<i>STEREO</i>OBSERVATIONS OF FAST MAGNETOSONIC WAVES IN THE EXTENDED SOLAR CORONA ASSOCIATED WITH EIT/EUV WAVES

Kwon, Ryun-Young; Ofman, L.; Olmedo, Oscar; Kramar, Maxim; Davila, J. M.; Thompson, B. J.; Cho, Kyung-Suk

doi:10.1088/0004-637x/766/1/55

Cited by 53 publications

(68 citation statements)

References 48 publications

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“…The overall correspondence is in agreement with the unified picture of EUV waves synthesized from a series of findings by Patsourakos and Vourlidas (2012), whereby the inner brighter front is attributed to the expanding CME loops or bubble and the outer fainter front is the fast-mode wave ahead of the CME flanks and leading edge. Further agreement is found with the findings by Kwon et al (2013), who noted that the wavefront in the upper (white-light) solar corona turns out to be the counterpart of the EUV wave.…”

Section: About the Correspondence Between The Analyzed Regimessupporting

confidence: 91%

Moreton and EUV Waves Associated with an X1.0 Flare and CME Ejection

et al. 2016

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Several other phenomena took place in connection with this event, such as low coronal waves and a coronal mass ejection (CME). We analyze the association between the Moreton wave and the EUV signatures observed with the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory. These include their low-coronal surface-imprint, and the signatures of the full wave and shock dome propagating outward in the corona. We also study their relation to the whitelight CME. We perform a kinematic analysis by tracking the wavefronts in several directions. This analysis reveals a high-directional dependence of accelerations and speeds determined from data at various wavelengths. We speculate that a region of open magnetic field lines northward of our defined radiant point sets favorable conditions for the propagation of a coronal magnetohydrodynamic shock in this direction. The hypothesis that the Moreton wavefront is produced by a coronal shock-wave that pushes the chromosphere downward is supported by the high compression ratio in that region. Furthermore, we propose a 3D geometrical model to explain the observed wavefronts as the chromospheric and low-coronal traces of an expanding and outward-traveling bubble intersecting the Sun. The results of the model are in agreement with the coronal shock-wave being generated by a 3D piston that expands at the speed of the associated rising filament. The piston is attributed to the fast ejection of the filament -CME ensemble, also consistent with the good match between the speed profiles of the low-coronal and white-light shock-waves.

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Section: About the Correspondence Between The Analyzed Regimessupporting

confidence: 91%

Moreton and EUV Waves Associated with an X1.0 Flare and CME Ejection

et al. 2016

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“…Optically thin emission is weighted with density squared, so EUV and SXR emission is strongly concentrated towards the low corona, and this is where the strongest signal will be detected. Recently, white-light signatures were detected with STEREO/COR1 that were identified as the continuation of the EUV wavefronts into the higher corona (Kwon et al, 2013b). These observations have extended the maximum height at which signatures of coronal waves were detected to 1400 Mm.…”

Section: Propagation Heights and 3d Structurementioning

confidence: 90%

“…This has first been achieved with COR1 and EUVI aboard the STEREO spacecraft. Recently, Kwon et al (2013b) identified an laterally propagating wavefront-like feature seen in STEREO/COR1 as the upper coronal counterpart of an EUV coronal wave propagating on the solar disk (see Figure 8). This represents the first unambiguous detection of a coronal wave in the upper corona.…”

Section: White Lightmentioning

confidence: 99%

“…Recently, stationary EUV fronts were found to be located at the footpoints of coronal streamers that were deflected and excited to oscillate when the upper parts of a coronal EUV wave passed through them (Kwon et al, 2013b). The spatial and temporal characteristics of the fronts suggests that they are generated by the bouncing back of the deflected streamer, and not by magnetic reconfiguration associated with the erupting CME.…”

Section: Stationary Brighteningsmentioning

confidence: 99%

“…Recently, Kwon et al (2013b) showed that coronal streamers were deflected and excited to oscillate after the higher parts of a coronal EUV wave passed through them. The oscillation was identified as a quickly damped kink mode wave (e.g., Liu et al, 2012).…”

Section: Excitation Of Oscillationsmentioning

confidence: 99%

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Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

169

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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Comparison of the coronal mass ejection shock acceleration of three widespread SEP events during solar cycle 24

et al. 2017

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We studied three solar energetic particle (SEP) events observed on 14 August 2010, 3 November 2011, and 5 March 2013 by Solar Terrestrial Relations Observatory (STEREO) A, B, and near‐Earth (L1) spacecraft with a longitudinal distribution of particles >90°. Using a forward modeling method combined with extreme ultraviolet and white‐light images, we determined the angular extent of the shock, the time and location (cobpoint) of the shock intersection with the magnetic field line connecting to each spacecraft, and compute the shock speed at the cobpoint of each spacecraft. We then examine whether the observations of SEPs at each spacecraft were accelerated and injected by the spatially extended shocks or whether another mechanism such as cross‐field transport is required for an alternative explanation. Our analyses results indicate that the SEPs observed at the three spacecraft on 3 November, STEREO B (STB) and L1 on 14 August, and the 5 March SEP event at STEREO A (STA) can be explained by the direct shock acceleration. This is consistent with the observed significant anisotropies, short time delays between particle release times and magnetic connection times, and sharp rises in the SEP time profiles. Cross‐field diffusion is the likely cause for the 14 August SEP event observed by STA and the 5 March SEPs observed by STB and L1 spacecraft, as particle observations featured weak electron aniotropies and slow rising intensity profiles. Otherwise, the wide longitudinal spread of these SEP increases would require an existence of a circumsolar shock, which may not be a correct assumption in the corona and heliosphere.

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STEREOOBSERVATIONS OF FAST MAGNETOSONIC WAVES IN THE EXTENDED SOLAR CORONA ASSOCIATED WITH EIT/EUV WAVES

Cited by 53 publications

References 48 publications

Moreton and EUV Waves Associated with an X1.0 Flare and CME Ejection

Moreton and EUV Waves Associated with an X1.0 Flare and CME Ejection

Large-scale Globally Propagating Coronal Waves

Comparison of the coronal mass ejection shock acceleration of three widespread SEP events during solar cycle 24

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