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The Calculation of the Intensity of The Mg I Spectral Lines in Solar Prominences Using the Cloudy code Modelстатья
- Авторы: Kupryakov Yu A., Dodin A.V., Schwartz P., Kashapova L.K.
- Сборник: Proceedings of Eleventh Workshop “Solar Influences on the Magnetosphere, Ionosphere and Atmosphere”
- Глава в коллективной монографии
- Год издания: 2019
- Место издания: Primorsko, Bulgaria
- Первая страница: 139
- Последняя страница: 142
- DOI: 10.31401/WS.2019.proc
- Аннотация: Spectroscopical observations of several prominences in the MgI lines were carried out from 2014 to 2017. These lines from visible part of the solar spectrum play an important diagnostic role, complementing the UV Mg II resonance lines regularly observed by the IRIS satellite. We found that a rather weak Mg I emission, e.g., in the 5172.6 Å line correlates well with the presence of extended bright areas on the solar disk observed in the 1600 Å SDO/AIA band. However, in many cases the radiation in the 5172.6 Å line is very low, even not detectable, although a bright prominence above the limb or flare on the solar disc were observed. To explain this phenomenon, we have calculated spectra of optically thin plasma using Cloudy code and found that observed ratio of optical lines and UV continuum is possible and the presence of heel processes stimulates luminescence in Mg I and 1600 Å lines.
- Добавил в систему: Купряков Юрий Алексеевич