Filamentary electron-beam heating in solar flares

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F25%3A00619300" target="_blank" >RIV/67985815:_____/25:00619300 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0366066" target="_blank" >https://hdl.handle.net/11104/0366066</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/adc393" target="_blank" >10.3847/1538-4357/adc393</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Filamentary electron-beam heating in solar flares

Popis výsledku v původním jazyce

Radiation-hydrodynamic simulations of the solar-flare chromospheric emission very often lead to an excess of the line intensities when compared to observations. Various studies suggest that the flare loops have a certain intrinsic, multithread internal structure, which is still not resolved by current telescopes. Taking this into account, we want to test and compare two different approaches for flare simulations. The first approach is the commonly used one, based on a continuous flux of nonthermal electrons heating the chromosphere for a rather long time. In the second approach, we consider the heating by short beam pulses consecutively within spatially unresolved filaments. Superposition of these short-duration pulses gives us the same electron-beam flux as in the first approach, but we are showing that the filamentary heating generates lower intensities in both the H alpha and Mg ii k lines, as expected.

Název v anglickém jazyce

Filamentary electron-beam heating in solar flares

Popis výsledku anglicky

Radiation-hydrodynamic simulations of the solar-flare chromospheric emission very often lead to an excess of the line intensities when compared to observations. Various studies suggest that the flare loops have a certain intrinsic, multithread internal structure, which is still not resolved by current telescopes. Taking this into account, we want to test and compare two different approaches for flare simulations. The first approach is the commonly used one, based on a continuous flux of nonthermal electrons heating the chromosphere for a rather long time. In the second approach, we consider the heating by short beam pulses consecutively within spatially unresolved filaments. Superposition of these short-duration pulses gives us the same electron-beam flux as in the first approach, but we are showing that the filamentary heating generates lower intensities in both the H alpha and Mg ii k lines, as expected.

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/GA22-34841S" target="_blank" >GA22-34841S: Výzkum eruptivních procesů se sondou Solar Orbiter</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2025

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Svazek periodika

983

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

6

Strana od-do

155

Kód UT WoS článku

001469220900001

EID výsledku v databázi Scopus

2-s2.0-105003254154