, but also the faster EUV wave transits a magnetic separatrix, leaving another stationary EUV front behind.

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