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Computation of Infrared Hydrogen Lines

Published online by Cambridge University Press:  03 August 2017

Mats Carlsson  and
Robert J. Rutten
Mats Carlsson
Affiliation:
Institute of Theoretical Astrophysics, P.O. Box 1029, Blindern, N–0315 Oslo 3, Norway
Robert J. Rutten
Affiliation:
Sterrekundig Instituut, Postbus 80 000, NL–3508 TA, Utrecht, The Netherlands

Abstract

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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.

Keywords

atomic processeshydrogeninfrared: starsline: formationline: profilesSun: atmosphere
Type
Part 4: Infrared Atomic Physics and Line Formation
Information
Symposium - International Astronomical Union , Volume 154: Infrared Solar Physics , 1994 , pp. 341 - 346
Copyright
Copyright © Kluwer 1994 

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