Volume 640, August 2020
|Number of page(s)||12|
|Section||The Sun and the Heliosphere|
|Published online||13 August 2020|
Determining the dynamics and magnetic fields in He I 10830 Å during a solar filament eruption⋆
Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
2 Astronomical Institute, Slovak Academy of Sciences (AISAS), 05960 Tatranská Lomnica, Slovak Republic
3 Instituto de Astrofísica de Canarias (IAC), Vía Láctea s/n, 38205 La Laguna, Tenerife, Spain
4 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain
5 Leibniz-Institut für Sonnenphysik (KIS), Schöneckstrasse 6, 79104 Freiburg im Breisgau, Germany
Accepted: 17 June 2020
Aims. We investigate the dynamics and magnetic properties of the plasma, including the line-of-sight velocity (LOS) and optical depth, as well as the vertical and horizontal magnetic fields, belonging to an erupted solar filament.
Methods. The filament eruption was observed with the GREGOR Infrared Spectrograph at the 1.5-meter GREGOR telescope on July 3, 2016. We acquired three consecutive full-Stokes slit-spectropolarimetric scans in the He I 10830 Å spectral range. The Stokes I profiles were classified using the machine learning k-means algorithm and then inverted with different initial conditions using the HAZEL code.
Results. The erupting-filament material presents the following physical conditions: (1) ubiquitous upward motions with peak LOS velocities of ∼73 km s−1; (2) predominant large horizontal components of the magnetic field, on average, in the range of 173−254 G, whereas the vertical components of the fields are much lower, on average between 39 and 58 G; (3) optical depths in the range of 0.7−1.1. The average azimuth orientation of the field lines between two consecutive raster scans (<2.5 min) remained constant.
Conclusions. The analyzed filament eruption belongs to the fast rising phase, with total velocities of about 124 km s−1. The orientation of the magnetic field lines does not change from one raster scan to the other, indicating that the untwisting phase has not yet started. The untwisting appears to start about 15 min after the beginning of the filament eruption.
Key words: Sun: filaments / prominences / Sun: chromosphere / Sun: magnetic fields / methods: data analysis / techniques: high angular resolution / techniques: polarimetric
Movies attached to Figs. 1 and 3 are available at https://www.aanda.org
© ESO 2020
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