SOHO/SUMER observations of prominence  oscillation before eruption

Chen, P. F.; Innes, D. E.; Solanki, S. K.

doi:10.1051/0004-6361:200809544

Cited by 85 publications

(85 citation statements)

References 36 publications

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“…Since only one thread of the prominence was seen to erupt with the major part remaining in the low corona, this should be a partial prominence eruption event, which might be consistent with the rupture model (Sturrock et al 2001), where part of the flux rope struggle out of the overlying field lines, pushing some of them aside on the way, as simulated by Fan (2005). This paper might provide another example to illustrate that long-time prominence oscillation can be regarded as a precursor for CME eruptions, as proposed by Chen et al (2008). However, the eruption in this paper is different from theirs in the sense that their prominence oscillation was transverse, whereas ours is along the prominence axis, i.e., it is a longitudinal oscillation, although both of the prominence oscillations were probably triggered by magnetic reconnection between emerging flux and the pre-existing field lines.…”

Section: Possible Connection With the Later Cme/flaresupporting

confidence: 72%

“…With the main body of the prominence remaining undisturbed, a thread from the prominence was seen to erupt, leading to a CME and a C1.2-class flare. We tentatively propose that the prominence longitudinal oscillations studied in this paper might be a precursor of the CME/flare, which is related to the triggering process of the eruption, as proposed by Chen et al (2008).…”

Section: Discussionsupporting

confidence: 58%

“…Whatever mechanism is involved in triggering the eruption, the triggering process, as a kind of perturbation, should generate waves and oscillations in the prominence. Therefore, based on this line of thought and spectroscopic observations of an oscillating prominence prior to eruption, Chen et al (2008) proposed that long-time prominence oscillations can be considered as one of the precursors of CME eruptions. A prominence oscillation prior to eruption was also observed by Bocchialini et al (2011), and the oscillation was even able to be sustained until the eruption phase (Isobe & Tripathi 2006;Gosain et al 2009).…”

Section: Introductionmentioning

confidence: 99%

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Observations and simulations of longitudinal oscillations of an active region prominence

Zhang

Chen

Xia

et al. 2012

A&A

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128

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Context. Filament longitudinal oscillations have been observed in Hα observations of the solar disk. Aims. We intend to find an example of the longitudinal oscillations of a prominence, where the magnetic dip can be seen directly, and examine the restoring force of this type of oscillations. Methods. We carry out a multiwavelength data analysis of the active region prominence oscillations above the western limb on 2007 February 8. In addition, we perform a one-dimensional hydrodynamic simulation of the longitudinal oscillations. Results. Our analysis of high-resolution observations performed by Hinode/SOT indicate that the prominence, seen as a concaveinward shape in lower-resolution extreme ultraviolet (EUV) images, consists of many concave-outward threads, which is indicative of magnetic dips. After being injected into the dip region, a bulk of prominence material started to oscillate for more than 3.5 h, with the period of 52 min. The oscillation decayed with time, on the decay timescale 133 min. Our hydrodynamic simulation can reproduce the oscillation period, but the damping timescale in the simulation is 1.5 times as long as the observations. Conclusions. The results clearly show the prominence longitudinal oscillations around the dip of the prominence and our study suggests that the restoring force of the longitudinal oscillations might be the gravity. Radiation and heat conduction are insufficient to explain the decay of the oscillations. Other mechanisms, such as wave leakage and mass accretion, have to be considered. The possible relation between the longitudinal oscillations and the later eruption of a prominence thread, as well as a coronal mass ejection (CME), is also discussed.

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Section: Possible Connection With the Later Cme/flaresupporting

confidence: 72%

Section: Discussionsupporting

confidence: 58%

Section: Introductionmentioning

confidence: 99%

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Observations and simulations of longitudinal oscillations of an active region prominence

Zhang

Chen

Xia

et al. 2012

A&A

Self Cite

128

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“…The exciter of prominence oscillations does not seem to be related to flares or other activity that was reported before (e.g. Jing et al 2003;Okamoto et al 2004;Isobe & Tripathi 2006;Isobe et al 2007;Xu et al 2008;Chen et al 2008). It is generally thought that the thread oscillations stem from magnetoacoustic waves (e.g.…”

