Interpretation of a complex CME event: Coupling of scales in multiple flux systems

Maia, D.; Aulanier, G.; Wang, S. J.; Pick, M.; Malherbe, Jean-Marie; Delaboudinière, J.-P.

doi:10.1051/0004-6361:20030359

Cited by 27 publications

(19 citation statements)

References 27 publications

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“…The initial condition requires a multipolar complex field with coronal null points where magnetic reconnection can occur. So far only some observational evidence has been produced in support of the model (Manoharan & Kundu 2003;Maia et al 2003). Sterling & Moore (2004) have suggested a mixed model with slow pre-eruption reconnection at the top of a loop system preceding a fast eruption in the sheared core region.…”

Section: Discussionmentioning

confidence: 99%

Early signatures of large-scale field line opening

Pohjolainen¹,

Vilmer²,

Khan³

et al. 2005

A&A

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Abstract.A fast "halo"-type coronal mass ejection (CME) associated with a two-ribbon flare, GOES class M 1.3, was observed on February 8, 2000. Soft X-ray and EUV images revealed several loop ejections and one wave-like moving front that started from a remote location, away from the flare core region. A radio type-II burst was observed near the trajectory of the moving soft X-ray front, although association with the CME itself cannot be ruled out. Large-scale dimmings were observed in EUV and soft X-rays, both in the form of disappearing transequatorial loops. We can pinpoint the time and the location of the first large-scale field-line opening by tracing the electron propagation paths above the active region and along the transequatorial loop system, in which large-scale mass depletion later took place. The immediate start of a type-IV burst (interpreted as an upward moving structure) which was located over a soft X-ray dimming region, confirms that the CME had lifted off. We compare these signatures with those of another halo CME event observed on May 2, 1998, and discuss the possible connections with the "magnetic breakout" model.

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Section: Discussionmentioning

confidence: 99%

Early signatures of large-scale field line opening

Pohjolainen¹,

Vilmer²,

Khan³

et al. 2005

A&A

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“…Several studies found that Moreton and EIT waves are formed in front of an erupting filament, consistent with a wave or shock generated by the erupting flux rope (e.g., Foley et al, 2003;Maia et al, 2003;Narukage et al, 2008).…”

Section: Coronal Mass Ejections (Cmes)mentioning

confidence: 95%

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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“…Direct magnetic connections between secondary ribbons and the main flare could be responsible for the brightening of the secondary ribbons. These connections are either by magnetic loops (Herant et al 1989;Maia et al 2003) or by a system of null points, separatrices, and QSLs at high altitude (Schrijver & Title 2011). The brightness enhancement of secondary ribbons is generally weaker than the main central flare ribbons and appears later than the main ribbons Schmieder et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Flare Ribbons Approach Observed by the Interface Region Imaging Spectrograph and the Solar Dynamics Observatory

Zhang

Hou

2017

ApJ

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We report flare ribbons approach (FRA) during a multiple-ribbon M-class flare on 2015 November 4 in NOAA AR 12443, obtained by the Interface Region Imaging Spectrograph and the Solar Dynamics Observatory. The flare consisted of a pair of main ribbons and two pairs of secondary ribbons. The two pairs of secondary ribbons were formed later than the appearance of main ribbons, with respective time delays of 15 and 19 minutes. The negative-polarity main ribbon spread outward faster than the first secondary ribbon with the same polarity in front of it, and thus the FRA was generated. Just before their encounter, the main ribbon was darkening drastically and its intensity decreased by about 70 % in 2 minutes, implying the suppression of main-phase reconnection that produced two main ribbons. The FRA caused the deflection of the main ribbon to the direction of secondary ribbon with a deflection angle of about 60• . Post-approach arcade was formed about 2 minutes later and the downflows were detected along the new arcade with velocities of 35−40 km s −1 , indicative of the magnetic restructuring during the process of FRA. We suggest that there are three topological domains with footpoints outlined by the three pairs of ribbons. Close proximity of these domains leads to deflection of the ribbons in agreement with the magnetic field topology.

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Interpretation of a complex CME event: Coupling of scales in multiple flux systems

Cited by 27 publications

References 27 publications

Early signatures of large-scale field line opening

Early signatures of large-scale field line opening

Large-scale Globally Propagating Coronal Waves

Flare Ribbons Approach Observed by the Interface Region Imaging Spectrograph and the Solar Dynamics Observatory

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