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Gouttebroze, P.; Vial, J. C.; Heinzel, P.

doi:10.1023/a:1004986608429

Cited by 72 publications

(107 citation statements)

References 3 publications

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“…The normalization of Hα intensity allows observations to be compared with theoretical Hα profiles provided by radiative transfer codes (Gouttebroze et al 1993;Heinzel et al 2005) leading to the determination of physical quantities of prominences. This step is beyond the scope of this paper.…”

Section: Normalization Of the Hα Intensitiesmentioning

confidence: 99%

Velocity vectors of a quiescent prominence observed byHinode/SOT and the MSDP (Meudon)

Schmieder¹,

Chandra²,

Berlicki

et al. 2010

A&A

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Context. The dynamics of prominence fine structures present a challenge to our understanding of the formation of cool plasma prominence embedded in the hot corona. Aims. Observations performed by the high resolution Hinode/SOT telescope allow us to compute velocities perpendicular to the lineof-sight or transverse velocities. Combining simultaneous observations obtained in Hα with Hinode/SOT and the MSDP spectrograph operating in the Meudon solar tower, we derive the velocity vectors of a quiescent prominence. Methods. The velocities perpendicular to the line-of-sight are measured using a time-slice technique and the Doppler shifts velocity using the bisector method.Results. The Doppler shifts of bright threads derived from the MSDP show counterstreaming of the order of 5 km s −1 in the prominence and reaching 15 km s −1 at the edges of the prominence. Even though they are minimum values because of seeing effects, they are of the same order as the transverse velocities. Conclusions. These measurements are very important because they suggest that the vertical structures detected by SOT may not be true vertical magnetic structures in the sky plane. The vertical structures could be a pile up of dips in more or less horizontal magnetic field lines in a 3D perspective, as proposed by many MHD modelers. In our analysis, we also calibrate the Hinode Hα data using MSDP observations obtained simultaneously.

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Section: Normalization Of the Hα Intensitiesmentioning

confidence: 99%

Velocity vectors of a quiescent prominence observed byHinode/SOT and the MSDP (Meudon)

Schmieder¹,

Chandra²,

Berlicki

et al. 2010

A&A

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show abstract

“…Such models were first developed by Poland & Anzer (1971) and Heasley & Mihalas (1976). Later, Gouttebroze et al (1993) used a sophisticated hydrogen atom with more than 20 levels plus continuum and a large grid of 1D isothermal isobaric slab models. This was followed by Anzer & Heinzel (1998, 1999, who developed 1D magnetohydrostatic equilibrium models of the Kippenhahn-Schlüter (K-S) type.…”

Section: Introductionmentioning

confidence: 99%

Non-LTE modelling of prominence fine structures using hydrogen Lyman-line profiles

Schwartz

Gunár

Curdt

2015

A&A

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Aims. We perform a detailed statistical analysis of the spectral Lyman-line observations of the quiescent prominence observed on May 18, 2005. Methods. We used a profile-to-profile comparison of the synthetic Lyman spectra obtained by 2D single-thread prominence finestructure model as a starting point for a full statistical analysis of the observed Lyman spectra. We employed 2D multi-thread finestructure models with random positions and line-of-sight velocities of each thread to obtain a statistically significant set of synthetic Lyman-line profiles. We used for the first time multi-thread models composed of non-identical threads and viewed at line-of-sight angles different from perpendicular to the magnetic field. Results. We investigated the plasma properties of the prominence observed with the SoHO/SUMER spectrograph on May 18, 2005 by comparing the histograms of three statistical parameters characterizing the properties of the synthetic and observed line profiles. In this way, the integrated intensity, Lyman decrement ratio, and the ratio of intensity at the central reversal to the average intensity of peaks provided insight into the column mass and the central temperature of the prominence fine structures.

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“…Results for the hydrogen atom have been compared with those of Heasley & Milkey (1983), Gouttebroze et al (1993), andPaletou (1995). Results for the helium atom have been compared mainly with Labrosse & Gouttebroze (2001, 2004.…”

Section: Resultsmentioning

confidence: 99%

“…Its temperature is T = 8000 K, and its gas pressure is p g = 0.05 dyn cm −2 , which are typical values for modelling quiescent prominences (see e.g., Gouttebroze et al 1993). The microturbulent velocity is ξ = 5 km s −1 .…”

Section: Single Slab Modelsmentioning

confidence: 93%

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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Cited by 72 publications

References 3 publications

Velocity vectors of a quiescent prominence observed byHinode/SOT and the MSDP (Meudon)

Velocity vectors of a quiescent prominence observed byHinode/SOT and the MSDP (Meudon)

Non-LTE modelling of prominence fine structures using hydrogen Lyman-line profiles

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

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