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Resonance broadening and van der waals broadening

Published online by Cambridge University Press:  16 November 2010

R. Monier ,
B. Smalley ,
G. Wahlgren ,
Ph. Stee  and
L. Mashonkina
L. Mashonkina*
Affiliation:
Institute of Astronomy, Russian Academy of Science, Pyatnitskaya 48, 119017 Moscow, Russia. e-mail: [email protected]
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Abstract

Resonance broadening is important for the hydrogen lines in the spectra of F-type and later stars. In the corresponding temperature regime, the extended wings of the Balmer lines are used as a stellar effective temperature indicator. We show the effect of the use of two broadening theories, Ali & Griem (1965, 1966) and Barklem et al. (2000a, 2000b), on the effective temperature derived in non-LTE from Hα and Hβ in the Sun and the metal-poor star HD19445. Van der Waals broadening is important for strong spectral lines in the atmospheres of F-type and later stars. For the selected transitions in Ca I and Ca II, line profile comparisons are made between applying the van der Waals damping constants from laboratory measurements, the ABO perturbation theory, and the classic Unsöld approximation.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 43: Non-LTE Line Formation for Trace Elements in Stellar Atmospheres , 2010 , pp. 135 - 141
Copyright
© EAS, EDP Sciences 2010

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