Volume 631, November 2019
|Number of page(s)||12|
|Published online||11 November 2019|
2D non-LTE modelling of a filament observed in the Hα line with the DST/IBIS spectropolarimeter
Astronomical Institute of Slovak Academy of Sciences, 05960 Tatranská Lomnica, Slovak Republic
2 Astronomical Institute, The Czech Academy of Sciences, 25165 Ondřejov, Czech Republic
3 UCL-Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
4 Department of Physics & Astronomy, California State University, Northridge, CA 91330-8268, USA
Accepted: 26 September 2019
Context. We study a fragment of a large quiescent filament observed on May 29, 2017 by the Interferometric BIdimensional Spectropolarimeter (IBIS) mounted at the Dunn Solar Telescope. We focus on its quiescent stage prior to its eruption.
Aims. We analyse the spectral observations obtained in the Hα line to derive the thermodynamic properties of the plasma of the observed fragment of the filament.
Methods. We used a 2D filament model employing radiative transfer computations under conditions that depart from the local thermodynamic equilibrium. We employed a forward modelling technique in which we used the 2D model to produce synthetic Hα line profiles that we compared with the observations. We then found the set of model input parameters, which produces synthetic spectra with the best agreement with observations.
Results. Our analysis shows that one part of the observed fragment of the filament is cooler, denser, and more dynamic than its other part that is hotter, less dense, and more quiescent. The derived temperatures in the first part range from 6000 K to 10 000 K and in the latter part from 11 000 K to 14 000 K. The gas pressure is 0.2–0.4 dyn cm−2 in the first part and around 0.15 dyn cm−2 in the latter part. The more dynamic nature of the first part is characterised by the line-of-sight velocities with absolute values of 6–7 km s−1 and microturbulent velocities of 8–9 km s−1. On the other hand, the latter part exhibits line-of-sight velocities with absolute values 0–2.5 km s−1 and microturbulent velocities of 4–6 km s−1.
Key words: Sun: filaments / prominences / radiative transfer / line: profiles / techniques: spectroscopic / methods: data analysis / methods: numerical
© ESO 2019
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