<i>HINODE</i>/XRT AND<i>STEREO</i>OBSERVATIONS OF A DIFFUSE CORONAL “WAVE”-CORONAL MASS EJECTION-DIMMING EVENT

Attrill, G. D. R.; Engell, Alexander; Wills-Davey, M. J.; Grigis, P. C.; Testa, Paola

doi:10.1088/0004-637x/704/2/1296

Cited by 51 publications

(45 citation statements)

References 87 publications

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“…This behavior was supported by observations of a coronal EUV wave and associated CME that were consistent with this scenario The reconnection front model has been criticized based on magnetic field extrapolations that showed that in the event studied by Attrill et al (2007), reconnection could not have happened with quiet sun fields (Delannée, 2009). Attrill et al (2009) replied to this critique that large-scale fields would not inhibit reconnection with small-scale quiet sun fields since the latter become open during a CME eruption. However, doubts remain whether a reconnection front can actually propagate globally.…”

Section: Current Shell Modelmentioning

confidence: 72%

“…Based on XRT intensity ratios, the perturbation was interpreted as a fast-mode shock. Attrill et al (2009) studied a coronal wave event that was observed with XRT and EUVI. They found that the strongest parts of the perturbation are cospatial in all wavelengths, and that the CME flanks as observed by STEREO/COR1 map back to the wavefronts.…”

Section: Soft X-rays (Sxr)mentioning

confidence: 99%

“…They found that the strongest parts of the perturbation are cospatial in all wavelengths, and that the CME flanks as observed by STEREO/COR1 map back to the wavefronts. Attrill et al (2009) concluded that the wavefront is actually the expanding CME shell. In a different event, Delannée et al (2014) observed a coronal wave with EUVI and XRT data.…”

Section: Soft X-rays (Sxr)mentioning

confidence: 99%

“…Using high-cadence EUV imaging, several authors have reported events where the coronal waves were cospatial to or remained closely attached to the expanding CME flanks (Chen, 2009;Attrill et al, 2009;Dai et al, 2010).…”

Section: Coronal Mass Ejections (Cmes)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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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: Current Shell Modelmentioning

confidence: 72%

Section: Soft X-rays (Sxr)mentioning

confidence: 99%

Section: Soft X-rays (Sxr)mentioning

confidence: 99%

Section: Coronal Mass Ejections (Cmes)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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“…(Liewer et al, 2009). The associated EUV dimming and EUV wave caused by the filament eruption was also analyzed (Attrill et al, 2009). Plasma motion and heating up to T e = 9 MK was observed for the same flare around 13:00 UT (Hara et al, 2011).…”

Section: Tests With Stereoscopic Observationsmentioning

confidence: 98%

A Nonlinear Force-Free Magnetic Field Approximation Suitable for Fast Forward-Fitting to Coronal Loops. III. The Free Energy

Aschwanden

2012

Sol Phys

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An analytical approximation of a nonlinear force-free magnetic field (NLFFF) solution was developed in Paper I, while a numerical code that performs fast forward-fitting of this NLFFF approximation to a line-of-sight magnetogram and coronal 3D loops has been described and tested in Paper II. Here we calculate the free magnetic energy E free = E N − E P , i.e., the difference of the magnetic energies between the nonpotential field and the potential field. A second method to estimate the free energy is obtained from the mean misalignment angle change ∆µ = µ P − µ N between the potential and nonpotential field, which scales as E free /E P ≈ tan 2 (∆µ). For four active regions observed with STEREO in 2007 we find free energies in the range of q free = (E free /E P ) ≈ 1% − 10%, with an uncertainty of less than ±2% between the two methods, while the free energies obtained from 11 other NLFFF codes exhibit a larger scatter of order ≈ ±10%. We find also a correlation between the free magnetic energy and the GOES flux of the largest flare that occurred during the observing period, which can be quantified by an exponential relationship, F GOES ∝ exp (q free /0.015), implying an exponentiation of the dissipated currents.

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