Volume 637, May 2020
|Number of page(s)||7|
|Section||The Sun and the Heliosphere|
|Published online||12 May 2020|
Transverse oscillations of a double-structured solar filament⋆
University of South Bohemia, Faculty of Science, Institute of Physics, Branišovská 1760, 370 05 České Budějovice, Czech Republic
2 Astronomical Institute of the Czech Academy of Sciences, Fričova 258, 251 65 Ondřejov, Czech Republic
3 Central (Pulkovo) Astronomical Observatory, Russian Academy of Sciences, Pulkovskoe Shausse 65, 196140 St. Petersburg, Russia
4 Crimean Astrophysical Observatory of the Russian Academy of Sciences Nauchny Russia, Russia
Accepted: 27 March 2020
Aims. We study the transverse oscillations of a double-structured solar filament.
Methods. We modelled the filament numerically via a 2D magnetohydrodynamic (MHD) model, in which we solved a full set of time-dependent MHD equations by means of the FLASH code, using the adaptive mesh refinement method. We used the wavelet analysis method as a diagnostic tool for analysing periods in simulated oscillations.
Results. We present a model of a solar filament combined with semi-empirical C7 model of the quiet solar atmosphere. This model is an alternative model of a filament based on the magnetostatic solution of MHD equations. We find that this double-structured filament oscillates with two different eigen frequencies. The ratio is approximately 1.75 (∼7.4 min/∼4.2 min), which is characteristic for this type of filament model. To show the details of these oscillations we present a time evolution of the plasma density, temperature, plasma beta parameter, and the ratio of gravity to magnetic pressure taken along the vertical axis of the filament at x = 0. The periods found by numerical simulations are then discussed in comparison with those observed.
Key words: Sun: filaments, prominences / Sun: oscillations / magnetohydrodynamics (MHD) / methods: numerical
The movie associated to Fig. 3 is available at https://www.aanda.org
© ESO 2020
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