Large Amplitude Oscillations in Prominences

Tripathi, Durgesh; Isobe, Hiroaki; Jain, Rekha

doi:10.1007/s11214-009-9583-9

Cited by 121 publications

(105 citation statements)

References 46 publications

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“…The velocity amplitude was about 19 and 14 km s −1 for the lower and upper threads, respectively, significantly larger than that of small-amplitude oscillations (from 0.1 to several kilometers per second) that are apparently ever-present in prominences (Arregui et al 2012). The present observation therefore provides an alternative cause for large-amplitude prominence oscillations (velocity amplitude 20 km s −1 ), which are relatively rare and have been suggested to be triggered by waves and disturbances produced by flares or jets (Tripathi et al 2009). …”

Section: Flux Feedingmentioning

confidence: 66%

A Prominence Eruption Driven by Flux Feeding From Chromospheric Fibrils

Zhang

Wang

et al. 2014

ApJ

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We present multi-wavelength observations of a prominence eruption originating from a quadrupolar field configuration, in which the prominence was embedded in a side arcade. Within the two-day period prior to its eruption on 2012 October 22, the prominence was perturbed three times by chromospheric fibrils underneath, which rose upward, became brightened, and merged into the prominence, resulting in horizontal flows along the prominence axis, suggesting that the fluxes carried by the fibrils were incorporated into the magnetic field of the prominence. These perturbations caused the prominence to oscillate and to rise faster than before. The absence of intense heating within the first two hours after the onset of the prominence eruption, which followed an exponential increase in height, indicates that ideal instability played a crucial role. The eruption involved interactions with the other side arcade, leading up to a twin coronal mass ejection, which was accompanied by transient surface brightenings in the central arcade, followed by transient dimmings and brightenings in the two side arcades. We suggest that flux feeding from chromospheric fibrils might be an important mechanism to trigger coronal eruptions.

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Section: Flux Feedingmentioning

confidence: 66%

A Prominence Eruption Driven by Flux Feeding From Chromospheric Fibrils

Zhang

Wang

et al. 2014

ApJ

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“…Filament oscillations triggered by Moreton or coronal waves are often of large amplitude (>20 km s −1 ; see the review by Tripathi et al 2009), distinct from commonly observed smallamplitude oscillations (∼2-3 km s −1 ; see the review by Arregui et al 2012), which are usually local and seemingly intrinsic to the filament itself without any obvious trigger. The physical nature of the wave-filament interaction is not well understood as observations are relatively scarce (Ramsey & Smith 1966;Hyder 1966;Eto et al 2002;Okamoto et al 2004;Gilbert et al 2008;Hershaw et al 2011;Liu et al 2012b;Jackiewicz & Balasubramaniam 2013), and a filament does not always oscillate when a wave passes by (Okamoto et al 2004).…”

Section: Introductionmentioning

confidence: 98%

Observation of a Moreton Wave and Wave-Filament Interactions Associated With the Renowned X9 Flare on 1990 May 24

Liu

et al. 2013

ApJ

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Using Big Bear Solar Observatory film data recently digitized at NJIT, we investigate a Moreton wave associated with an X9 flare on 1990 May 24, as well as its interactions with four filaments F1-F4 located close to the flaring region. The interaction yields interesting insight into physical properties of both the wave and the filaments. The first clear Moreton wavefront appears at the flaring-region periphery at approximately the same time as the peak of a microwave burst and the first of two γ -ray peaks. The wavefront propagates at different speeds ranging from 1500-2600 km s −1 in different directions, reaching as far as 600 Mm away from the flaring site. Sequential chromospheric brightenings are observed ahead of the Moreton wavefront. A slower diffuse front at 300-600 km s −1 is observed to trail the fast Moreton wavefront about one minute after the onset. The Moreton wave decelerates to ∼550 km s −1 as it sweeps through F1. The wave passage results in F1's oscillation which is featured by ∼1 mHz signals with coherent Fourier phases over the filament, the activation of F3 and F4 followed by gradual recovery, but no disturbance in F2. Different height and magnetic environment together may account for the distinct responses of the filaments to the wave passage. The wavefront bulges at F4, whose spine is oriented perpendicular to the upcoming wavefront. The deformation of the wavefront is suggested to be due to both the forward inclination of the wavefront and the enhancement of the local Alfvén speed within the filament channel.

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“…The oscillations are categorised as either large amplitude oscillations, where the entire prominence oscillates with a velocity amplitude of the order of tens of km s −1 and periods ranging from around 6 to 150 min, or small amplitude oscillations which are localised to part of the prominence, and have velocity amplitudes of around 2-3 km s −1 and typical periods of 10 to 80 min. While small amplitude oscillations are very common (see Oliver & Ballester 2002), large amplitude oscillations are less widely reported and there are relatively few observational analyses (see the review by Tripathi et al 2009, their Table 1). …”

Section: Introductionmentioning

confidence: 99%

Damped large amplitude transverse oscillations in an EUV solar prominence, triggered by large-scale transient coronal waves

Hershaw

Foullon

Nakariakov

et al. 2011

A&A

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Aims. We investigate two successive trains of large amplitude transverse oscillations in an arched EUV prominence, observed with SoHO/EIT on the north-east solar limb on 30 July 2005. The oscillatory trains are triggered by two large scale coronal waves, associated with an X-class and a C-class flare occurring in the same remote active region. Methods. The oscillations are tracked within rectangular slits parallel to the solar limb at different heights, which are taken to move with the apparent height profile of the prominence to account for solar rotation. Time series for the two prominence arch legs are extracted using Gaussian fitting on the 195 Å absorption features, and fitted to a damped cosine curve to determine the oscillatory parameters.Results. Differing energies of the two triggering flares and associated waves are found to agree with the velocity amplitudes, of 50.6 ± 3.2 and 15.9 ± 8.0 km s −1 at the apex, for the first and second oscillatory trains respectively, as estimated in the transverse direction. The period of oscillation is similar for both trains, with an average of 99 ± 11 min, indicating a characteristic frequency as predicted by magnetohydrodynamics. Increasing velocity amplitude with height during the first oscillatory train, and in-phase starting motions of the two legs regardless of height, for each train, demonstrate that the prominence exhibits a global kink mode to a first approximation. However, discrepancies between the oscillatory characteristics of the two legs and an apparent dependence of period upon height, suggest that the prominence actually oscillates as a collection of separate but interacting threads. Damping times of around two to three cycles are observed. Combining our results with those of previously analysed loop oscillations, we find an approximately linear dependence of damping time upon period for kink oscillations, supporting resonant absorption as the damping mechanism despite limitations in testing this theory.

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Large Amplitude Oscillations in Prominences

Cited by 121 publications

References 46 publications

A Prominence Eruption Driven by Flux Feeding From Chromospheric Fibrils

A Prominence Eruption Driven by Flux Feeding From Chromospheric Fibrils

Observation of a Moreton Wave and Wave-Filament Interactions Associated With the Renowned X9 Flare on 1990 May 24

Damped large amplitude transverse oscillations in an EUV solar prominence, triggered by large-scale transient coronal waves

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