Solar Phenomena Associated with “EIT Waves”

Biesecker, D. A.; Myers, D. C.; Thompson, B. J.; Hammer, D.; Vourlidas, A.

doi:10.1086/339402

Cited by 245 publications

(260 citation statements)

References 22 publications

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“…A recent study by Nitta et al (2013) found a higher association of AIA waves with type II bursts, namely 54%. This higher percentage could be due to a selection effect, since the AIA wave sample did not include slow and weak disturbances that are part of the EIT wave catalog used by Biesecker et al (2002). This is consistent with the finding that the median speed of AIA waves without type II bursts was somewhat lower than the speed of the burst-associated waves (550 versus 650 km s -1 ).…”

Section: Metric Type II Radio Burstssupporting

confidence: 77%

“…The converse is not true, since only 21% of EIT waves are accompanied by type II bursts (Biesecker et al, 2002). A recent study by Nitta et al (2013) found a higher association of AIA waves with type II bursts, namely 54%.…”

Section: Metric Type II Radio Burstsmentioning

confidence: 95%

“…A diffuse bright front is propagating quasi-isotropically through the corona. A small subset (7%) of events, the so called S-waves (Biesecker et al, 2002;Thompson and Myers, 2009) or brow waves (Gopalswamy et al, 2000a) are characterized by arc-like, sharp fronts (see Figure 5b) that later decay to the more usual diffuse fronts Warmuth et al, 2004b). There are also many propagating disturbances that have been tentatively identified as waves, but which do not propagate to large distances and which show rather irregular fronts (cf.…”

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confidence: 99%

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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: Metric Type II Radio Burstssupporting

confidence: 77%

Section: Metric Type II Radio Burstsmentioning

confidence: 95%

mentioning

confidence: 99%

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Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

168

140

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“…Following Chen & Fang (2012), we use "EIT waves" for the slower type of EUV waves specifically. Biesecker et al (2002) did a statistical study of EIT waves observed by SOHO/EIT (195 Å) telescope and found that some of the EIT waves have sharp, bright features, which they called "S-waves." These S-waves may be the signature of Moreton 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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“…Such large-scale events as EIT wave connect to flares or CME (e.g. Chertok & Grechnev (2003), Biesecker et al (2002), Wills-Davey et al (2007)). …”

Section: Introductionmentioning

confidence: 99%

Coronal waves in coronal loops during non-flare stage

Prosovetsky¹

2008

Proc. IAU

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Abstract. Using SOHO/EIT Fe XII λ195Å observations the new type of oscillations in coronal loops was detected. The oscillation corresponds to wave propagated to outer area of atmosphere of active area. As opposed to most kind of oscillations associated with coronal loops the waves are observed at non-flare stage of active areas evolution. Velocities of the wave propagation were 8-20 km s −1 and had quasi-perpendicular direction with magnetic field. Such waves were detected in active areas located on solar disk and loops structures outside solar limb. Investigation of EIT data shows the waves are not result of changes of topology of a magnetic field and loops configuration. The nature and probable sources of waves are discussed.

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Solar Phenomena Associated with “EIT Waves”

Cited by 245 publications

References 22 publications

Large-scale Globally Propagating Coronal Waves

Large-scale Globally Propagating Coronal Waves

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

Coronal waves in coronal loops during non-flare stage

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