Transverse oscillations of a double-structured solar filament

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F60076658%3A12310%2F20%3A43901135" target="_blank" >RIV/60076658:12310/20:43901135 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/67985815:_____/20:00534078

Výsledek na webu

<a href="https://www.aanda.org/articles/aa/abs/2020/05/aa36836-19/aa36836-19.html" target="_blank" >https://www.aanda.org/articles/aa/abs/2020/05/aa36836-19/aa36836-19.html</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201936836" target="_blank" >10.1051/0004-6361/201936836</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Transverse oscillations of a double-structured solar filament

Popis výsledku v původním jazyce

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 (similar to 7.4 min/similar to 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.

Název v anglickém jazyce

Transverse oscillations of a double-structured solar filament

Popis výsledku anglicky

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 (similar to 7.4 min/similar to 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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2020

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astronomy &amp; Astrophysics

ISSN

1432-0746

e-ISSN

—

Svazek periodika

637

Číslo periodika v rámci svazku

MAY 12 2020

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

7

Strana od-do

—

Kód UT WoS článku

000534337300005

EID výsledku v databázi Scopus

2-s2.0-85089031610