New Observation of Failed Filament Eruptions: The Influence of Asymmetric Coronal Background Fields on Solar Eruptions

Liu, Yu; Su, Jiangtao; Xu, Zhe; Lin, Haosheng; Shibata, Kazunari; Kurokawa, Hiroshi

doi:10.1088/0004-637x/696/1/l70

Cited by 61 publications

(63 citation statements)

References 16 publications

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“…Remarkably, north of the eruption region, there appeared abundant cool material (arrows in panels c−d), staying there for about 20 min after the eruption. This indicated that the filament eruption was likely confined, and the mass was ejected to places far away, similar to the example in Liu et al (2009). We also investigated the failed eruption in AIA 304 Å images in the right panels.…”

Section: Failed Filament Eruptionmentioning

confidence: 64%

“…Failed filament eruptions are particular events and have been observed in some cases (Moore et al 2001;Ji et al 2003;Liu et al 2009;Shen et al 2011). They generally are non-ejective and not associated with expelled CMEs.…”

Section: Discussionmentioning

confidence: 99%

“…Liu (2008) showed that the magnetic field's decrease with height is faster in a successful eruption than that in a failed eruption, and found that the field intensity at low altitude in a failed eruption was a few times stronger than that in a successful one. Liu et al (2009) reported two failed filament eruptions in the asymmetric coronal fields, which could not only influence the trajectories of the ejecta, but also provided a relatively stronger confinement for flux rope eruptions. Similar to the event in Sterling et al (2011), the filament eruption we studied was due to the gradual magnetic cancelation around it and confined by the large-scale overlying loops.…”

Section: Discussionmentioning

confidence: 99%

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An extreme ultraviolet wave associated with a failed eruption observed by the Solar Dynamics Observatory

Zheng

et al. 2012

A&A

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Aims. Taking advantage of the high temporal and spatial resolution of the Solar Dynamics Observatory (SDO) observations, we present an extreme ultraviolet (EUV) wave associated with a failed filament eruption that generated no coronal mass ejection (CME) on 2011 March 1. We aim at understanding the nature and origin of this EUV wave. Methods. Combining the high-quality observations in the photosphere, the chromosphere, and the corona, we studied the characteristics of the wave and its relations to the associated eruption. Results. The event occurred at an ephemeral region near a small active region. The continuous magnetic flux cancelation in the ephemeral region produced pre-eruption brightenings and two EUV jets, and excited the filament eruption, accompanying it with a microflare. After the eruption, the filament material appeared far from the eruption center, and the ambient loops seemed to be intact. It was evident that the filament eruption had failed and was not associated with a CME. The wave happened just after the north jet arrived, and apparently emanated ahead of the north jet, far from the eruption center. The wave propagated at nearly constant velocities in the range of 260−350 km s −1 , with a slight negative acceleration in the last phase. Remarkably, the wave continued to propagate, and a loop in its passage was intact when wave and loop met. Conclusions. Our analysis confirms that the EUV wave is a true wave, which we interpret as a fast-mode wave. In addition, the close temporal and spatial relationship between the wave and the jet provides evidence that the wave was likely triggered by the jet when the CME failed to happen.

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Section: Failed Filament Eruptionmentioning

confidence: 64%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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An extreme ultraviolet wave associated with a failed eruption observed by the Solar Dynamics Observatory

Zheng

et al. 2012

A&A

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“…A key question of successive eruptions is whether they are physically connected or not. It seems that the answer is positive, and the connection is often of a magnetic nature (e.g., Jiang et al (2008), Jiang et al (2011), Török et al (2011), Shen, Liu & Su (2012, Titov et al (2012), Lynch & Edmondson (2013), Schrijver & Title (2011), Schrijver et al (2013). …”

Section: Introductionmentioning

confidence: 99%

Successive filament eruptions within one solar breakout event

Shen

2013

Proc. IAU

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Abstract. The magnetic breakout model has been widely used to explain solar eruptive activities. Here, we apply it to explain successive filament eruptions occurred in a quadrupolar magnetic source region. Based on the high temporal and spatial resolution, multi-wavelengths observations taken by the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamic Observatory (SDO), we find some signatures that support the occurrence of breakout-like external reconnection just before the start of the successive filament eruptions. Furthermore, the extrapolated three-dimensional coronal field also reveals that the magnetic topology above the quadrupolar source region resembles that of the breakout model. We propose a possible mechanism within the framework of the breakout model to interpret the successive filament eruptions, in which the so-called magnetic implosion mechanism is firstly introduced to be the physical linkage of successive filament eruptions. We conclude that the structural properties of coronal fields are important for producing successive filament eruptions.

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“…Shen, Liu, and Liu (2011) have reported the dynamics of a filament that failed in the eruption several times, and finally succeeded to erupt with the triggering of a C-class flare process and associated CME on 8 February 2010 from active region (AR) NOAA 11045. Before that work, the observational evidence of flux ropes failed in eruption has been reported as well (Ji et al, 2003;Alexander, Liu, and Gilbert, 2006;Liu et al, 2009). Filippov and Den (2001) have studied the critical height and compared it with the stability criterion of the filaments.…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength Observations of a Failed Flux Rope in the Eruption and Associated M-Class Flare from NOAA AR 11045

et al. 2011

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We present the multi-wavelength observations of a flux rope that was trying to erupt from NOAA AR 11045 and the associated M-class solar flare on 12 February 2010 using space and ground based observations from TRACE, STEREO, SOHO/MDI, Hinode/XRT and BBSO. While the flux rope was rising from the active region, an M1.1/2F class flare was triggered nearby one of its footpoints. We suggest that the flare triggering was due to the reconnection of a rising flux rope with the surrounding low-lying magnetic loops. The flux rope reached a projected height of ≈ 0.15R with a speed of ≈90 km s −1 while the soft X-ray flux enhanced gradually during its rise. The flux rope was suppressed by an overlying field and the filled plasma moved towards the negative polarity field to the west of its activation site. We find the first observational evidence of the initial suppression of a flux rope due to a remnant filament visible both at chromospheric and coronal temperatures that evolved couple of days before at the same location in the active region. SOHO/MDI magnetograms show the emergence of a bipole ≈12 h prior to the flare initiation. The emerged negative polarity moved towards the flux rope activation site, and flare triggering near the photospheric polarity inversion line (PIL) took place. The motion of the negative polarity region towards PIL helped in the build-up of magnetic energy at the flare and flux rope activation site. This study provides a unique observational

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New Observation of Failed Filament Eruptions: The Influence of Asymmetric Coronal Background Fields on Solar Eruptions

Cited by 61 publications

References 16 publications

An extreme ultraviolet wave associated with a failed eruption observed by the Solar Dynamics Observatory

An extreme ultraviolet wave associated with a failed eruption observed by the Solar Dynamics Observatory

Successive filament eruptions within one solar breakout event

Multiwavelength Observations of a Failed Flux Rope in the Eruption and Associated M-Class Flare from NOAA AR 11045

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