Triggering Mechanism for the Filament Eruption on 2005 September 13 in NOAA Active Region 10808

Nagashima, K.; Isobe, Hiroaki; Yokoyama, T.; Ishii, Takako T.; Okamoto, Takenori J.; Shibata, Kazunari

doi:10.1086/521139

Cited by 33 publications

(37 citation statements)

References 31 publications

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“…In the case of Nagashima et al (2007), on the other hand, a sequence of small flares close to the filament footpoints was identified at the time the filament was slowly lifting off (40 h before the eruption). This was followed by the filament eruption and a CME.…”

Section: Living Reviews In Solar Physicsmentioning

confidence: 99%

Solar Prominences: Observations

Parenti

2014

Living Rev. Solar Phys.

290

234

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Solar prominences are one of the most common features of the solar atmosphere. They are found in the corona but they are one hundred times cooler and denser than the coronal material, indicating that they are thermally and pressure isolated from the surrounding environment. Because of these properties they appear at the limb as bright features when observed in the optical or the EUV cool lines. On the disk they appear darker than their background, indicating the presence of a plasma absorption process (in this case they are called filaments). Prominence plasma is embedded in a magnetic environment that lies above magnetic inversion lines, denoted a filament channel.This paper aims at providing the reader with the main elements that characterize these peculiar structures, the prominences and their environment, as deduced from observations. The aim is also to point out and discuss open questions on prominence existence, stability and disappearance.The review starts with a general introduction of these features and the instruments used for their observation. Section 2 presents the large scale properties, including filament morphology, thermodynamical parameters, magnetic fields, and the properties of the surrounding coronal cavity, all in stable conditions. Section 3 is dedicated to small-scale observational properties, from both the morphological and dynamical points of view. Section 4 introduces observational aspects during prominence formation, while Section 5 reviews the sources of instability leading to prominence disappearance or eruption. Conclusions and perspectives are given in Section 6.

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Section: Living Reviews In Solar Physicsmentioning

confidence: 99%

Solar Prominences: Observations

Parenti

2014

Living Rev. Solar Phys.

290

234

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“…This event was also studied independently by Nagashima et al (2007) and Chifor et al (2007) mainly on the long-term evolution of filaments and flare precursors in X-rays, respectively. We, however, mainly concentrate on the detailed timing analysis of the event as evidenced by the flare ribbon motion and filament dynamics.…”

Section: Introductionmentioning

confidence: 99%

Successive Flaring during the 2005 September 13 Eruption

Wang

Liu

Jing

et al. 2007

ApJ

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We report a detailed analysis of successive flaring during the X1.5 event in the NOAA AR 0808 on 2005 September 13. We identify a filament lying at the southeast boundary of the active region as the physical linkage between the two flares in close succession. It is noticeable that the filament erupted $13 minutes after the initial flare onset at $19:22 UT near the central magnetic polarity inversion line (PIL). During this time period, the filament only showed a slow rising; meanwhile, a spatially associated large magnetic loop with one leg connecting to the initial flaring site began to brighten in the TRACE 195 8 channel. After $19:35 UT, the filament abruptly erupted together with the bright TRACE loop. Besides the moving ribbons at the first flaring site, the filament eruption caused a secondary flare identified with another set of moving ribbons. This event thus provides a clear evidence for the successive flaring where the initial flare destabilizes the nearby flux loop system, leading to the filament eruption with the second flare. We also identify the initial flare core by finding rapid, irreversible enhancements of the photospheric transverse magnetic fields at a section of the PIL.

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“…Common mechanisms proposed as the possible triggers for flares have been interactions with emerging magnetic flux (Rust, 1976;Wang and Sheeley, 1999;Feynman and Martin, 2001;Xu et al, 2007), interactions of filament magnetic fields with overlying coronal fields (Antiochos et al, 1999), interactions of the root fields of filaments with adjacent magnetic fields, the occurence of small solar flares (Nagashima et al, 2007), and in relatively rare cases, being hit by flare waves (Harvey et al, 1974;Okamoto et al, 2004). The concept presented here is not dependent upon any particular triggering mechanism.…”

Section: The Triggering Of Eruptive Eventsmentioning

confidence: 89%

The link between CMEs, filaments and filament channels

et al. 2008

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Abstract. We present a broad concept for the build-up to eruptive solar events which needs to be tested in future observational and theoretical research. In this concept an eruptive solar event consists of a coronal mass ejection, a filament eruption, a cavity around the filament, and a flare. In our picture, the initial energy source must be external to this eruptive system but also feed into it. Among all eruptive events the common denominator is a filament channel with canceling magnetic fields along a primary polarity reversal boundary. We find that magnetic reconnection at or close to the photosphere is the only interpretation of canceling fields to date that is consistent with observations of filament channels. This reconnection serves to transfer magnetic flux from the photosphere into the chromosphere and corona along polarity reversal boundaries and concurrently initiates the building of a filament channel. Magnetic flux, in excess of that needed to sustain the filament channel, goes into building a filament magnetic field that is always aligned with the polarity reversal boundary and the channel magnetic field. The filament magnetic field remains separated from overarching coronal magnetic fields by the magnetic field of the cavity. The magnetic flux being transported upward from the photosphere/chromosphere carries streams of plasma into the corona along the filament magnetic field. However, the flowing and counterstreaming filament mass also slowly drains out of the field and thereby leaves behind new strands of cavity magnetic field with little or no associated mass. When the build-up of magnetic pressure in the filament and cavity magnetic fields exceeds that of the overlying coronal loops, the coronal loops, the filament and the cavity together begin an observable slow rise which can last a few hours to many days before rapid onset and ejection with a solar flare. We suggest that this process can be accelerated by any number of external triggering mechanisms which serve as catalysts Correspondence to: S. F. Martin (sara@helioresearch.org) to cause the impending eruption to happen earlier than it otherwise would occur.

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Triggering Mechanism for the Filament Eruption on 2005 September 13 in NOAA Active Region 10808

Cited by 33 publications

References 31 publications

Solar Prominences: Observations

Solar Prominences: Observations

Successive Flaring during the 2005 September 13 Eruption

The link between CMEs, filaments and filament channels

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