Flows along arch filaments observed in the GRIS ‘very fast spectroscopic mode’

Manrique, S. J. González; Denker, C.; Kuckein, C.; Yabar, A. Pastor; Collados, M.; Balthasar, H.; Diercke, A.; Fischer, C. E.; Gömöry, P.; González, N. Bello; Schlichenmaier, R.; Armas, Melania Cubas; Berkefeld, T.; Feller, A.; Hoch, Sascha; Hofmann, Axel; Lagg, A.; Nicklas, H.; Suárez, D. Orozco; Schmidt, Dirk; Schmidt, Wolfgang; Sigwarth, M.; Sobotka, M.; Solanki, S. K.; Soltau, D.; Staude, J.; Strassmeier, K. G.; Volkmer, R.; Lühe, O. von der; Waldmann, T.

doi:10.1017/s1743921317000278

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“…Hence, the He I profiles are seen slightly in emission (Lagg et al 2007). On the contrary, Xu et al (2010) did not find any evidence for shocks in the He I triplet and, therefore, proposed that the shock occurs below the formation height of He I. This study is the continuation of González Manrique et al (2017bManrique et al ( , 2018, who studied the evolution of an AFS in He I. The goal of the present study is to follow the evolution of the plasma flows across several heights at the footpoints of an AFS.…”

Section: Introductionmentioning

confidence: 76%

“…The spectral region observed with GRIS comprises the photospheric Ca I 10839 Å and Si I 10827 Å lines, as well as the chromospheric He I 10830 Å triplet among others. González Manrique et al (2017bManrique et al ( , 2018 studied the same data set of GRIS in the very fast spectroscopic mode in the He I 10830 Å spectral line. This study builds on the results of the previously mentioned papers.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

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Tracking Downflows from the Chromosphere to the Photosphere in a Solar Arch Filament System

Manrique

Kuckein

Yabar

et al. 2020

ApJ

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We study the dynamics of plasma along the legs of an arch filament system (AFS) from the chromosphere to the photosphere, observed with high-cadence spectroscopic data from two ground-based solar telescopes: the GREGOR telescope (Tenerife) using the GREGOR Infrarred Spectrograph (GRIS) in the He I 10830 Å range and the Swedish Solar Telescope (La Palma) using the CRisp Imaging Spectro-Polarimeter to observe the Ca II 8542 Å and Fe I 6173 Å spectral lines. The temporal evolution of the draining of the plasma was followed along the legs of a single arch filament from the chromosphere to the photosphere. The average Doppler velocities inferred at the upper chromosphere from the He I 10830 Å triplet reach velocities up to 20 -24 km s −1 , in the lower chromosphere and upper photosphere the Doppler velocities reach up to 11 km s −1 and 1.5 km s −1 in the case of the Ca II 8542 Å and Si I 10827 Å spectral lines, respectively. The evolution of the Doppler velocities at different layers of the solar atmosphere (chromosphere and upper photosphere) shows that they follow the same LOS velocity pattern, which confirm the observational evidence that the plasma drains towards the photosphere as proposed in models of AFSs. The Doppler velocity maps inferred from the lower photospheric Ca I 10839 Å or Fe I 6173 Å spectral lines do not show the same LOS velocity pattern. Thus, there is no evidence that the plasma reaches the lower photosphere. The observations and the nonlinear force-free field extrapolations demonstrate that the magnetic field loops of the AFS rise with time. We found flow asymmetries at different footpoints of the AFS. The NLFFF values of the magnetic field strength give us a clue to explain these flow asymmetries.

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