Loop oscillations and an extreme ultraviolet wave associated with a micro-sigmoid eruption

Zheng, Ruisheng; YC, Jiang; JY, Yang; JC, Hong; Bi, Yong; Yang, Bo; Yang, Danni

doi:10.1093/mnras/stt258

Cited by 22 publications

(18 citation statements)

References 62 publications

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“…In the present event, the temporal and spatial relationship between the wave and the expanding loop system provide evidence that the EUV wave was driven by the expanding loop system. We emphasize that the expanding loop observed in the present event and the newly formed loops in Zheng et al (2012d) and Zheng et al (2013b) can be considered as the CME prototype in the low corona. Although miniature solar eruptions involving expanding loops can not launch successful CMEs that can be observed by coronagraphs, they resemble many characteristics with large-scale successful CMEs during the initiation eruption stage.…”

Section: Conclusion and Discussionmentioning

confidence: 52%

On a Small-scale EUV Wave: The Driving Mechanism and the Associated Oscillating Filament

Shen

Liu

Tian

et al. 2017

ApJ

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We present observations of a small-scale Extreme-ultraviolet (EUV) wave that was associated with a mini-filament eruption and a GOES B1.9 micro-flare in the quiet Sun region. The initiation of the event was due to the photospheric magnetic emergence and cancellation in the eruption source region, which first caused the ejection of a small plasma ejecta, then the ejecta impacted on a nearby mini-filament and thereby led to the filament's eruption and the associated flare. During the filament eruption, an EUV wave at a speed of 182 -317 km s −1 was formed ahead of an expanding coronal loop, which propagated faster than the expanding loop and showed obvious deceleration and reflection during the propagation. In addition, the EUV wave further resulted in the transverse oscillation of a remote filament whose period and damping time are 15 and 60 minutes, respectively. Based on the observational results, we propose that the small-scale EUV wave should be a fast-mode magnetosonic wave that was driven by the the expanding coronal loop. Moreover, with the application of filament seismology, it is estimated that the radial magnetic field strength is about 7 Gauss. The observations also suggest that small-scale EUV waves associated with miniature solar eruptions share similar driving mechanism and observational characteristics with their large-scale counterparts.

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Section: Conclusion and Discussionmentioning

confidence: 52%

On a Small-scale EUV Wave: The Driving Mechanism and the Associated Oscillating Filament

Shen

Liu

Tian

et al. 2017

ApJ

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“…This was supported by actual observations of coronal waves in SXR, where corresponding SXR ejecta were identified as likely wave sources (Hudson et al, 2003;Narukage et al, 2004, see Figures 18 and 19, respectively). such as plasma blobs (Kumar and Manoharan, 2013, see Figure 40), surges (Zheng et al, 2012a(Zheng et al, , 2013a, EUV jets (Zheng et al, 2012b), mini-CMEs (Zheng et al, 2011), mini-filament eruptions (Zheng et al, 2012c), and micro-sigmoid eruptions (Zheng et al, 2012d(Zheng et al, , 2013b. However, even increased observational capabilities are not always sufficient to distinguish between different scenarios.…”

Section: Small-scale Ejectamentioning

confidence: 99%

Large-scale Globally Propagating Coronal Waves

Warmuth

2015

Living Rev. Sol. Phys.

162

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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“…The authors found that these micro-sigmoids were manifestations of merging "Jshaped" loops at scales significantly smaller than their AR counterparts (McKenzie & Canfield 2008). Such observations and dynamics, along with EUV observations of micro-sigmoids (Zheng et al 2013), point to a possible multi-scaled selfsimilarity in the ensemble of sigmoid events leading to eruptive activity. Raouafi et al (2010) concluded that if there are selfsimilarities between event properties and instability mechanisms, then the eruptions of micro-sigmoids could lead to magnetic energy dissipations and injections of helicity into the heliosphere.…”

Section: Introductionmentioning

confidence: 83%

Quiet-Sun Network Bright Point Phenomena With Sigmoidal Signatures

Chesny

Oluseyi

Orange³

et al. 2015

ApJ

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Ubiquitous solar atmospheric coronal and transition region bright points (BPs) are compact features overlying strong concentrations of magnetic flux. Here, we utilize high-cadence observations from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory to provide the first observations of extreme ultraviolet quietSun (QS) network BP activity associated with sigmoidal structuring. To our knowledge, this previously unresolved fine structure has never been associated with such small-scale QS events. This QS event precedes a bi-directional jet in a compact, low-energy, and low-temperature environment, where evidence is found in support of the typical fan-spine magnetic field topology. As in active regions and micro-sigmoids, the sigmoidal arcade is likely formed via tether-cutting reconnection and precedes peak intensity enhancements and eruptive activity. Our QS BP sigmoid provides a new class of small-scale structuring exhibiting self-organized criticality that highlights a multiscaled self-similarity between large-scale, high-temperature coronal fields and the small-scale, lower-temperature QS network. Finally, our QS BP sigmoid elevates arguments for coronal heating contributions from cooler atmospheric layers, as this class of structure may provide evidence favoring mass, energy, and helicity injections into the heliosphere.

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Loop oscillations and an extreme ultraviolet wave associated with a micro-sigmoid eruption

Cited by 22 publications

References 62 publications

On a Small-scale EUV Wave: The Driving Mechanism and the Associated Oscillating Filament

On a Small-scale EUV Wave: The Driving Mechanism and the Associated Oscillating Filament

Large-scale Globally Propagating Coronal Waves

Quiet-Sun Network Bright Point Phenomena With Sigmoidal Signatures

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