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, V. V.; Afanasyev, A. N.; Uralov, A. M.; Chertok, I. M.; Еселевич, М.; Еселевич, В. Г.; Rudenko, G. V.; Kubo, Yûki

doi:10.1007/978-1-4614-4403-9_11

Cited by 4 publications

(11 citation statements)

References 42 publications

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“…Note that this is consistent with the finding that metric type II bursts (which often show quasiradial propagation) tend to be faster than the laterally propagating associated waves (Warmuth, 2010;Ma et al, 2011;Grechnev et al, 2011a). The different expansion velocities could either reflect the increase of the fast-mode speed with height in the low corona (a wave or shock would speed up under these circumstances; see e.g., Grechnev et al, 2011a) or a scenario where the upper part of the disturbance is continuously driven by the erupting CME, while its flanks are freely propagation (e.g., Veronig et al, 2010).…”

Section: Lateral and Radial Kinematicssupporting

confidence: 90%

“…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%

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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: Lateral and Radial Kinematicssupporting

confidence: 90%

Section: Small-scale Ejectamentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

163

140

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“…If the large-scale v fast distribution is strongly inhomogeneous (e.g. because of the presence of a large coronal hole), then the orientation of the axis gradually displaces toward the region of a higher v fast (Grechnev et al, 2011a(Grechnev et al, , 2013a. The shock front is "hard" like an ocean tube wave, being governed by the global wave expansion and does not depend on local inhomogeneities in the v fast distribution.…”

Section: Euv Wavementioning

confidence: 99%

“…The stronger near-surface retardation causes a tilt of the shock front sometimes observed (Hudson et al, 2003;Warmuth et al, 2004b). Local inhomogeneities in the v fast distribution over the solar surface determine the brightness of the EUV wave (Grechnev et al, 2011a), while larger inhomogeneities affect its propagation velocity and cause its reflection and refraction (e.g. Veronig et al, 2008;Gopalswamy et al, 2009;Grechnev et al, 2011b).…”

Section: Euv Wavementioning

confidence: 99%

Multi-instrument view on solar eruptive events observed with the Siberian Radioheliograph: From detection of small jets up to development of a shock wave and CME

Grechnev

Lesovoi

Kochanov

et al. 2018

Journal of Atmospheric and Solar-Terrestrial Physics

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The first 48-antenna stage of the Siberian Radioheliograph (SRH) started single-frequency test observations early in 2016, and since August 2016 it routinely observes the Sun at several frequencies in the 4-8 GHz range with an angular resolution of 1-2 arc minutes and an imaging interval of about 12 seconds. With limited opportunities of the incomplete antenna configuration, a high sensitivity of about 100 Jy allows the SRH to contribute to the studies of eruptive phenomena along three lines. First, some eruptions are directly visible in SRH images. Second, some small eruptions are detectable even without a detailed imaging information from microwave depressions caused by screening the background emission by cool erupted plasma. Third, SRH observations reveal new aspects of some events to be studied with different instruments. We focus on an eruptive C2.2 flare on 16 March 2016 around 06:40, one of the first flares observed by the SRH. Proceeding from SRH observations, we analyze this event using extreme-ultraviolet, hard X-ray, white-light, and metric radio data. An eruptive prominence expanded, brightened, and twisted, which indicates a time-extended process of the flux-rope formation together with the development of a large coronal mass ejection (CME). The observations rule out a passive role of the prominence in the CME formation. The abrupt prominence eruption impulsively excited a blast-wave-like shock, which appeared during the microwave burst and was manifested in an "EUV wave" and Type II radio burst. The shock wave decayed and did not transform into a bow shock because of the low speed of the CME. Nevertheless, this event produced a clear proton enhancement near Earth. Comparison with our previous studies of several events confirms that the impulsive-piston shock-excitation scenario is typical of various events.

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“…The shock wave initially propagated faster at the nose than at the flanks, which corresponds to what were conceived as EIT waves. The observed kinematic behaviors have been partially reproduced in theory and models (Zhao et al, 2011;Grechnev et al, 2011;Temmer, Vrsnak, and Veronig, 2013) of the 17 January 2010 event reported by Veronig et al (2010). For the 13 June 2010 event, Kouloumvakos et al (2014) concluded that both the nose and flank of the CME drove the shock.…”

Section: Discussionmentioning

confidence: 60%

The Relation Between Large-Scale Coronal Propagating Fronts and Type II Radio Bursts

et al. 2014

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Large-scale, wave-like disturbances in extreme-ultraviolet (EUV) and type II radio bursts are often associated with coronal mass ejections (CMEs). Both phenomena may signify shock waves driven by CMEs. Taking EUV full-disk images at an unprecedented cadence, the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory has observed the so-called EIT waves or large-scale coronal propagating fronts (LCPFs) from their early evolution, which coincides with the period when most metric type II bursts occur. This article discusses the relation of LCPFs as captured by AIA with metric type II bursts. We show examples of type II bursts without a clear LCPF and fast LCPFs without a type II burst. Part of the disconnect between the two phenomena may be due to the difficulty in identifying them objectively. Furthermore, it is possible that the individual LCPFs and type II bursts may reflect different physical processes and external factors. In particular, the type II bursts that start at low frequencies and high altitudes tend to accompany an extended arcshaped feature, which probably represents the 3D structure of the CME and the shock wave around it, rather than its near-surface track, which has usually been identified with EIT waves. This feature expands and propagates toward and beyond the limb. These events may be characterized by stretching of field lines in the radial direction, and be distinct from other LCPFs, which may be explained in terms of sudden lateral expansion of the coronal volume. Neither LCPFs nor type II bursts by themselves serve as necessary conditions for coronal shock waves, but these phenomena may provide useful information on the early evolution of the shock waves in 3D when both are clearly identified in eruptive events.

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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

Cited by 4 publications

References 42 publications

Large-scale Globally Propagating Coronal Waves

Large-scale Globally Propagating Coronal Waves

Multi-instrument view on solar eruptive events observed with the Siberian Radioheliograph: From detection of small jets up to development of a shock wave and CME

The Relation Between Large-Scale Coronal Propagating Fronts and Type II Radio Bursts

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