First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen
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 α line, utilizing the FLAR...
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2024-01-01
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| author | Krzysztof Radziszewski Petr Heinzel Jana Kašparová Michalina Litwicka Arkadiusz Berlicki Paweł Rudawy Robert Falewicz |
| author_facet | Krzysztof Radziszewski Petr Heinzel Jana Kašparová Michalina Litwicka Arkadiusz Berlicki Paweł Rudawy Robert Falewicz |
| author_sort | Krzysztof Radziszewski |
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| 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 α 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 α 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 α line profiles were compared with the observed spectra. During the impulsive phase of the flare, the evolution of the observed and synthetic H α line intensity agrees, but discrepancies were found in intensities at specific wavelengths of the H α line profile. Fluctuations in the energy flux of NTEs exhibited a strong correlation with the H α 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. |
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| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-cc99b47cfb3d49d6a9fae620280c13e32025-08-20T02:20:21ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01977113210.3847/1538-4357/ad8ba9First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of HydrogenKrzysztof Radziszewski0https://orcid.org/0000-0003-0310-1598Petr Heinzel1https://orcid.org/0000-0002-5778-2600Jana Kašparová2https://orcid.org/0000-0001-9559-4136Michalina Litwicka3https://orcid.org/0000-0001-5843-7473Arkadiusz Berlicki4https://orcid.org/0000-0002-6505-4478Paweł Rudawy5https://orcid.org/0000-0002-3989-1619Robert Falewicz6https://orcid.org/0000-0003-1853-2809Astronomical Institute, University of Wrocław , 51-622 Wrocław, ul. Kopernika 11, Poland ; krzysztof.radziszewski@uwr.edu.pl, pawel.rudawy@uwr.edu.pl, robert.falewicz@uwr.edu.pl, arkadiusz.berlicki@uwr.edu.plCenter of Excellence—Solar and Stellar Activity, University of Wrocław , ul. Kopernika 11, 51-622 Wrocław, Poland ; petr.heinzel@asu.cas.cz, michalina.litwicka@uwr.edu.pl; Astronomical Institute of the Czech Academy of Sciences , 251 65 Ondřejov, Czech Republic ; jana.kasparova@asu.cas.czAstronomical Institute of the Czech Academy of Sciences , 251 65 Ondřejov, Czech Republic ; jana.kasparova@asu.cas.czCenter of Excellence—Solar and Stellar Activity, University of Wrocław , ul. Kopernika 11, 51-622 Wrocław, Poland ; petr.heinzel@asu.cas.cz, michalina.litwicka@uwr.edu.plAstronomical Institute, University of Wrocław , 51-622 Wrocław, ul. Kopernika 11, Poland ; krzysztof.radziszewski@uwr.edu.pl, pawel.rudawy@uwr.edu.pl, robert.falewicz@uwr.edu.pl, arkadiusz.berlicki@uwr.edu.pl; Center of Excellence—Solar and Stellar Activity, University of Wrocław , ul. Kopernika 11, 51-622 Wrocław, Poland ; petr.heinzel@asu.cas.cz, michalina.litwicka@uwr.edu.pl; Astronomical Institute of the Czech Academy of Sciences , 251 65 Ondřejov, Czech Republic ; jana.kasparova@asu.cas.czAstronomical Institute, University of Wrocław , 51-622 Wrocław, ul. Kopernika 11, Poland ; krzysztof.radziszewski@uwr.edu.pl, pawel.rudawy@uwr.edu.pl, robert.falewicz@uwr.edu.pl, arkadiusz.berlicki@uwr.edu.plAstronomical Institute, University of Wrocław , 51-622 Wrocław, ul. Kopernika 11, Poland ; krzysztof.radziszewski@uwr.edu.pl, pawel.rudawy@uwr.edu.pl, robert.falewicz@uwr.edu.pl, arkadiusz.berlicki@uwr.edu.plThe 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 α 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 α 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 α line profiles were compared with the observed spectra. During the impulsive phase of the flare, the evolution of the observed and synthetic H α line intensity agrees, but discrepancies were found in intensities at specific wavelengths of the H α line profile. Fluctuations in the energy flux of NTEs exhibited a strong correlation with the H α 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.https://doi.org/10.3847/1538-4357/ad8ba9Solar flaresSolar flare spectraSolar x-ray flaresSolar x-ray emissionAstronomy data analysisSolar chromospheric heating |
| spellingShingle | Krzysztof Radziszewski Petr Heinzel Jana Kašparová Michalina Litwicka Arkadiusz Berlicki Paweł Rudawy Robert Falewicz First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen The Astrophysical Journal Solar flares Solar flare spectra Solar x-ray flares Solar x-ray emission Astronomy data analysis Solar chromospheric heating |
| title | First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen |
| title_full | First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen |
| title_fullStr | First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen |
| title_full_unstemmed | First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen |
| title_short | First Comparison of FLARIX Simulations with MSDP Observation of the C1.6 Solar Flare in the Hα Line of Hydrogen |
| title_sort | first comparison of flarix simulations with msdp observation of the c1 6 solar flare in the hα line of hydrogen |
| topic | Solar flares Solar flare spectra Solar x-ray flares Solar x-ray emission Astronomy data analysis Solar chromospheric heating |
| url | https://doi.org/10.3847/1538-4357/ad8ba9 |
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