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A new method for determining the helium abundance in the solar atmosphere

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Abstract

Recent observations of a cut-off frequency in the acoustic modes of the Sun (Claverie et al., 1981b) should help determine the mean molecular weight and, thereby, the helium abundance in the visible layers of the solar atmosphere. A first preliminary result of Y = 0.42 ± 0.04 is obtained for an assumed minimum photospheric temperature of 4400 K ± 200 K.

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Authors and Affiliations

  1. Department of Physics, University of Birmingham, P.O. Box 363, B15 2TT, Birmingham, UK

    G. R. Isaak

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  1. G. R. Isaak
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Additional information

Proceedings of the 66th IAU Colloquium: Problems in Solar and Stellar Oscillations, held at the Crimean Astrophysical Observatory, U.S.S.R., 1–5 September, 1981.

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Isaak, G.R. A new method for determining the helium abundance in the solar atmosphere. Sol Phys 82, 205–207 (1983). https://doi.org/10.1007/BF00145559

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  • DOI: https://doi.org/10.1007/BF00145559

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