<i>Hinode</i>
                    SOT Observations of Solar Quiescent Prominence Dynamics

Berger, Thomas; Shine, R. A.; Slater, G. L.; Tarbell, T. D.; Title, A. M.; Okamoto, Takenori J.; Ichimoto, Kiyoshi; Katsukawa, Y.; Suematsu, Y.; Tsuneta, S.; Lites, B. W.; Shimizu, Toshifumi

doi:10.1086/587171

Cited by 245 publications

(271 citation statements)

References 21 publications

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“…This is supported both by observations (e.g., Berger et al 2008;Lin et al 2005) and MHD simulations (e.g., Low & Petrie 2005). The effect of the increased penetration of the incident radiation, using multiple layer modelling, was also shown in 1D by Gouttebroze et al (2002).…”

Section: D Multi-thread Modelssupporting

confidence: 77%

2D non-LTE radiative modelling of He I spectral lines formed in solar prominences

Léger

Paletou

2009

A&A

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Context. The interpretation of high-resolution spectropolarimetric observations of solar prominences completed primarily at visible and near-infrared wavelengths, requires radiative modelling that takes into account both multi-dimensional geometry and complex atomic models.Aims. We enhance the interpretation of observations of He i multiplets, by considering 2D non-LTE unpolarized radiation transfer, and taking into account of the atomic fine-structure of helium. Methods. We apply our 2D non-LTE radiative transfer code, which is based on the multi-grid Gauss-Seidel/SOR iterative schemes.Results. It allows us to compute realistic emergent intensity profiles for the He i λ10 830 Å and D 3 multiplets, which can be directly compared to the simultaneous and high-resolution observations completed at THéMIS. A preliminary 2D multi-thread modelling is also discussed.

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Section: D Multi-thread Modelssupporting

confidence: 77%

2D non-LTE radiative modelling of He I spectral lines formed in solar prominences

Léger

Paletou

2009

A&A

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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%

“…Also, the presence in filaments of oscillating absorbing features which, at the same time, move along the filament axis has been reported (Lin 2004). In limb prominences different kinds of flows are observed (Chae et al 2008;Schmieder et al 2010) and, for instance, observations made by Berger et al (2008) with Hinode/SOT pointed out a complex dynamics with vertical downflows and upflows. In this case, velocities seem to be slightly higher than in filaments (up to 35 km s −1 ) and the orientation with respect to the magnetic field is unclear (Chae et al 2008;Schmieder et al 2010;Labrosse et al 2010).…”

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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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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“…Locally, they consist of fine and vertically oriented plasma structures, so-called threads, that evolve continually (e.g., Engvold 1976;Zirker et al 1994). Recent ob-A movie is available in electronic form at http://www.aanda.org 1 There are many papers about solar prominences, but we recommend that the reader first go through the historical work of Einar Tandberg-Hanssen (e.g., Tandberg-Hanssen 1998, 2011 servations taken with the Hinode satellite have revolutionized our knowledge of the fine-scale structuring and dynamics of quiescent prominences; for instance, plasma oscillations, supersonic downflows, or plasma instabilities like the Rayleigh-Taylor instability in prominence bubbles (Berger et al 2008(Berger et al , 2010Chae et al 2008;Okamoto et al 2007). …”

Section: Introductionmentioning

confidence: 99%

The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He i 10 830 Å triplet

Suárez

Ramos

Bueno

2014

A&A

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Context. Determining the magnetic field vector in quiescent solar prominences is possible by interpreting the Hanle and Zeeman effects in spectral lines. However, observational measurements are scarce and lack high spatial resolution. Aims. We determine the magnetic field vector configuration along a quiescent solar prominence by interpreting spectropolarimetric Results. For the most probable magnetic field vector configuration, the analysis depicts a mean field strength of 7 gauss. We do not find local variations in the field strength except that the field is, on average, lower in the prominence body than in the prominence feet, where the field strength reaches ∼25 gauss. The averaged magnetic field inclination with respect to the local vertical is ∼77 • . The acute angle of the magnetic field vector with the prominence main axis is 24 • for the sinistral chirality case and 58 • for the dextral chirality. These inferences are in rough agreement with previous results obtained from the analysis of data acquired with lower spatial resolutions.

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Hinode SOT Observations of Solar Quiescent Prominence Dynamics

Cited by 245 publications

References 21 publications

2D non-LTE radiative modelling of He I spectral lines formed in solar prominences

2D non-LTE radiative modelling of He I spectral lines formed in solar prominences

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

The magnetic field configuration of a solar prominence inferred from spectropolarimetric observations in the He i 10 830 Å triplet

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