Abstract
Fraunhofer lines are not really black. Inside each line the brightness varies according to very characteristic laws, connected with the structure of the outer solar layers. Such a ‘profile’ should be determined on high resolution spectrograms by means of a microphotometer, which measures the transmission inside very narrow strips. Our simple microphotometer does not satisfy such high requirements but will give interesting results just the same.
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References
Unsöld, A.: 1955, Physik der Sternatmosphären, Kapitel IX, Springer, Berlin.
Wright, K. O.: 1962, in Stars and Stellar Systems, Part II, chapter 4, Chicago.
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© 1987 D. Reidel Publishing Company
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Kleczek, J. (1987). Profiles of Fraunhofer Lines (L). In: Kleczek, J. (eds) Exercises in Astronomy. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3769-7_27
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DOI: https://doi.org/10.1007/978-94-009-3769-7_27
Publisher Name: Springer, Dordrecht
Print ISBN: 978-90-277-2423-6
Online ISBN: 978-94-009-3769-7
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