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On the temperature of the helium emission regions in the solar atmosphere

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Abstract

An analysis of the spectral distribution of intensity of the Hei recombination continuum is probably the only direct method for determination of the electron temperature of helium emission regions on the Sun. On the basis of data on the Hei Lyman continuum, obtained by Dupree and Reeves from OSO-4, the electron temperature of undisturbed helium regions is determined: T e = = 12500 K. Such a low T e value is a serious argument in favour of the predominant role of UV coronal radiation in the helium ionization on the Sun. Comparison of the Hei Lyman continuum data with results of observations of the λ 10830 line showed that the visible helium lines and Hei Lyman continuum are produced within the same regions of the undisturbed solar atmosphere at T e = 12500 K.

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Authors and Affiliations

  1. Laboratory of Solar Activity, Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, Academy of Sciences of U.S.S.R., Moscow, U.S.S.R.

    R. A. Gulyaev

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  1. R. A. Gulyaev
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Gulyaev, R.A. On the temperature of the helium emission regions in the solar atmosphere. Sol Phys 24, 72–78 (1972). https://doi.org/10.1007/BF00231083

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  • DOI: https://doi.org/10.1007/BF00231083

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