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Intensity fluctuations in Fraunhofer lines

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Abstract

An expression is derived for the fluctuation φ(t) in emergent intensity (observed at some wavelength λ in a Fraunhofer line or the continuum) caused by a perturbation in temperature θ(z, t) in the Sun's atmosphere. If the contribution function for the observed intensity is single-peaked near z λ and if θ(z) and p(z) are not too rapidly varying, then φ λ(t) ∼ m λη(z λ, t)+N λp(z λ, t) where m λ and N λ depend on the structure of the atmosphere. We compute M, N, and contribution functions for several values of μ and Δλ in the inner wings of the K line (λ13933 Caii).

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Authors and Affiliations

  1. High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colo., U.S.A.

    Frank Q. Orrall

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  1. Frank Q. Orrall
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Presently on leave of absence from the Institute for Astronomy, Honolulu, Hawaii.

The National Center for Atmospheric Research is sponsored by the National Science Foundation.

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Frank Q. Orrall Intensity fluctuations in Fraunhofer lines. Sol Phys 23, 30–46 (1972). https://doi.org/10.1007/BF00153890

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  • DOI: https://doi.org/10.1007/BF00153890

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