High-Resolution Observations of a Flux Rope with the Interface Region Imaging Spectrograph

Li, Ting; Zhang, Jun

doi:10.1007/s11207-015-0768-y

Cited by 14 publications

(4 citation statements)

References 44 publications

(28 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Overall then, Case 1 is the better-fitting run. Additionally, the smaller initial twist of this case is in better agreement with recent estimates of the twist that can accumulate in active regions before an eruption occurs (see Guo et al 2013;Li & Zhang 2015;Liu et al 2016).…”

Section: Discussionsupporting

confidence: 89%

“…The range of initial twists considered here is consistent with the results of Guo et al (2013), Li & Zhang (2015), and Liu et al (2016), who found values up to about 4π in other eruptive solar events. The parametric simulation study of the present event in HK16 favored this same value but yielded a reasonable agreement with the observations also for Φ = 4.5π.…”

Section: Simulation Of the Confined Eruptionsupporting

confidence: 91%

See 1 more Smart Citation

Helical kink instability in the confined solar eruption on 2002 May 27

2016

View full text Add to dashboard Cite

This paper presents an improved MHD modeling of the confined filament eruption in solar active region NOAA 9957 on 2002 May 27 by extending the parametric studies of the event in Török & Kliem (2005) and Hassanin & Kliem (2016). Here the initial flux rope equilibrium is chosen to possess a small apex height identical to the observed initial filament height, which implies a more realistic inclusion of the photospheric line tying. The model matches the observations as closely as in the preceding studies, with the closest agreement again being obtained for an initial average flux rope twist of about 4π. Thus, the model for strongly writhing confined solar eruptions, which assumes that a kink‐unstable flux rope in the stability domain of the torus instability exists at the onset of the eruption's main acceleration phase, is further substantiated. (© 2016 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)

show abstract

Section: Discussionsupporting

confidence: 89%

Section: Simulation Of the Confined Eruptionsupporting

confidence: 91%

Helical kink instability in the confined solar eruption on 2002 May 27

2016

View full text Add to dashboard Cite

show abstract

“…The light wall apparently consists of warm (1330 Å and 1400 Å) and cold (Hα) material simultaneously. In the 1330 Å and 1400 Å channels, the cold material seems semitransparent and optically thin, while the hot structure was clearly detected (Li & Zhang 2015). This causes the wall body to appear as a brightening (see panels d-f).…”

Section: Conclusion and Discussionmentioning

confidence: 96%

Light walls around sunspots observed by the Interface Region Imaging Spectrograph

Hou

Yang

et al. 2016

A&A

View full text Add to dashboard Cite

Context. The Interface Region Imaging Spectrograph (IRIS) mission provides high-resolution observations of the chromosphere and transition region. Using these data, some authors have reported the new finding of light walls above sunspot light bridges. Aims. We try to determine whether the light walls exist somewhere else in active regions in addition to the light bridges. We also examine how the material of these walls evolves. Methods. Employing six months of (from 2014 December to 2015 June) high tempo-spatial data from the IRIS, we find many light walls either around sunspots or above light bridges. Results. For the first time, we report one light wall near an umbral-penumbral boundary and another along a neutral line between two small sunspots. The former light wall has a multilayer structure and is associated with the emergence of positive magnetic flux in the ambient negative field. The latter light wall is associated with a filament activation, and the wall body consists of the filament material, which flowed to a remote plage region with a negative magnetic field after the light wall disappeared. Conclusions. These new observations reveal that these light walls are multilayer and multithermal structures that occur along magnetic neutral lines in active regions.

show abstract

“…One possibility is a twisted flux rope Demoulin & Priest 1989;Amari et al 2000;Jiang et al 2014;Su et al 2015;Li et al 2015) and the other is a sheared arcade structure (Amari et al 1991;Antiochos et al 1994;DeVore & Antiochos 2000;Welsch et al 2005). For this event, the nonlinear force free extrapolation suggests that the filament has a twisted magnetic structure, but such a twisted structure cannot be seen clearly in the observations at present.…”

Section: Discussionmentioning

confidence: 86%

The Formation of an Inverse S-Shaped Active-Region Filament Driven by Sunspot Motion and Magnetic Reconnection

Yan

Priest

Guo

et al. 2016

ApJ

View full text Add to dashboard Cite

We present a detailed study of the formation of an inverse S-shaped filament prior to its eruption in active region NOAA 11884 from October 31 to November 2, 2013. In the initial stage, clockwise rotation of a small positive sunspot around the main negative trailing sunspot formed a curved filament. Then the small sunspot cancelled with negative magnetic flux to create a longer activeregion filament with an inverse S-shape. At the cancellation site a brightening was observed in UV and EUV images and bright material was transferred to the filament. Later the filament erupted after cancellation of two opposite polarities under the upper part of the filament. Nonlinear force-free field (NLFFF) extrapolation of vector photospheric fields suggests that the filament may have a twisted structure, but this cannot be confirmed from the current observations.

show abstract

High-Resolution Observations of a Flux Rope with the Interface Region Imaging Spectrograph

Cited by 14 publications

References 44 publications

Helical kink instability in the confined solar eruption on 2002 May 27

Helical kink instability in the confined solar eruption on 2002 May 27

Light walls around sunspots observed by the Interface Region Imaging Spectrograph

The Formation of an Inverse S-Shaped Active-Region Filament Driven by Sunspot Motion and Magnetic Reconnection

Contact Info

Product

Resources

About