Relation between a Moreton Wave and an EIT Wave Observed on 1997 November 4

Eto, Shigeru; Isobe, Hiroaki; Narukage, Noriyuki; Asai, Ayumi; Morimoto, Taro; Thompson, B. J.; Yashiro, S.; Wang, Tongjiang; Kitai, Reizaburo; Kurokawa, H.; Shibata, Kazunari

doi:10.1093/pasj/54.3.481

Cited by 131 publications

(133 citation statements)

References 20 publications

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“…However, other authors (Narukage et al 2002;Muhr et al 2010) suggest that Moreton waves are generated prior to the flare ignition, which supports hypothesis H2. The onset time obtained in this paper from curve A indicates that the Moreton wave event is generated close to the flare explosive phase (Smith & Harvey 1971).…”

Section: The Kinematics Of the Moreton Wave Eventsupporting

confidence: 61%

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HαMoreton waves observed on December 06, 2006

Francile

Costa

Luoni

et al. 2013

A&A

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Context. We present high temporal resolution observations of a Moreton wave event detected with the Hα Solar Telescope for Argentina (HASTA) in the Hα line 656.3 nm, on December 6, 2006. Aims. The aim is to contribute to the discussion about the nature and triggering mechanisms of Moreton wave events. Methods. We describe the HASTA telescope capabilities and the observational techniques. We carried out a detailed analysis to determine the flare onset, the radiant point location, the kinematics of the disturbance and the activation time of two distant filaments. We used a 2D reconstruction of the HASTA and corresponding TRACE observations, together with conventional techniques, to analyze the probable origin of the phenomenon. Results. The kinematic parameters and the probable onset time of the Moreton wave event are determined. A small-scale ejectum and the winking of two remote filaments are analyzed to discuss their relation with the Moreton disturbance. Conclusions. The analysis of the Moreton wave event favors the hypothesis that the phenomenon can be described as the chromospheric imprint of a single fast coronal shock triggered from a single source in association with a coronal mass ejection. Its onset time is concurrent with a Lorentz force peak measured in the photosphere, as stated by other authors. However, the existence of multiple shock waves that were generated almost simultaneously cannot be discarded.

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Section: The Kinematics Of the Moreton Wave Eventsupporting

confidence: 61%

“…2a). We analyzed the winking of the NF and SF to determine their activation times and their possible correlation with the Moreton wavefront passage (Smith & Harvey 1971;Okamoto et al 2004;Eto et al 2002;Gilbert et al 2008). …”

Section: D Analysis Of the Filament Winkingmentioning

confidence: 99%

HαMoreton waves observed on December 06, 2006

Francile

Costa

Luoni

et al. 2013

A&A

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“…These disturbances produce large-amplitude oscillations with velocity amplitudes of 20 km s −1 or higher. Observations of large-amplitude oscillations in filaments are rare, although in recent years with the help of new observational capabilities more detections have been reported (Eto et al, 2002;Okamoto et al, 2004;Jing et al, 2003Jing et al, , 2006Gilbert et al, 2008). Also, theoretical modeling of such events is lacking.…”

Section: Overviewmentioning

confidence: 99%

Physics of Solar Prominences: II—Magnetic Structure and Dynamics

et al. 2010

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Observations and models of solar prominences are reviewed. We focus on non-eruptive prominences, and describe recent progress in four areas of prominence research: (1) magnetic structure deduced from observations and models, (2) the dynamics of prominence plasmas (formation and flows), (3) Magneto-hydrodynamic (MHD) waves in prominences and (4) the formation and large-scale patterns of the filament channels in which prominences are located. Finally, several outstanding issues in prominence research are discussed, along with observations and models required to resolve them.

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“…The association of EUV waves with filament oscillations was called into question in one event where the filament oscillation seemed to start before the wave arrival (Eto et al, 2002). It has been argued that this could be explained in terms of a tilted wavefront (Warmuth et al, 2004b), where higher parts of the front reach the filament earlier than the lower parts that generate stronger signatures.…”

Section: Excitation Of Oscillationsmentioning

confidence: 99%

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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Relation between a Moreton Wave and an EIT Wave Observed on 1997 November 4

Cited by 131 publications

References 20 publications

HαMoreton waves observed on December 06, 2006

HαMoreton waves observed on December 06, 2006

Physics of Solar Prominences: II—Magnetic Structure and Dynamics

Large-scale Globally Propagating Coronal Waves

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