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Stellar chromospheric temperatures

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The emission doublet 2800 Mgii of stellar chromospheric origin is always stronger than the emission in the Lα line of hydrogen. At the same time, the ratio of their fluxes,Q=F(Mgii)/F(Lα), varies over a wide range— from 2 up to 20 in stars of one and the same type. Assuming that both emission structures, 2800 Mgii and Lα, are excited in one and the same region of the chromosphere, an attempt is made to represent the ratioQ as a function from one physical parameter only—chromospheric electron temperature. Such an approach explains easily the observed behaviour of the ratioQ in different stars.

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Gurzadyan, G.A. Stellar chromospheric temperatures. Astrophys Space Sci 91, 157–165 (1983). https://doi.org/10.1007/BF00650221

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  • Hydrogen
  • Physical Parameter
  • Electron Temperature
  • Mgii
  • Emission Structure