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Comparison of effective depths of Fraunhofer line formation calculated by various methods

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Abstract

The effective depths of formation of some typical Fraunhofer lines, calculated by the methods suggested by Gurtovenko et al. (1974), Beckers and Milkey (1975), and Makita (1977) are compared.

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References

  • Beckers, J. M. and Milkey, R. W.: 1975, Solar Phys. 43, 289.

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  • Caccin, B. Gomez, M. T., Marmolino, C., and Severine, G.: 1977, Astron. Astrophys. 54, 227.

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  • Gurtovenko, E.: 1975, Solar Phys. 45, 25.

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  • Gurtovenko, E., Ratnikova, V., and De Jager, C.: 1974, Solar Phys. 37, 43.

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  • Lyubimkov, L. S.: 1977, Izv. Krym. Astrofiz. Obs. 57, 87.

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  • Makita, M.: 1977, Solar Phys. 45, 25.

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Authors and Affiliations

  1. Main Astronomical Observatory of the Ukrainian Academy of Sciences, Kiev, U.S.S.R.

    E. A. Gurtovenko & V. A. Ratnikova-Sheminova

Authors
  1. E. A. Gurtovenko
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  2. V. A. Ratnikova-Sheminova
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Gurtovenko, E.A., Ratnikova-Sheminova, V.A. Comparison of effective depths of Fraunhofer line formation calculated by various methods. Sol Phys 58, 241–242 (1978). https://doi.org/10.1007/BF00157269

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  • DOI: https://doi.org/10.1007/BF00157269

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