Euv Wave Reflection From a Coronal Hole

Gopalswamy, Ν.; Yashiro, S.; Temmer, Manuela; Davila, J. M.; Thompson, W. T.; Jones, S. I.; McAteer, R. T. J.; Wüelser, Jean-Pierre; Freeland, S.; Howard, R. A.

doi:10.1088/0004-637x/691/2/l123

Cited by 155 publications

(168 citation statements)

References 31 publications

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“…This was first observed for a coronal EUV wave by Long et al (2008) and Veronig et al (2008), and studied in detail by Gopalswamy et al (2009). The reflected wave was clearly seen in difference images and in intensity profile stack plots (see Figure 30).…”

Section: Reflectionmentioning

confidence: 64%

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: Reflectionmentioning

confidence: 64%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

156

140

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“…They have a typical velocity of the order of 1000 km s −1 (Smith & Harvey 1971). Despite some apparent evidence that seems to support the fast-mode wave nature of EIT waves (e.g., Ballai et al 2005;Gopalswamy et al 2009;Olmedo et al 2012), a serious problem with the fast-mode wave model is that the EIT wave speed is typically ∼3 times slower than Moreton waves (Klassen et al 2000), and in some cases the EIT wave speed is only ∼80 km s −1 (Klassen et al 2000) or even ∼10 km s −1 (Zhukov et al 2009). Nitta et al (2013) claimed that the large-scale coronal propagating fronts have a mean wave speed of 644 km s −1 , which is comparable to that of Moreton waves.…”

Section: Discussionmentioning

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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“…The EUV wave simulations of Wang (2000) and Schmidt and Ofman (2010) showed wave reflection from the boundaries of coronal holes. The EUVI observations of the 19 May 2007 wave by Gopalswamy et al (2009) showed evidence of wave reflection from a small equatorial coronal hole. The speed of the reflected wave was similar to the speed of the incoming wave.…”

Section: Kinematics Amplitudes and Dispersionmentioning

confidence: 96%

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

2012

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A major, albeit serendipitous, discovery of the SOlar and Heliospheric Observatory mission was the observation by the Extreme Ultraviolet Telescope (EIT) of large-scale Extreme Ultraviolet (EUV) intensity fronts propagating over a significant fraction of the Sun's surface. These so-called EIT or EUV waves are associated with eruptive phenomena and have been studied intensely. However, their wave nature has been challenged by non-wave (or pseudo-wave) interpretations and the subject remains under debate. A string of recent solar missions has provided a wealth of detailed EUV observations of these waves bringing us closer to resolving their nature. With this review, we gather the current state-of-art knowledge in the field and synthesize it into a picture of an EUV wave driven by the lateral expansion of the CME. This picture can account for both wave and pseudo-wave interpretations of the observations, thus resolving the controversy over the nature of EUV waves to a large degree but not completely. We close with a discussion of several remaining open questions in the field of EUV waves research.

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Euv Wave Reflection From a Coronal Hole

Cited by 155 publications

References 31 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

On the Nature and Genesis of EUV Waves: A Synthesis of Observations from SOHO, STEREO, SDO, and Hinode (Invited Review)

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