Micro-Sigmoids as Progenitors of Coronal Jets: Is Eruptive Activity Self-Similarly Multi-Scaled?

Raouafi, N. E.; Georgoulis, Manolis K.; Rust, David M.; Bernasconi, P. N.

doi:10.1088/0004-637x/718/2/981

Cited by 58 publications

(82 citation statements)

References 46 publications

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“…Recently, a self-similar AR-coronal BP jet connection was made when Raouafi et al (2010) observed micro-sigmoids at the bases of coronal jets in XRT data. The authors found that these micro-sigmoids were manifestations of merging "Jshaped" loops at scales significantly smaller than their AR counterparts (McKenzie & Canfield 2008).…”

Section: Introductionmentioning

confidence: 99%

“…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: 99%

“…The previously considered events (except Raouafi et al 2010) were associated directly with large-scale concentrations of bipolar magnetic flux. However, it is an open question as to whether the small-scale network magnetic flux of the quiet Sun (QS) can form and sustain EUV BP activity with sigmoidal structuring and dynamics self-similar to their higher temperature counterparts.…”

Section: Introductionmentioning

confidence: 99%

“…However, it is an open question as to whether the small-scale network magnetic flux of the quiet Sun (QS) can form and sustain EUV BP activity with sigmoidal structuring and dynamics self-similar to their higher temperature counterparts. The QS network is known to be able to sustain non-potential fields and sigmoidal activity (Chesny et al 2013), but non-potentiality has only been associated with high-temperature BP activity by Raouafi et al (2010). Evidence of such cool activity will show a multi-scaled self-similarity in the sigmoid-BP relationship down to the QS network scale.…”

Section: Introductionmentioning

confidence: 99%

“…These unique data may help to resolve whether certain instability mechanisms are self-similar throughout different temperature and magnetic field regimes in the solar atmosphere. Raouafi et al (2010) noted that the spatial resolution of XRT observations is insufficient for resolving very small BPs, so we look to address the question as to whether there are QS-scale BPs that can be associated with sigmoid activity. These data may provide the observations of unique simultaneous magnetic field dynamics and jet development in the QS.…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

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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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Quiet-Sun Network Bright Point Phenomena With Sigmoidal Signatures

Chesny

Oluseyi

Orange³

et al. 2015

ApJ

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Observations of solar X‐ray and EUV jets and their related phenomena

et al. 2016

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Solar jets are fast‐moving, elongated brightenings related to ejections seen in both images and spectra on all scales from barely visible chromospheric jets to coronal jets extending up to a few solar radii. The largest, most powerful jets are the source of type III radio bursts, energetic electrons and ions with greatly enhanced 3He and heavy element abundances. The frequent coronal jets from polar and equatorial coronal holes may contribute to the solar wind. The primary acceleration mechanism for all jets is believed to be release of magnetic stress via reconnection; however the energy buildup depends on the jets' source environment. In this review, we discuss how certain features of X‐ray and EUV jets, such as their repetition rate and association with radio emission, depends on their underlying photospheric field configurations (active regions, polar and equatorial coronal holes, and quiet Sun). (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

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Comparative Analysis of a Transition Region Bright Point with a Blinker and Coronal Bright Point Using Multiple EIS Emission Lines

et al. 2013

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Since their discovery twenty year ago, transition region bright points have never been observed spectroscopically. Bright point properties have not been compared with similar transition region and coronal structures. In this work we have investigated three transient quiet Sun brightenings including a transition region bright point (TR BP), a coronal bright point (CBP) and a blinker. We use time-series observations of the extreme ultraviolet emission lines of a wide range of temperature T (log T = 5.3 − 6.4) from the EUV imaging spectrometer (EIS) onboard the Hinode satellite. We present the EIS temperature maps and Doppler maps, which are compared with magnetograms from the Michelson Doppler Imager (MDI) onboard the SOHO satellite. Doppler velocities of the TR BP and blinker are ≤ 25 km s −1 , which is typical of transient TR phenomena. The Dopper velocities of the CBP were found to be ≤ 20 km s −1 with exception of those measured at log T = 6.2 where a distinct bi-directional jet is observed. From an EM loci analysis we find evidence of single and double isothermal components in the TR BP and CBP, respectively. TR BP and CBP loci curves are characterized by broad distributions suggesting the existence of unresolved structure. By comparing and contrasting the physical characteristics of the events we find the BP phenomena are an indication of multi-scaled self similarity, given similarities in both their underlying magnetic field configuration and evolution in relation to EUV flux changes. In contrast, the blinker phenomena and the TR BP are sufficiently dissimilar in their observed properties as to constitute different event classes. Our work is an indication that the measurement of similar characteristics across multiple event types holds class-predictive power, and is a significant step towards automated solar atmospheric multiclass classification of unresolved transient EUV sources. Finally, the analysis performed here establishes a connection between solar quiet region CBPs and jets.

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Micro-Sigmoids as Progenitors of Coronal Jets: Is Eruptive Activity Self-Similarly Multi-Scaled?

Cited by 58 publications

References 46 publications

Quiet-Sun Network Bright Point Phenomena With Sigmoidal Signatures

Quiet-Sun Network Bright Point Phenomena With Sigmoidal Signatures

Observations of solar X‐ray and EUV jets and their related phenomena

Comparative Analysis of a Transition Region Bright Point with a Blinker and Coronal Bright Point Using Multiple EIS Emission Lines

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