Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. I. Reconciliation of “EIT Waves”, Type II Radio Bursts, and Leading Edges of CMEs

Grechnev, V. V.; Uralov, A. M.; Chertok, I. M.; Kuzmenko, I. V.; Afanasyev, A. N.; Meshalkina, N. S.; Kalashnikov, S. S.; Kubo, Yûki

doi:10.1007/s11207-011-9780-z

Cited by 71 publications

(114 citation statements)

References 70 publications

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“…Dome-shaped coronal waves with an almost circular appearance in EUV and soft X-ray observations have been reported by several authors (e.g. Narukage et al, 2004;Veronig et al, 2010;Kozarev et al, 2011;Ma et al, 2011;Grechnev et al, 2011a;Li et al, 2012;Cheng et al, 2012), while numerical simulations also confirm this aspect (Warmuth, 2015, and references therein). If the model is accurate enough, the intersection of a spherical shock-front with the solar sphere would coincide with the measured traces in the chromospheric and transition region, sector by sector, if a common shock wavefront is responsible for all the effects.…”

Section: About the Correspondence Between The Analyzed Regimessupporting

confidence: 62%

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: 62%

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

et al. 2016

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“…This can be interpreted as a line-of-sight integration effect: the leading front represents the leading edge of the 3D wavefront at larger heights where a large column length contributes to emission, while the second front comes from the low parts of the wavefront where emission measure is highest due to the density stratification. This is illustrated in Figure 10 in Grechnev et al (2011b).…”

Section: Multiple Wavefrontsmentioning

confidence: 90%

“…This is shown by the power-law indices, which have a typical value of ≈ 0.6 for both Moreton waves and combined fronts (Warmuth et al, 2004a;Warmuth and Mann, 2011). Such power-laws are predicted for the distance-time curves of freely propagating shock waves (Grechnev et al, 2008(Grechnev et al, , 2011b according to the Sedov solution (Sedov, 1959). Note that Moreton fronts actually tend to lag some ≈ 20 -30 Mm behind the coronal EUV and SXR wavefronts (Warmuth, 2010).…”

Section: Deceleration Of a Single Disturbancementioning

confidence: 91%

“…Analytical models based on fast-mode shocks have successfully reproduced the kinematics of coronal waves (Grechnev et al, 2008;Temmer et al, 2009;Grechnev et al, 2011b;Afanasyev and Uralov, 2011;Grechnev et al, 2011a;Temmer et al, 2013), while in the framework of numerical A more shallow signature in He i is generated in front of the main perturbation by increased irradiation, heat flux, and possibly accelerated particles from the higher parts of the inclined shock front. At the quasi-perpendicular part of the shock, a type II burst is generated.…”

Section: Small-scale Ejectamentioning

confidence: 99%

“…This scenario is still the basis of the fast-mode wave/shock model of coronal waves (see e.g., Vršnak and Lulić, 2000a,b;Warmuth et al, 2004b;Vršnak and Cliver, 2008;Grechnev et al, 2011b;Warmuth and Mann, 2011). This model postulates the following:…”

Section: Small-scale Ejectamentioning

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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Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. III. Shock-Associated CME/EUV Wave in an Event with a Two-Component EUV Transient

Grechnev

Afanasyev

Uralov

et al. 2011

Energy Storage and Release Through the Solar Activity Cycle

Self Cite

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On 17 January 2010, STEREO-B observed in extreme ultraviolet (EUV) and white light a large-scale dome-shaped expanding coronal transient with perfectly connected off-limb and on-disk signatures. Veronig et al. (2010, ApJL 716, 57) concluded that the dome was formed by a weak shock wave. We have revealed two EUV components, one of which corresponded to this transient. All of its properties found from EUV, white light, and a metric type II burst match expectations for a freely expanding coronal shock wave including correspondence to the fast-mode speed distribution, while the transient sweeping over the solar surface had a speed typical of EUV waves. The shock wave was presumably excited by an abrupt filament eruption. Both a weak shock approximation and a power-law fit match kinematics of the transient near the Sun. Moreover, the power-law fit matches expansion of the CME leading edge up to 24 solar radii. The second, quasi-stationary EUV component near the dimming was presumably associated with a stretched CME structure; no indications of opening magnetic fields have been detected far from the eruption region.

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Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. I. Reconciliation of “EIT Waves”, Type II Radio Bursts, and Leading Edges of CMEs

Cited by 71 publications

References 70 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

Coronal Shock Waves, EUV Waves, and Their Relation to CMEs. III. Shock-Associated CME/EUV Wave in an Event with a Two-Component EUV Transient

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