Abstract
It is necessary to measure not only the wavelength but also the ‘strength’ of the Fraunhofer lines. This was done by Rowland according to an empirically estimated scale, established by looking at the lines of a spectrogram. The concept of ‘equivalent width’ gives a more quantitative estimate.
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Moore, CH. E., Minnaert, M. G. J., and Houtgast, J.: 1966 ‘The Solar Spectrum 3935Å to 8770Å, Nat. Bur. St., Monograph 61.
Mulders, G. F. W.: 1934, Aequivalente Breedten van Fraunhoferlijnen, Nijmegen; 1935, Z. Astrophys. 11, 132.
Wempe, J.: 1947, Astron. Nachr. 275, 97.
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© 1987 D. Reidel Publishing Company
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Kleczek, J. (1987). Equivalent Width of Fraunhofer Lines (L). In: Kleczek, J. (eds) Exercises in Astronomy. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3769-7_28
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DOI: https://doi.org/10.1007/978-94-009-3769-7_28
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