Large-scale Bright Fronts in the Solar Corona: A Review of “EIT waves”

Gallagher, Peter T.; Long, David M.

doi:10.1007/s11214-010-9710-7

Cited by 114 publications

(72 citation statements)

References 87 publications

(183 reference statements)

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“…The main contenders are the MHD wave/shock model (see Sections 2.2 and 6.1) and different magnetic reconfiguration models (Sections 2.3 and 6.2), as well as various combinations of these scenarios (Section 6.3). For more reviews on the topic of large-scale coronal waves, see Warmuth (2007); Wills-Davey and Attrill (2009) ;Gallagher and Long (2011);Zhukov (2011);Warmuth (2011); Patsourakos and Vourlidas (2012); Liu and Ofman (2014). The recently discovered phenomena of small-scale EUV waves (Innes et al, 2009;…”

Section: Overviewmentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

168

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: Overviewmentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

168

140

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“…From observations with the Extreme Ultraviolet Imager (EUVI) on board STEREO-B, Veronig et al (2010) found that coronal waves are dome shaped with erupting CME loops inside the dome. The CW properties can be found tabulated in Gallagher & Long (2011).…”

Section: In Hα Observations Prop-mentioning

confidence: 99%

“…The interpretations include fast-mode waves (Wills-Davey & Thompson 1999;Warmuth et al 2001;Schmidt & Ofman 2010), slow-mode waves or solitons (Wills-Davey et al 2007), and non-waves related to a current shell (Delannée et al 2008) or successively reconnecting mag- netic field lines at a CME front (Delannée et al 2014;Attrill 2010, and the references therein). More details on the properties and modelling of coronal waves can be found in several reviews by Vršnak & Cliver (2008), Long (2011), andVourlidas (2012). The most recent review by Liu & Ofman (2014) summarises the very latest findings from AIA/SDO observations and modelling of coronal/EIT waves.…”

Section: In Hα Observations Prop-mentioning

confidence: 99%

A coronal wave and an asymmetric eruptive filament in SUMER, CDS, EIT, and TRACE co-observations

Madjarska¹,

Doyle²,

Shetye³

2015

A&A

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Context. The investigation covers the complex subject of coronal waves and the phenomena contributing to and/or causing their formation. Aims. The objectives of the present study is to provide a better physical understanding of the complex inter-relation and evolution of several solar coronal features comprising a double-peak flare, a coronal dimming caused by a Coronal Mass Ejection (CME), a CME-driven compression, and a fast-mode wave. For the first time, the evolution of an asymmetric eruptive filament is analysed in simultaneous Solar Ultraviolet Measurement of Emitted Radiation (SUMER) spectroscopic and Transition Region and Coronal Explorer (TRACE) and Extreme-ultraviolet Imaging Telescope (EIT) imaging data. Methods. We use imaging observations from EIT and TRACE in the 195 Å channel and spectroscopic observations from the Coronal Diagnostic Spectrometer (CDS) in a rastering and SUMER in a sit-and-stare observing mode. The SUMER spectra cover spectral lines with formation temperatures from logT (K) ∼ 4.0 to 6.1. Results. Although the event was already analysed in two previous studies, our analysis brings a wealth of new information on the dynamics and physical properties of the observed phenomena. We found that the dynamic event is related to a complex flare with two distinct impulsive peaks, one according to the Geostationary Operational Environmental Satellite (GOES) classification as C1.1 and the second -C1.9. The first energy release triggers a fast-mode wave and a CME with a clear CME driven compression ahead of it. This activity is related to, or possibly caused, by an asymmetric filament eruption. The filament is observed to rise with its leading edge moving at a speed of ∼300 km s −1 detected both in the SUMER and CDS data. The rest of the filament body moves at only ∼150 km s −1 while untwisting. No signature is found of the fast-mode wave in the SUMER data, suggesting that the plasma disturbed by the wave had temperatures above 600 000 K. The erupting filament material is found to emit only in spectral lines at transition region temperatures. Earlier identification of a coronal response detected in the Mg x 609.79 Å line is found to be caused by a blend from the O iv 609.83 Å line. Conclusions. We present a unique analysis of the complex phenomenon called 'EIT/Coronal Wave', confirming its bimodal nature. We suggest that the disintegration of the dimming/CME and the CME-driven compression are either caused by a CME-CME interaction taking place in the low solar atmosphere or by an impulsive CME cavity overexpansion in the low solar atmosphere.

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“…It should be noted at this point that the name "EIT wave" is typically used for historical reasons. To reflect the uncertainty surrounding the physical interpretation of "EIT waves" we shall adopt the suggested nomenclature of Gallagher & Long (2010) and refer to these disturbances as coronal bright fronts (CBFs) throughout this paper.…”

Section: Introductionmentioning

confidence: 99%

“…A conclusive result has been hampered by the diffuse nature of CBFs and the relatively low temporal cadence of the observing instruments, both of which make it difficult to characterize their true nature. A full review of CBFs, their morphology, kinematics, relationship to other solar phenomena, and theoretical interpretations may be found in Wills-Davey & Attrill (2010) and Gallagher & Long (2010).…”

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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Large-scale Bright Fronts in the Solar Corona: A Review of “EIT waves”

Cited by 114 publications

References 87 publications

Large-scale Globally Propagating Coronal Waves

Large-scale Globally Propagating Coronal Waves

A coronal wave and an asymmetric eruptive filament in SUMER, CDS, EIT, and TRACE co-observations

Deceleration and dispersion of large-scale coronal bright fronts

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