Evolution of Two EIT/Hα Moreton Waves

Warmuth, A.; Vršnak, Bojan; Auraß, H.; Hanslmeier, A.

doi:10.1086/324055

Cited by 171 publications

(190 citation statements)

References 17 publications

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“…Actually, the pulse broadening and amplitude decrease was first measured quantitatively for Hα Moreton wave signatures (Warmuth et al, 2001(Warmuth et al, , 2004a Figure 26) and was subsequently found in all Moreton events (Warmuth, 2010). Therefore, the three basic characteristics of the coronal disturbances associated with Moreton waves are deceleration (see Section 4.2), pulse widening, and amplitude decrease.…”

Section: Perturbation Profilementioning

confidence: 87%

“…So far, we have considered mean or linear wave speeds (i.e., obtained from a linear fit of the measured distances). However, Warmuth et al (2001) found that Moreton waves do not propagate at constant speeds but instead showed pronounced deceleration. Additionally, they could show that Moreton and EIT wavefronts are nearly cospatial and show similarities in morphology, which strongly suggests a single physical disturbance that generates the different signatures.…”

Section: Deceleration Of a Single Disturbancementioning

confidence: 97%

“…Distances on the disk are measured along great circles emanating from the radiant point (cf. Thompson et al, 1999;Warmuth et al, 2001), which accounts for foreshortening, or less frequently via Huygens plotting (cf. Wills-Davey and Hudson et al, 2003), which accounts for changes in propagation direction.…”

Section: Kinematicsmentioning

confidence: 99%

“…An alternative method is to measure intensity profiles and use the detected pulses to derive speeds (cf. Warmuth et al, 2001). The latter method is now being used extensively for wave events observed at high cadences with SDO/AIA (e.g., Long et al, 2014).…”

Section: Kinematicsmentioning

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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Section: Perturbation Profilementioning

confidence: 87%

Section: Deceleration Of a Single Disturbancementioning

confidence: 97%

Section: Kinematicsmentioning

confidence: 99%

Section: Kinematicsmentioning

confidence: 99%

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Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

163

140

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“…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). The non-wave interpretation refers to EUV waves as signatures of a current shell or successive restructuring of field lines during a CME (Delannée 2000;Delannée et al 2008;Chen et al 2002;Attill et al 2007;Schrijver et al 2011).…”

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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Solar Flares — Observations and Theory

Vršnak

2005

Solar Magnetic Phenomena

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Evolution of Two EIT/Hα Moreton Waves

Cited by 171 publications

References 17 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

Solar Flares — Observations and Theory

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