Abstract
We compare infrared hydrogen lines observed with ATMOS with computations for two models of the solar atmosphere, one without and one with a chromosphere. The weaker H I lines are formed in the photosphere. Proper evaluation of Stark broadening is required to reproduce their profiles; the heavy ion contribution is most important. The cores of the stronger lines are sensitive to the structure of the chromosphere, but detailed NLTE modeling is needed for diagnostic applications.
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© 1994 Springer Science+Business Media Dordrecht
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Carlsson, M., Rutten, R.J. (1994). Computation of Infrared Hydrogen Lines. In: Rabin, D.M., Jefferies, J.T., Lindsey, C. (eds) Infrared Solar Physics. International Astronomical Union / Union Astronomique Internationale, vol 154. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-1926-9_41
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DOI: https://doi.org/10.1007/978-94-011-1926-9_41
Publisher Name: Springer, Dordrecht
Print ISBN: 978-0-7923-2523-9
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