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On the mean depth of line formation in a magnetic field

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Abstract

Probability interpretation of radiative transfer is used to calculate the contribution of different layers of the solar atmosphere to the emergent intensity. Generally the mean depths of line formation increase with increasing intensity; this is valid also for arbitrarily polarized constituents of a line formed in a magnetic field.

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Authors and Affiliations

  1. Zentralinstitut für Solar-Terrestrische Physik (HHI), Bereich C1, Sonnenobservatorium Einsteinturm, Potsdam, D.D.R.

    Jürgen Staude

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  1. Jürgen Staude
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Staude, J. On the mean depth of line formation in a magnetic field. Sol Phys 24, 255–261 (1972). https://doi.org/10.1007/BF00153366

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  • DOI: https://doi.org/10.1007/BF00153366

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