Astrophysics and Space Science

, Volume 91, Issue 1, pp 157–165 | Cite as

Stellar chromospheric temperatures

  • G. A. Gurzadyan


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.


Hydrogen Physical Parameter Electron Temperature Mgii Emission Structure 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


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Copyright information

© D. Reidel Publishing Co. 1983

Authors and Affiliations

  • G. A. Gurzadyan
    • 1
  1. 1.Polytechnic InstituteErevanArmenian SSR, USSR

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