Evolution of photospheric flows under an erupting filament in the quiet-Sun region

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F20%3A00534857" target="_blank" >RIV/67985815:_____/20:00534857 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1051/0004-6361/202037525" target="_blank" >https://doi.org/10.1051/0004-6361/202037525</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202037525" target="_blank" >10.1051/0004-6361/202037525</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Evolution of photospheric flows under an erupting filament in the quiet-Sun region

Popis výsledku v původním jazyce

We studied the dynamics of the solar atmosphere in the region of a large quiet-Sun filament, which erupted on 21 October 2010. The filament eruption started at its northern end and disappeared from the H alpha line-core filtergrams line within a few hours. The very fast motions of the northern leg were recorded in ultraviolet light by the Atmospheric Imaging Assembly (AIA) imager. We aim to study a wide range of available datasets describing the dynamics of the solar atmosphere for five days around the filament eruption. This interval covers three days of the filament evolution, one day before the filament growth and one day after the eruption. We search for possible triggers that lead to the eruption of the filament.

Název v anglickém jazyce

Evolution of photospheric flows under an erupting filament in the quiet-Sun region

Popis výsledku anglicky

We studied the dynamics of the solar atmosphere in the region of a large quiet-Sun filament, which erupted on 21 October 2010. The filament eruption started at its northern end and disappeared from the H alpha line-core filtergrams line within a few hours. The very fast motions of the northern leg were recorded in ultraviolet light by the Atmospheric Imaging Assembly (AIA) imager. We aim to study a wide range of available datasets describing the dynamics of the solar atmosphere for five days around the filament eruption. This interval covers three days of the filament evolution, one day before the filament growth and one day after the eruption. We search for possible triggers that lead to the eruption of the filament.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA18-06319S" target="_blank" >GA18-06319S: Vývoj slunečních skvrn a aktivních oblastí</a><br>

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 & Astrophysics

ISSN

1432-0746

e-ISSN

—

Svazek periodika

636

Číslo periodika v rámci svazku

April

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

10

Strana od-do

A102

Kód UT WoS článku

000530353600001

EID výsledku v databázi Scopus

2-s2.0-85094137289