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Abstract <p>We observed M1.9 class solar flare in NOAA 10808 active region by the HSFA spectrograph of Ondřejov observatory. We registered emission in hydrogen H<InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(\alpha\)</EquationSource> <!--BPhysMGU2570220Maliutin-m1--> </InlineEquation>, H<InlineEquation ID="IEq2"> <EquationSource Format="TEX">\(\beta\)</EquationSource> <!--BPhysMGU2570220Maliutin-m2--> </InlineEquation>, H<InlineEquation ID="IEq3"> <EquationSource Format="TEX">\(\varepsilon\)</EquationSource> <!--BPhysMGU2570220Maliutin-m3--> </InlineEquation> lines and in H, K CaII lines. After the spectra processing the integral emission fluxes were derived. In the Joule heating framework we conducted calculation of gas parameters utilizing the physical conditions of the chromosphere, particularly self-absorbtion at spectral lines. All general populating and depopulating processes of discrete energetic levels were taken into account. We considered model of gas layers oriented perpendicular to the line of sight. Registered emission in five lines needed two-layered model for interpretation. The farther one has temperature <InlineEquation ID="IEq4"> <EquationSource Format="TEX">\(7300\)</EquationSource> <!--BPhysMGU2570220Maliutin-m4--> </InlineEquation> K and concentration <InlineEquation ID="IEq5"> <EquationSource Format="TEX">\(\sim 10^{14}\)</EquationSource> <!--BPhysMGU2570220Maliutin-m5--> </InlineEquation> cm<InlineEquation ID="IEq6"> <EquationSource Format="TEX">\({}^{-3}\)</EquationSource> <!--BPhysMGU2570220Maliutin-m6--> </InlineEquation>. The nearby layer has has temperature <InlineEquation ID="IEq7"> <EquationSource Format="TEX">\(30000\)</EquationSource> <!--BPhysMGU2570220Maliutin-m7--> </InlineEquation> K and concentration <InlineEquation ID="IEq8"> <EquationSource Format="TEX">\(\sim 10^{12}\)</EquationSource> <!--BPhysMGU2570220Maliutin-m8--> </InlineEquation> cm<InlineEquation ID="IEq9"> <EquationSource Format="TEX">\({}^{-3}\)</EquationSource> <!--BPhysMGU2570220Maliutin-m9--> </InlineEquation>.</p>

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Observations and Theoretical Calculation of Emission in Calcium and Hydrogen Lines for the SOL2005-09-10 Flare

  • 期刊论文

  • 发表日期：

    2025年12月1日

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  • V. A. Maliutin,
  • Yu. A. Kupryakov,
  • K. V. Bychkov,
  • O. M. Belova,
  • A. B. Gorshkov

摘要

Abstract

We observed M1.9 class solar flare in NOAA 10808 active region by the HSFA spectrograph of Ondřejov observatory. We registered emission in hydrogen H \(\alpha\) , H \(\beta\) , H \(\varepsilon\) lines and in H, K CaII lines. After the spectra processing the integral emission fluxes were derived. In the Joule heating framework we conducted calculation of gas parameters utilizing the physical conditions of the chromosphere, particularly self-absorbtion at spectral lines. All general populating and depopulating processes of discrete energetic levels were taken into account. We considered model of gas layers oriented perpendicular to the line of sight. Registered emission in five lines needed two-layered model for interpretation. The farther one has temperature \(7300\) K and concentration \(\sim 10^{14}\) cm \({}^{-3}\) . The nearby layer has has temperature \(30000\) K and concentration \(\sim 10^{12}\) cm \({}^{-3}\) .