Are Moreton Waves Coronal Phenomena?

Balasubramaniam, Krishnan; Pevtsov, Alexei A.; Neidig, D. F.

doi:10.1086/512001

Cited by 33 publications

(30 citation statements)

References 26 publications

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“…They interpreted this behavior in terms of an event driven by expansion of the ends of an erupting flux rope rather than in terms of explosive heating by the flare. A similar event was reported by Balasubramaniam et al (2007) for the same AR, on 2003 October 29. Both Muhr et al (2010) and Veronig et al (2008) used timing relationships similar to that in Figure 6 (with wave onset in each case preceding the peak of hard X-ray emission by ∼0.5 minutes) to argue against flare drivers in the waves they investigated.…”

Section: Growing Evidence For Cme Drivers Of Large-scale Wavessupporting

confidence: 84%

“…Such waves have characteristic speeds of ∼1000 km s −1 and tend to be directional, with angular widths typically in the range from 60 • to 150 • (Smith & Harvey 1971;Warmuth et al 2004a;Veronig et al 2006), although cases with fragmented arcs collectively spanning larger angles have been reported (Pick et al 2005;Balasubramaniam et al 2007;Muhr et al 2008Muhr et al , 2010. Following their discovery, the pre-eminent research result on these dramatic solar events was Uchida's synthesis (Uchida 1968(Uchida , 1973(Uchida , 1974a(Uchida , 1974bUchida et al 1973) of Moreton waves and metric type II radio bursts (Payne-Scott et al 1947;Wild & McReady 1950) in terms of a flare-generated fast-mode MHD wave.…”

Section: Introductionmentioning

confidence: 99%

“…Following their discovery, the pre-eminent research result on these dramatic solar events was Uchida's synthesis (Uchida 1968(Uchida , 1973(Uchida , 1974a(Uchida , 1974bUchida et al 1973) of Moreton waves and metric type II radio bursts (Payne-Scott et al 1947;Wild & McReady 1950) in terms of a flare-generated fast-mode MHD wave. The characteristic down-up pattern of Moreton waves indicates a depression of the chromosphere (or lower corona; Balasubramaniam et al 2007) by a coronal shock and subsequent relaxation or restoration. Recently, Warmuth et al (2004a) 12 Emeritus. have argued for a general synthesis of large-scale wave phenomena-including waves observed in soft X-rays (Khan & Aurass 2002;Narukage et al 2002;Hudson et al 2003;Warmuth et al 2005), extreme ultra-violet (EIT or EUV waves; Neupert 1989; Thompson et al 1998Thompson et al , 1999, He i 10830 Å (Vršnak et al 2002;Gilbert & Holzer 2004), microwaves (Warmuth et al 2004a;White & Thompson 2005), as well as Moreton waves and type II radio bursts.…”

Section: Introductionmentioning

confidence: 99%

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On the Origin of the Solar Moreton Wave of 2006 December 6

Balasubramaniam

Cliver

Pevtsov

et al. 2010

ApJ

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We analyzed ground-and space-based observations of the eruptive flare (3B/X6.5) and associated Moreton wave (∼850 km s −1 ; ∼270 • azimuthal span) of 2006 December 6 to determine the wave driver-either flare pressure pulse (blast) or coronal mass ejection (CME). Kinematic analysis favors a CME driver of the wave, despite key gaps in coronal data. The CME scenario has a less constrained/smoother velocity versus time profile than is the case for the flare hypothesis and requires an acceleration rate more in accord with observations. The CME picture is based, in part, on the assumption that a strong and impulsive magnetic field change observed by a GONG magnetograph during the rapid rise phase of the flare corresponds to the main acceleration phase of the CME. The Moreton wave evolution tracks the inferred eruption of an extended coronal arcade, overlying a region of weak magnetic field to the west of the principal flare in NOAA active region 10930. Observations of Hα foot point brightenings, disturbance contours in off-band Hα images, and He i 10830 Å flare ribbons trace the eruption from 18:42 to 18:44 UT as it progressed southwest along the arcade. Hinode EIS observations show strong blueshifts at foot points of this arcade during the post-eruption phase, indicating mass outflow. At 18:45 UT, the Moreton wave exhibited two separate arcs (one off each flank of the tip of the arcade) that merged and coalesced by 18:47 UT to form a single smooth wave front, having its maximum amplitude in the southwest direction. We suggest that the erupting arcade (i.e., CME) expanded laterally to drive a coronal shock responsible for the Moreton wave. We attribute a darkening in Hα from a region underlying the arcade to absorption by faint unresolved post-eruption loops.

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Section: Growing Evidence For Cme Drivers Of Large-scale Wavessupporting

confidence: 84%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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On the Origin of the Solar Moreton Wave of 2006 December 6

Balasubramaniam

Cliver

Pevtsov

et al. 2010

ApJ

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“…One could thus assume that filaments are actually a more sensitive tracer of the expanding coronal wavefront proposed by Uchida (1968) than the chromosphere itself (cf. also Balasubramaniam et al, 2007).…”

Section: Excitation Of Oscillationsmentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

168

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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“…On December 6, 2006 the filaments exhibit a high intensity oscillation, i.e., both disappear completely in the Hα images and the winking can be attributed to the motion of the filament structure that shifts it out of the observed Hα bandpass (Balasubramaniam et al 2007). As stated by Gilbert et al (2008), the SF shows a mixture of transverse and perpendicular motion with respect to the filament spine, while the NF exhibits a less dynamic response, probably only oscillating in the plane of the sky.…”

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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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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Are Moreton Waves Coronal Phenomena?

Cited by 33 publications

References 26 publications

On the Origin of the Solar Moreton Wave of 2006 December 6

On the Origin of the Solar Moreton Wave of 2006 December 6

Large-scale Globally Propagating Coronal Waves

HαMoreton waves observed on December 06, 2006

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