Physical Conditions in Solar Coronal Holes on the Base of Non-LTE Calculations

Malanushenko, E.; Baranovsky, E.

doi:10.1007/978-94-010-0760-3_14

E. Malanushenko³ &
E. Baranovsky³

Part of the book series: Astrophysics and Space Science Library ((ASSL,volume 259))

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Abstract

We show that the intensity variations of the He I 10830 Å and the H Ly_α lines which are observed in coronal holes and quiet regions can be explained by the model variations in the upper chromosphere.

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Authors and Affiliations

Crimean Astrophysical Observatory, p/o Nauchny, 334413, Crimea, Ukraine
E. Malanushenko & E. Baranovsky

Authors

E. Malanushenko
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E. Baranovsky
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Editors and Affiliations

Institute for Geophysics, Astrophysics and Meteorology, University of Graz, Austria
Arnold Hanslmeier & Astrid Veronig &
Trieste Astronomical Observatory, Italy
Mauro Messerotti

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Malanushenko, E., Baranovsky, E. (2001). Physical Conditions in Solar Coronal Holes on the Base of Non-LTE Calculations. In: Hanslmeier, A., Messerotti, M., Veronig, A. (eds) The Dynamic Sun. Astrophysics and Space Science Library, vol 259. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0760-3_14

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DOI: https://doi.org/10.1007/978-94-010-0760-3_14
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-3826-3
Online ISBN: 978-94-010-0760-3
eBook Packages: Springer Book Archive

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