Are “EIT Waves” Fast‐Mode MHD Waves?

Wills-Davey, M. J.; DeForest, C. E.; Stenflo, J. O.

doi:10.1086/519013

Cited by 122 publications

(117 citation statements)

References 48 publications

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“…Another surprising finding was the large range of speeds, ranging from a few 10 km s -1 up to 700 km s -1 (Thompson and Myers, 2009). This large spread has been interpreted as evidence against the fast-mode wave model (Wills-Davey et al, 2007). It should be noted, however, that the very low speeds are associated with weak and irregular events (cf.…”

Section: Mean Velocities Of Different Signaturesmentioning

confidence: 99%

“…This will be discussed further in Section 6.3. -Davey et al (2007) argued that the fast-mode wave model fails to reproduce several observational constraints, in particular i) the large variation of EIT wave speeds both between different events (cf. Thompson and Myers, 2009) and within one wave event (Wills-Davey and , ii) the fact that a significant fraction of these speeds is below the coronal sound speed (i.e., < 185 km s -1 for a coronal temperature of 1.5 MK), and iii) the observation that EIT waves retain their coherence over large distances.…”

Section: Small-scale Ejectamentioning

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.…”

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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: Mean Velocities Of Different Signaturesmentioning

confidence: 99%

Section: Small-scale Ejectamentioning

confidence: 99%

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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“…Several models have been proposed that can be grouped into wave, non-wave and hybrid wave interpretations. The wave interpretation considers that EUV waves are real waves, including fast-mode magnetohydrodynamic (MHD) waves or shock waves (e.g., Wang 2000;Wu 2001;Schmidt & Ofman 2010), slow-mode MHD waves (Wang et al 2009a) and soliton waves (Wills-Davey et al 2007). Among them, the fast-mode MHD wave model is the most popular and supported by many observations (Warmuth et al 2001;Veronig et al 2008;Kienreich et al 2009;Gopalswamy et al 2009;Patsourakos & Vourlidas 2009;Liu et al 2011;Zheng et al 2011;Asai et al 2012).…”

Section: Introductionmentioning

confidence: 99%

SDO/AIA and Hinode/EIS observations of interaction between an EUV wave and active region loops

Liu¹,

Zhang²,

Li³

et al. 2012

Proc. IAU

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We present detailed analysis of an extreme ultraviolet (EUV) wave and its interaction with active region (AR) loops observed by the Solar Dynamics Observatory/Atmospheric Imaging Assembly and the Hinode EUV Imaging Spectrometer (EIS). This wave was initiated from AR 11261 on 2011 August 4 and propagated at velocities of 430-910 km s −1 . It was observed to traverse another AR and cross over a filament channel on its path. The EUV wave perturbed neighboring AR loops and excited a disturbance that propagated toward the footpoints of these loops. EIS observations of AR loops revealed that at the time of the wave transit, the original redshift increased by about 3 km s −1 , while the original blueshift decreased slightly. After the wave transit, these changes were reversed. When the EUV wave arrived at the boundary of a polar coronal hole, two reflected waves were successively produced and part of them propagated above the solar limb. The first reflected wave above the solar limb encountered a large-scale loop system on its path, and a secondary wave rapidly emerged 144 Mm ahead of it at a higher speed. These findings can be explained in the framework of a fast-mode magnetosonic wave interpretation for EUV waves, in which observed EUV waves are generated by expanding coronal mass ejections.

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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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Are “EIT Waves” Fast‐Mode MHD Waves?

Cited by 122 publications

References 48 publications

Large-scale Globally Propagating Coronal Waves

Large-scale Globally Propagating Coronal Waves

SDO/AIA and Hinode/EIS observations of interaction between an EUV wave and active region loops

Coronal waves in coronal loops during non-flare stage

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