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Transverse oscillations of a double-strutured solar filament View all abstracts by submitter

Petr Jelinek   Submitted: 2020-04-12 07:05

We study the transverse oscillations of a double-structured solar filament. We modelled the filament numerically via a 2-D 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 (AMR) method. We used the wavelet analysis method as a diagnostic tool for analysing periods in simulated oscillations. 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 eigenfrequencies. 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.

Authors: P. Jelínek, M. Karlický, V. V. Smirnova, A. A. Solov'ev
Projects: None

Publication Status: Accepted for publication in A&A
Last Modified: 2020-04-12 15:55
Go to main E-Print page  Simulating White-Light Images of Coronal Structures for Parker Solar Probe/WISPR: Study of the Total Brightness Profiles  Predicting Coronal Mass Ejections Using SDO/HMI Vector Magnetic Data Products and Recurrent Neural Networks  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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