First comparison of FLARIX simulations with MSDP observation of the C1.6 Solar flare in the Hα line of hydrogen

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F24%3A00602920" target="_blank" >RIV/67985815:_____/24:00602920 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0360344" target="_blank" >https://hdl.handle.net/11104/0360344</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/ad8ba9" target="_blank" >10.3847/1538-4357/ad8ba9</a>

Jazyk výsledku

angličtina

Název v původním jazyce

First comparison of FLARIX simulations with MSDP observation of the C1.6 Solar flare in the Hα line of hydrogen

Popis výsledku v původním jazyce

The primary objective of this study is to develop a time-dependent model of the flaring atmosphere based on observational data. Here, we present, for the first time, a comparison between numerical simulations of the flaring emission, specifically focusing on the hydrogen H alpha line, utilizing the FLARIX code and spectral observations of a compact C1.6 GOES-class flare observed on 2012 September 10, by the MSDP imaging spectrograph installed at the Białków Observatory. The Multichannel Subtractive Double Pass imaging spectrograph spectral data, collected with a temporal resolution as fine as 50 ms, enabled a comprehensive analysis of H alpha line profiles and light curves measured within an area of the flare's emission. An initial atmospheric model close to VAL-C, with a modified temperature in the upper chromosphere, was employed in simulations. To enhance temporal resolution, modulations of the nonthermal electron (NTE) beam's parameters were introduced based on variations in observed hard X-ray (HXR) flux (using RHESSI data). The synthesized H alpha line profiles were compared with the observed spectra. During the impulsive phase of the flare, the evolution of the observed and synthetic H alpha line intensity agrees, but discrepancies were found in intensities at specific wavelengths of the H alpha line profile. Fluctuations in the energy flux of NTEs exhibited a strong correlation with the H alpha emission during the HXR pulse. After considering various effects (such as the filling factor FF = 0.20) that could influence observed emissions, relatively good agreement between theoretical and observed lines was achieved.

Název v anglickém jazyce

First comparison of FLARIX simulations with MSDP observation of the C1.6 Solar flare in the Hα line of hydrogen

Popis výsledku anglicky

The primary objective of this study is to develop a time-dependent model of the flaring atmosphere based on observational data. Here, we present, for the first time, a comparison between numerical simulations of the flaring emission, specifically focusing on the hydrogen H alpha line, utilizing the FLARIX code and spectral observations of a compact C1.6 GOES-class flare observed on 2012 September 10, by the MSDP imaging spectrograph installed at the Białków Observatory. The Multichannel Subtractive Double Pass imaging spectrograph spectral data, collected with a temporal resolution as fine as 50 ms, enabled a comprehensive analysis of H alpha line profiles and light curves measured within an area of the flare's emission. An initial atmospheric model close to VAL-C, with a modified temperature in the upper chromosphere, was employed in simulations. To enhance temporal resolution, modulations of the nonthermal electron (NTE) beam's parameters were introduced based on variations in observed hard X-ray (HXR) flux (using RHESSI data). The synthesized H alpha line profiles were compared with the observed spectra. During the impulsive phase of the flare, the evolution of the observed and synthetic H alpha line intensity agrees, but discrepancies were found in intensities at specific wavelengths of the H alpha line profile. Fluctuations in the energy flux of NTEs exhibited a strong correlation with the H alpha emission during the HXR pulse. After considering various effects (such as the filling factor FF = 0.20) that could influence observed emissions, relatively good agreement between theoretical and observed lines was achieved.

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

2024

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

977

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

11

Strana od-do

132

Kód UT WoS článku

001372783200001

EID výsledku v databázi Scopus

2-s2.0-85212081547