An Extreme Ultraviolet Wave Associated with a Solar Filament Activation

A solar filament is a dense cool condensation that is supported and thermally insulated by magnetic fields in the rarefied hot corona. Its evolution and stability, leading to either an eruption or disappearance, depend on its coupling with the surrounding hot corona through a thin transition region, where the temperature steeply rises. However, the heating and dynamics of this transition region remain elusive. We report extreme-ultraviolet observations of quiescent filaments from the Solar Dynamics Observatory that reveal prominence spicules propagating through the transition region of the filament-corona system. These thin needle-like jet features are generated and heated to at least 0.7 MK by turbulent motions of the material in the filament. We suggest that the prominence spicules continuously channel the heated mass into the corona and aid in the filament evaporation and decay. Our results shed light on the turbulence-driven heating in magnetized condensations that are commonly observed on the Sun and in the interstellar medium.

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On the partial eruption of a bifurcated solar filament structure

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2902 ◽

2020 ◽

Vol 500 (1) ◽

pp. 684-695

Author(s):

Aabha Monga ◽

Rahul Sharma ◽

Jiajia Liu ◽

Consuelo Cid ◽

Wahab Uddin ◽

...

Keyword(s):

Magnetic Field ◽

Extreme Ultraviolet ◽

Free Field ◽

Small Scale ◽

Data Sets ◽

Imaging Data ◽

Filament Structure ◽

Filament Channel ◽

Solar Filament ◽

Using Data

ABSTRACT The partial eruption of a filament channel with bifurcated substructures is investigated using data sets obtained from both ground-based and space-borne facilities. Small-scale flux reconnection/cancellation events in the region triggered the pile-up of ambient magnetic field, observed as bright extreme ultraviolet (EUV) loops in close proximity to the filament channel. This led to the formation of a V-shaped cusp structure at the site of interaction between the coalesced EUV loops and the filament channel, with the presence of distinct plasmoid structures and associated bidirectional flows. Analysis of imaging data from SDO/AIA further suggests vertical splitting of the filament structure into two substructures. The perturbed upper branch of the filament structure rose up and erupted with the onset of an energetic GOES M1.4 flare at 04:30 ut on 2015 January 28. The estimated twist number and squashing factor obtained from non-linear force free-field extrapolation of the magnetic field data support the vertical split in the filament structure with high twist in the upper substructure. The loss in equilibrium of the upper branch due to torus instability implies that this is a potential triggering mechanism for the observed partial eruption.

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On the Role of Magnetic Fields in an Erupting Solar Filament

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320000149 ◽

2019 ◽

Vol 15 (S354) ◽

pp. 452-453

Author(s):

Qiao Song ◽

Shuhong Yang ◽

Jing-Song Wang

Keyword(s):

Magnetic Fields ◽

Space Weather ◽

Extreme Ultraviolet ◽

Flux Rope ◽

Solar Dynamics Observatory ◽

Driving Mechanisms ◽

Solar Filament ◽

Solar Dynamics ◽

Mass Ejection

AbstractA filament eruption may lead to a coronal mass ejection (CME), which is one of the main driving mechanisms of space weather. This work analyses a slow and flareless CME event associated with an erupting quiescent filament. By using the extreme ultraviolet images of the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory, we trace the evolution of the filament in detail, and present the manifestations of the role of magnetic fields in the low corona. The results suggest the existence of a magnetic flux rope in the pre-eruption structures. Our study of this complex magnetic system may lead to a better understanding of CMEs and their impact on the space weather.

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Spectral Observations of Filament Activation

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313011496 ◽

2013 ◽

Vol 8 (S300) ◽

pp. 447-448 ◽

Cited By ~ 1

Author(s):

G. Mashnich

Keyword(s):

Spectral Data ◽

Northern Hemisphere ◽

Doppler Velocity ◽

Velocity Measurements ◽

Solar Filament ◽

Filament Activation ◽

Solar Uv ◽

Intensity Fluctuations ◽

Quiescent Filament

AbstractStudies of solar filament (prominence) activation and eruption are often based on measurements of intensity fluctuations in various solar emission bands and rarely on Doppler velocity measurements. The goal of this paper is to analyze the process of quiescent filament activation, using spectral data, and its associated events in solar UV band. Motions have been examined in a small southern fragment of a quiescent, extended filament in the northern hemisphere prior to and during its activation on June 14 2012. A part of the fragment disappeared after the filament activation.

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Coronal Mass Ejections and Solar Filament Disappearances at Solar Maximum

International Astronomical Union Colloquium ◽

10.1017/s0252921100025161 ◽

1994 ◽

Vol 144 ◽

pp. 127-129

Author(s):

S. Dinulescu ◽

G. Maris

Keyword(s):

Coronal Mass Ejections ◽

Solar Maximum ◽

Solar Filament

AbstractOccurrence of CMEs as a result of solar filament disappearance is discussed over the cycle 22.

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Prominences and Solar Activity

International Astronomical Union Colloquium ◽

10.1017/s0252921100065817 ◽

1979 ◽

Vol 44 ◽

pp. 357-372

Author(s):

Z. Švestka

Keyword(s):

Solar Activity ◽

Solar Cycle ◽

List Type ◽

Type Number ◽

Flare Loops ◽

Filament Activation

The following subjects were discussed:(1)Filament activation(2)Post-flare loops.(3)Surges and sprays.(4)Coronal transients.(5)Disk vs. limb observations.(6)Solar cycle variations of prominence occurrence.(7)Active prominences patrol service.Of all these items, (1) and (2) were discussed in most detail and we also pay most attention to them in this report. Items (3) and (4) did not bring anything new when compared with the earlier invited presentations given by RUST and ZIRIN and therefore, we omit them.

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