Section: Conclusion and Discussionmentioning

confidence: 80%

Small-scale oscillations in a quiescent prominence observed by HINODE/SOT

Ning¹,

Cao²,

Okamoto³

et al. 2009

A&A

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Context. Investigations of the behavior of small-scale threads can provide an alternative approach to studying prominence dynamics and understanding its origin and nature. Aims. The behavior of threads are analyzed in a quiescent prominence, including drifting and both the horizontally and vertically oscillating motions. These indicate waves in the solar prominence. Methods. We used the Hα images at a setting wavelength of +0.076 Å. A quiescent prominence was observed by HINODE/SOT on 2008 January 15 for about 3 h in total. Results. Consistent with previous findings, prominences show numerous thread-like structures. Some threads clearly exhibit both vertically and horizontally oscillatory motions, while others are only drifting. Complicated cases show both drifting and oscillatory motions simultaneously. In the upper part of the prominence, the threads are oscillating independently of each other. We find that three threads oscillate with the same phase for at least two periods. The oscillations seem to be strongly damped since they disappear after a few periods. The maximum number of observed periods is 8 in our observations. In the lower part of the prominence, however, the different threads have a mixed character with the individual oscillatory motions unstable for one entire period. Most oscillatory motions will disappear after a half period or less, while the new oscillatory motions are excited nearby. A 5-min period is predominant, and the oscillating amplitudes show an average value of ±3.5 km s −1 . We find some upflows in the spicule layer, and they appear to transport the mass from photosphere (or spicules themselves) to the prominence. These upflows have an average velocity amplitude of 0.8 km s −1 . Conclusions. The threads exhibit three distinct behaviors. The first is only drifting, the second is typically oscillating, and the third shows both characteristics. There are no substantial differences between the periods of horizontally and vertically oscillating threads in this prominence.

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“…SOHO/SUMER observations of a prominence oscillation were discussed in the context of the physics of CMEs (Chen et al 2008). It was suggested that repetitive reconnections between emerging flux and the pre-existing magnetic field are the trigger mechanism of Doppler velocity oscillations leading to the eruption.…”

Section: Introductionmentioning

confidence: 99%

Oscillatory motions observed in eruptive filaments

Bocchialini

Baudin

Koutchmy

et al. 2011

A&A

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Context. The origin of the variable component of the solar wind is of great intrinsic interest for heliophysics and spaceweather, e.g. the initiation of coronal mass ejections and the problem of mass loss of all stars. It is also related to the physics of coronal neutral sheets and streamers, which occur above lines of magnetic polarity reversal. Filaments and prominences correspond to the cool coronal component of these regions. Aims. We examine the dynamical behaviour of these structures where reconnection and dissipation of magnetic energy in the turbulent plasma are occurring. The link between the observed oscillatory motions and the eruption occurrence is investigated in detail for two different events. Methods. Two filaments were analysed using two different datasets: time series of spectra using a transition region line (He I at 584.33 Å) and a coronal line (Mg X at 609.79 Å) measured with CDS on-board SOHO, observed on May 30, 2003, and time series of intensity and velocity images from the NSO/Dunn Solar Telescope in the Hα line on September 18, 1994 for the other. The oscillatory content was investigated using Fourier transform and wavelet analysis and compared to different models. Results. In both filaments, oscillations are clearly observed, in intensity and velocity in the He I and Mg X lines, in velocity in Hα, with similar periods from a few minutes up to 80 min, with a main range from 20 to 30 min, simultaneously with eruptions. Both filaments exhibit vertical oscillating motions. For the filament observed in the UV (He I and Mg X lines), we provide evidence of damped velocity oscillations, and for the filament observed in the visible (Hα line), we provide evidence that parts of the filament are oscillating, while the filament is moving over the solar surface, before its disappearance.

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SOHO/SUMER observations of prominence oscillation before eruption

Cited by 85 publications

References 36 publications

Observations and simulations of longitudinal oscillations of an active region prominence

Observations and simulations of longitudinal oscillations of an active region prominence

Small-scale oscillations in a quiescent prominence observed by HINODE/SOT

Oscillatory motions observed in eruptive filaments

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