On the Origin of the Solar Moreton Wave of 2006 December 6

Balasubramaniam, Krishnan; Cliver, E. W.; Pevtsov, Alexei A.; Temmer, Manuela; Henry, T. W.; Hudson, H. S.; Imada, Shinsuke; Ling, A. G.; Moore, Ronald L.; Muhr, N.; Neidig, D. F.; Petrie, Gordon; Veronig, Astrid; Vršnak, Bojan; White, S. M.

doi:10.1088/0004-637x/723/1/587

Cited by 47 publications

(68 citation statements)

References 125 publications

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“…High cadence movies of EUV waves observed either on disk or off-limb show that the first instances of a wave front are seen ahead of the flanks of the rising and expanding loops of the early CME (e.g., Long et al, 2008;Patsourakos et al, 2009;Kienreich, Temmer, and Veronig, 2009;Patsourakos and Vourlidas, 2009;Patsourakos, Vourlidas, and Kliem, 2010;Patsourakos, Vourlidas, and Stenborg, 2010;Veronig et al, 2010;Liu et al, 2010;Ma et al, 2011;Kozarev et al, 2011;Schrijver et al, 2011). Disk observations of Moreton waves show a similar trend with the first wave fronts seen in the AR periphery and never in its core (e.g., Balasubramaniam et al, 2010;Temmer et al, 2009;Muhr et al, 2010). Based on off-limb STEREO and AIA observations of impulsive events (e.g., Patsourakos, Vourlidas, and Kliem, 2010;Patsourakos, Vourlidas, and Stenborg, 2010;Kozarev et al, 2011;Ma et al, 2011;Cheng et al, 2012), the following evolutionary pattern is seen (Figure 19 and 21).…”

Section: The Genesis Of Euv Wavesmentioning

confidence: 75%

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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Section: The Genesis Of Euv Wavesmentioning

confidence: 75%

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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“…Vršnak et al, 2002b;Warmuth et al, 2004a;Warmuth, 2010;Balasubramaniam et al, 2010). In all of these events, the wavefronts recorded in the different spectral bands are consistent with a decelerating disturbance (see left panel of Figure 23 for an example).…”

Section: Deceleration Of a Single Disturbancementioning

confidence: 80%

“…Warmuth et al, 2004a;Narukage et al, 2008;Muhr et al, 2010;Balasubramaniam et al, 2010;Warmuth, 2010;Asai et al, 2012;Francile et al, 2013). The initial velocities are in the range of 600 -1200 km s -1 and decline to ≈ 500 km s -1 before the Hα wave signatures vanish.…”

Section: Deceleration Of a Single Disturbancementioning

confidence: 98%

“…The propagation of Moreton waves is almost always confined to a certain angular extent, on average ≈ 90° (Smith and Harvey, 1971;Warmuth et al, 2004a;Zhang et al, 2011, see right of Figure 17 for an example). Only three events have been reported where Moreton fronts were observed to propagate in a full (or broken) circle like the "textbook" EUV waves (Pick et al, 2005;Liu et al, 2006;Muhr et al, 2010;Balasubramaniam et al, 2010). Interestingly, the associated EUV waves span an angle that is on average twice as larger as for Moreton waves .…”

Section: Frequency Of Occurrencementioning

confidence: 99%

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Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

163

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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“…Ramsey. Figure 10 shows an excellent recent example (SOL2006-12-06T18:40; Balasubramaniam et al 2010).…”

Section: Chromospheric Wavesmentioning

confidence: 99%

Global Properties of Solar Flares

2011

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This article broadly reviews our knowledge of solar flares. There is a particular focus on their global properties, as opposed to the microphysics such as that needed for magnetic reconnection or particle acceleration as such. Indeed solar flares will always remain in the domain of remote sensing, so we cannot observe the microscales directly and must understand the basic physics entirely via the global properties plus theoretical inference. The global observables include the general energetics-radiation in flares and mass loss in coronal mass ejections (CMEs)-and the formation of different kinds of ejection and global wave disturbance: the type II radio-burst exciter, the Moreton wave, the EIT "wave", and the "sunquake" acoustic waves in the solar interior. Flare radiation and CME kinetic energy can have comparable magnitudes, of order 10 32 erg each for an X-class event, with the bulk of the radiant energy in the visible-UV continuum. We argue that the impulsive phase of the flare dominates the energetics of all of these manifestations, and also point out that energy and momentum in this phase largely reside in the electromagnetic field, not in the observable plasma.

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On the Origin of the Solar Moreton Wave of 2006 December 6

Cited by 47 publications

References 125 publications

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

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

Large-scale Globally Propagating Coronal Waves

Global Properties of Solar Flares

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