Coronal Seismology Using Eit Waves: Estimation of the Coronal Magnetic Field Strength in the Quiet Sun

West, M. J.; Zhukov, A. N.; Dolla, L.; Rodriguez, L.

doi:10.1088/0004-637x/730/2/122

Cited by 47 publications

(48 citation statements)

References 63 publications

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“…This is in good agreement with the solar mean magnetic field (Chaplin et al, 2003). Using Hinode/EIS to measure coronal densities, West et al (2011) have found lower values of cor ≈ 0.7 G. This probably reflects the conditions of the deep activity minimum between the solar cycles 23 and 24. Using high-resolution TRACE EUV data, Ballai (2007) have derived the spatial distribution of cor (right panel in Figure 49).…”

Section: Global Coronal Seismologysupporting

confidence: 81%

“…Using high-resolution TRACE EUV data, Ballai (2007) have derived the spatial distribution of cor (right panel in Figure 49). They found field strengths ranging from 0.5 to 5.6 G, thus basically covering the whole range given by Warmuth and Mann (2005a) and West et al (2011). Recently, Long et al (2013) have used data from SDO/AIA and Hinode/EIS to derive cor = 2 -6 G in the low corona, while Kwon et al (2013b,a) found cor = 0.4 -2.5 G at larger heights of 1 -3 S using white-light signatures of coronal waves.…”

Section: Global Coronal Seismologymentioning

confidence: 71%

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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: Global Coronal Seismologysupporting

confidence: 81%

Section: Global Coronal Seismologymentioning

confidence: 71%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

156

140

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“…The difference in the asymptotic speeds of the "reflected" waves, slice "A" (380 versus 280 km s −1 ), of the meridional track toward the north, slice "B" (260 km s −1 ), and of the SW track (280 km s −1 ), which crossed the CH, seem to reflect the variations of the local fast-mode speed in the corona and are in agreement with global MHD models (e.g., Schmidt & Ofman 2010;Zhao et al 2011). Furthermore, these differences may provide good diagnostics for coronal seismology (e.g., Yang & Chen 2010;West et al 2011), but this topic is outside of Notes. Initial refers to the initial velocity; for slice A this refers to the velocity of the wave upon being launched by the cascading loops, and for slice B and slice C refers to the velocity of the primary wave soon after the flare onset.…”

Section: Conclusion and Discussionsupporting

confidence: 57%

SECONDARY WAVES AND/OR THE “REFLECTION” FROM AND “TRANSMISSION” THROUGH A CORONAL HOLE OF AN EXTREME ULTRAVIOLET WAVE ASSOCIATED WITH THE 2011 FEBRUARY 15 X2.2 FLARE OBSERVED WITHSDO/AIA ANDSTEREO/EUVI

Olmedo

Vourlidas

Zhang

et al. 2012

ApJ

109

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For the first time, the kinematic evolution of a coronal wave over the entire solar surface is studied. Full Sun maps can be made by combining images from the Solar Terrestrial Relations Observatory satellites, Ahead and Behind, and the Solar Dynamics Observatory, thanks to the wide angular separation between them. We study the propagation of a coronal wave, also known as the "Extreme Ultraviolet Imaging Telescope" wave, and its interaction with a coronal hole (CH) resulting in secondary waves and/or reflection and transmission. We explore the possibility of the wave obeying the law of reflection. In a detailed example, we find that a loop arcade at the CH boundary cascades and oscillates as a result of the extreme ultraviolet (EUV) wave passage and triggers a wave directed eastward that appears to have reflected. We find that the speed of this wave decelerates to an asymptotic value, which is less than half of the primary EUV wave speed. Thanks to the full Sun coverage we are able to determine that part of the primary wave is transmitted through the CH. This is the first observation of its kind. The kinematic measurements of the reflected and transmitted wave tracks are consistent with a fast-mode magnetohydrodynamic wave interpretation. Eventually, all wave tracks decelerate and disappear at a distance. A possible scenario of the whole process is that the wave is initially driven by the expanding coronal mass ejection and subsequently decouples from the driver and then propagates at the local fast-mode speed.

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“…West et al (2011)) used EIS density sensitive lines to get the coronal density over the QS where the 13 February 2009 wave propagated. From the propagation speed of the wave, the inferred density, and under the assumption that the observed disturbance was a fast-mode wave they obtained 0.7 ± 0.7 G for the magnetic field.…”

Section: Spectroscopic Observationsmentioning

confidence: 99%

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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Coronal Seismology Using Eit Waves: Estimation of the Coronal Magnetic Field Strength in the Quiet Sun

Cited by 47 publications

References 63 publications

Large-scale Globally Propagating Coronal Waves

Large-scale Globally Propagating Coronal Waves

SECONDARY WAVES AND/OR THE “REFLECTION” FROM AND “TRANSMISSION” THROUGH A CORONAL HOLE OF AN EXTREME ULTRAVIOLET WAVE ASSOCIATED WITH THE 2011 FEBRUARY 15 X2.2 FLARE OBSERVED WITHSDO/AIA ANDSTEREO/EUVI

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

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