Tracking Large‐Scale Propagating Coronal Wave Fronts (EIT Waves) using Automated Methods

Wills-Davey, M. J.

doi:10.1086/504144

Cited by 46 publications

(61 citation statements)

References 29 publications

(47 reference statements)

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“…This is consistent with a nonlinear fast-mode wave or shock, as first proposed by Warmuth et al (2001). Conversely, Wills-Davey (2006) have reported a wave observed with TRACE that retained its coherence (i.e., no pulse broadening). However, this wave was tracked only over a comparatively short distance (200 Mm), which could have been an insufficient distance for the broadening to take effect.…”

Section: Perturbation Profilesupporting

confidence: 87%

“…Harra and Sterling (2003) first reported evidence for two distinct wavefronts in an event observed with TRACE. 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).…”

Section: Propagation Heights and 3d Structurementioning

confidence: 84%

“…Consequently, the spatial scale of the soliton in Hall-MHD is of the order of few ion inertial lengths (see Miteva and Mann, 2008), which only amounts to some 10 m in the corona. Finally, the observational constraint of the retainment of coherence (i.e., no increase in pulse width) is imposed only by a single weak EUV wave observed with TRACE (Wills-Davey and Wills-Davey, 2006). Conversely, most coronal waves do actually show a widening of the perturbation profile, as discussed in Section 4.3.…”

Section: Willsmentioning

confidence: 99%

“…While the Transition Region and Coronal Explorer (TRACE; Handy et al, 1999) provided EUV images at sub-minute cadences, its restricted field of view has limited its usefulness for studies of large-scale phenomena, and there is only a single EUV wave event that has been studied extensively using TRACE (Wills-Davey and Wills-Davey, 2006;Wills-Davey et al, 2007). Significant progress has resulted from the high-cadence EUV imaging that has become available with the Extreme Ultraviolet Imager (EUVI; Wülser et al, 2004;Howard et al, 2008) on the two STEREO spacecraft, the Sun Watcher using Active Pixel detectors and Image Processing (SWAP; Halain et al, 2010) aboard PROBA2, and the Atmospheric Imaging Assembly (AIA; Lemen et al, 2012) aboard SDO.…”

mentioning

confidence: 99%

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Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

162

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: Perturbation Profilesupporting

confidence: 87%

Section: Propagation Heights and 3d Structurementioning

confidence: 84%

Section: Willsmentioning

confidence: 99%

mentioning

confidence: 99%

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Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

162

140

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“…Several authors have examined CBF pulse broadening using observations of multiple events from different passbands, including a combination of EUV and Hα observations (Warmuth et al 2001;Warmuth 2010;Veronig et al 2010) as well as observations of a disturbance in soft X-ray data from GOES/SXI (Warmuth et al 2005). In contrast, Wills-Davey (2006) observed no measurable increase in the FWHM of a pulse using high-cadence observations of a single CBF across the limited field-of-view of the Transition Region And Coronal Explorer (TRACE). This led Wills-Davey et al (2007) to propose that CBFs were soliton-like waves which exhibit no significant dispersion with propagation.…”

Section: Introductionmentioning

confidence: 99%

Deceleration and dispersion of large-scale coronal bright fronts

Long

Gallagher

McAteer

et al. 2011

A&A

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Context. One of the most dramatic manifestations of solar activity are large-scale coronal bright fronts (CBFs) observed in extreme ultraviolet (EUV) images of the solar atmosphere. To date, the energetics and kinematics of CBFs remain poorly understood, due to the low image cadence and sensitivity of previous EUV imagers and the limited methods used to extract the features. Aims. In this paper, the trajectory and morphology of CBFs was determined in order to investigate the varying properties of a sample of CBFs, including their kinematics and pulse shape, dispersion, and dissipation. Methods. We have developed a semi-automatic intensity profiling technique to extract the morphology and accurate positions of CBFs in 2.5-10 min cadence images from STEREO/EUVI. The technique was applied to sequences of 171 Å and 195 Å images from STEREO/EUVI in order to measure the wave properties of four separate CBF events. Results. Following launch at velocities of ∼240-450 km s −1 each of the four events studied showed significant negative acceleration ranging from ∼−290 to −60 m s −2 . The CBF spatial and temporal widths were found to increase from ∼50 Mm to ∼200 Mm and ∼100 s to ∼1500 s respectively, suggesting that they are dispersive in nature. The variation in position-angle averaged pulse-integrated intensity with propagation shows no clear trend across the four events studied. These results are most consistent with CBFs being dispersive magnetoacoustic waves.

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Global Coronal Waves

Chen¹

2016

Geophysical Monograph Series

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Tracking Large‐Scale Propagating Coronal Wave Fronts (EIT Waves) using Automated Methods

Cited by 46 publications

References 29 publications

Large-scale Globally Propagating Coronal Waves

Large-scale Globally Propagating Coronal Waves

Deceleration and dispersion of large-scale coronal bright fronts

Global Coronal Waves

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