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Spectral Characteristics of the He i D3 Line in a Quiescent Prominence Observed by THEMIS

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Abstract

We analyze the observations of a quiescent prominence acquired by the Téléscope Heliographique pour l’Étude du Magnetisme et des Instabilités Solaires (THEMIS) in the He i 5876 Å (He i D3) multiplet aiming to measure the spectral characteristics of the He i D3 profiles and to find for them an adequate fitting model. The component characteristics of the He i D3 Stokes I profiles are measured by the fitting system by approximating them with a double Gaussian. This model yields an He i D3 component peak intensity ratio of \(5.5\pm0.4\), which differs from the value of 8 expected in the optically thin limit. Most of the measured Doppler velocities lie in the interval ± 5 km s−1, with a standard deviation of ± 1.7 km s−1 around the peak value of 0.4 km s−1. The wide distribution of the full-width at half maximum has two maxima at 0.25 Å and 0.30 Å for the He i D3 blue component and two maxima at 0.22 Å and 0.31 Å for the red component. The width ratio of the components is \(1.04\pm0.18\). We show that the double-Gaussian model systematically underestimates the blue wing intensities. To solve this problem, we invoke a two-temperature multi-Gaussian model, consisting of two double-Gaussians, which provides a better representation of He i D3 that is free of the wing intensity deficit. This model suggests temperatures of 11.5 kK and 91 kK, respectively, for the cool and the hot component of the target prominence. The cool and hot components of a typical He i D3 profile have component peak intensity ratios of 6.6 and 8, implying a prominence geometrical width of 17 Mm and an optical thickness of 0.3 for the cool component, while the optical thickness of the hot component is negligible. These prominence parameters seem to be realistic, suggesting the physical adequacy of the multi-Gaussian model with important implications for interpreting He i D3 spectropolarimetry by current inversion codes.

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Acknowledgements

We thank an anonymous referee for valuable comments, which improved the article substantially. J. Koza is grateful to P. Heinzel and E. Dzifčáková for fruitful discussions, comments, and suggestions. J. Koza and M. Kozák would like to thank B. Gelly, the director of the THEMIS solar telescope, and the technical team for their support during their THEMIS observing campaign. The authors thank M. Saniga for language corrections of the article. This work was supported by the Science Grant Agency project VEGA 2/0004/16. The THEMIS observations were taken within the EU-7FP-SOLARNET Transnational Access and Service Programme (High Resolution Solar Physics Network – FP7-INFRASTRUCTURES-2012-1). This article was created by the realization of the project ITMS No. 26220120029, based on the supporting operational Research and development program financed from the European Regional Development Fund. This work uses GONG data obtained by the NSO Integrated Synoptic Program (NISP), managed by the National Solar Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. The AIA data used here are courtesy of SDO (NASA) and the AIA consortium. The STEREO B data used here were produced by an international consortium of the Naval Research Laboratory (USA), Lockheed Martin Solar and Astrophysics Lab (USA), NASA Goddard Space Flight Center (USA), Rutherford Appleton Laboratory (UK), University of Birmingham (UK), Max-Planck-Institut for Solar System Research (Germany), Centre Spatiale de Liege (Belgium), Institut d’Optique Theorique et Appliquee (France), and Institut d’Astrophysique Spatiale (France). This research has made use of NASA Astrophysics Data System.

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  1. Astronomical Institute, Slovak Academy of Sciences, Tatranská Lomnica, Slovakia

    Július Koza, Ján Rybák, Peter Gömöry & Matúš Kozák

  2. UPS-OMP, Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, Toulouse, France

    Arturo López Ariste

  3. Institut de Recherche en Astrophysique et Planétologie, CNRS, 14 Avenue Edouard Belin, 31400, Toulouse, France

    Arturo López Ariste

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Koza, J., Rybák, J., Gömöry, P. et al. Spectral Characteristics of the He i D3 Line in a Quiescent Prominence Observed by THEMIS. Sol Phys 292, 98 (2017). https://doi.org/10.1007/s11207-017-1118-z

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