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

Result code in 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>

Result on the web

<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>

Result language

angličtina

Original language name

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

Original language description

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.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

—

OECD FORD branch

10308 - Astronomy (including astrophysics,space science)

Project

<a href="/en/project/GA22-34841S" target="_blank" >GA22-34841S: Science with Solar Orbiter: Focusing on eruptive processes</a><br>

Continuities

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year

2024

Confidentiality

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

Name of the periodical

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Volume of the periodical

977

Issue of the periodical within the volume

1

Country of publishing house

GB - UNITED KINGDOM

Number of pages

11

Pages from-to

132

UT code for WoS article

001372783200001

EID of the result in the Scopus database

2-s2.0-85212081547