Two-dimensional distribution of oscillations in a 
quiescent solar prominence

Terradas, J.; Molowny‐Horas, Roberto; Wiehr, E.; Balthasar, H.; Oliver, R.; Ballester, J. L.

doi:10.1051/0004-6361:20020967

Cited by 88 publications

(156 citation statements)

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“…Observational evidence of the time damping of small amplitude oscillations in prominences has been reported by Landman (1977), Tsubaki & Takeuchi (1986), Tsubaki (1988), Wiehr et al (1989), Molowny-Horas et al (1999), Terradas et al (2002), Lin (2004), Berger et al (2008) and Ning et al (2009a,b). MolownyHoras et al (1999) and Terradas et al (2002) studied twodimensional time series from a quiescent prominence and found that oscillations detected in large areas of the prominence were typically damped after 2−3 periods.…”

Section: Introductionmentioning

confidence: 83%

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Time damping of non-adiabatic magnetohydrodynamic waves in a partially ionised prominence medium: Effect of a background flow

Barceló

Carbonell

Ballester

2010

A&A

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Context. The simultaneous occurrence of flows and time damped small-amplitude oscillations in solar prominences is a common phenomenon. These oscillations are mostly interpreted in terms of magnetohydrodynamic (MHD) waves. Aims. We study the time damping of linear non-adiabatic MHD waves in a flowing partially ionised plasma with prominence-like physical conditions. Methods. Considering non-adiabatic single fluid equations for a partially ionised hydrogen plasma, we have solved our dispersion relations for the complex frequency, ω, and we have analysed the behavior of the period, damping time and the ratio of the damping time to the period, versus the real wavenumber k, for Alfvén, fast, slow, and thermal waves. Results. While in the case without flow there is a critical wavenumber at which the period of Alfvén and fast waves goes to infinite, when a flow is present two different critical wavenumbers appear. The smaller wavenumber depends on the flow speed and causes the period of the high-period branch to go to infinite. When the second critical wavenumber is attained the period of both branches become equal. In general, the time damping of Alfvén and fast waves is dominated by resistive effects, and its damping ratio is very inefficient when compared to observations. The damping of slow and thermal waves is basically dominated by non-adiabatic effects, and for slow waves it is possible to obtain a damping ratio close to observations, although it would correspond to long period oscillations with large damping times not often observed. The consideration of a structured medium produces new features such as the apparition of four critical wavenumbers for Alfvén waves, and one critical wavenumber for slow waves. For fast waves, constrained propagation substantially improves, within the range of observed wavelengths, the ratio of the damping time to period. Conclusions. The presence of a background flow in a partially ionised plasma gives place to new interesting features when the time damping of MHD waves is studied. In general, the results point out that ion-neutral collisions are an inefficient mechanism to explain the observed time damping of prominence oscillations if they are produced by Alfvén and fast waves. If the oscillations are produced by slow waves, only long period oscillations with large damping times produce damping ratios in agreement with observations.

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Section: Introductionmentioning

confidence: 83%

“…MolownyHoras et al (1999) and Terradas et al (2002) studied twodimensional time series from a quiescent prominence and found that oscillations detected in large areas of the prominence were typically damped after 2−3 periods. Similar results have been obtained recently by Mashnich et al (2009).…”

Section: Introductionmentioning

confidence: 99%

Time damping of non-adiabatic magnetohydrodynamic waves in a partially ionised prominence medium: Effect of a background flow

Barceló

Carbonell

Ballester

2010

A&A

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“…For instance, Terradas et al (2002) reported the existence of large regions with periodic Doppler (line of sight) velocity oscillations having similar periods, around 75 minutes, noticing also that the oscillatory amplitude tends to decrease in time in such a way that the periodicity totally disappears after a few periods. Reliable values for the damping time, τ D , have been derived from different Doppler velocity time series by Molowny-Horas et al (1999) and Terradas et al (2002). The values of τ D thus obtained are usually between 1 and 4 times the corresponding period, and large regions of the prominence display similar damping times.…”

Section: Ground-based Observationsmentioning

confidence: 99%

“…The values of τ D thus obtained are usually between 1 and 4 times the corresponding period, and large regions of the prominence display similar damping times. Also, Terradas et al (2002) reported the presence, along two selected paths in the prominence region, of plane propagating waves as well as a standing wave. The plane waves propagate in opposite directions with wavelengths of 67,500 and 50,000 km and phase speeds of 15 km s −1 and 12 km s −1 , respectively, while in the case of the standing wave the estimated wavelength is 44,000 km and a phase speed is 12 km s −1 .…”

Section: Ground-based Observationsmentioning

confidence: 99%

Physics of Solar Prominences: II—Magnetic Structure and Dynamics

et al. 2010

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Observations and models of solar prominences are reviewed. We focus on non-eruptive prominences, and describe recent progress in four areas of prominence research: (1) magnetic structure deduced from observations and models, (2) the dynamics of prominence plasmas (formation and flows), (3) Magneto-hydrodynamic (MHD) waves in prominences and (4) the formation and large-scale patterns of the filament channels in which prominences are located. Finally, several outstanding issues in prominence research are discussed, along with observations and models required to resolve them.

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“…Nakariakov et al 1999;Aschwanden et al 2002) and small amplitude prominence oscillations (e.g. Molowny-Horas et al 1999;Terradas et al 2002), and the damping theories in these fields are more developed.…”

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

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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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Two-dimensional distribution of oscillations in a quiescent solar prominence

Cited by 88 publications

References 15 publications

Time damping of non-adiabatic magnetohydrodynamic waves in a partially ionised prominence medium: Effect of a background flow

Time damping of non-adiabatic magnetohydrodynamic waves in a partially ionised prominence medium: Effect of a background flow

Physics of Solar Prominences: II—Magnetic Structure and Dynamics

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

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