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Non-LTE line blanketed atmospheres for hot stars

Published online by Cambridge University Press:  25 May 2016

D. J. Hillier
D. J. Hillier*
Affiliation:
University of Pittsburgh, USA

Abstract

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The modeling of hot star atmospheres falls into two broad classes: those where the plane parallel approximation can be used, and those where the effects of spherical extension and stellar winds are important. In both cases non-LTE modeling is a necessity for reliable spectroscopic analyses.

While simple ions (e.g., H, He I, and He II) have been treated routinely in non-LTE for many years it is only recently that advances in computing power, computational techniques, and the availability of atomic data have made it feasible to perform non-LTE line blanketing calculations. Present models, with varying degrees of approximation and sophistication, are now capable of treating the effects of tens of thousands of lines. We review the latest efforts in incorporating non-LTE line blanketing, highlighting recent advances in the modeling of 0 stars, hot sub-dwarfs, Wolf-Rayet stars, novae, and supernovae.

Type
Stellar Atmospheres
Information
Symposium - International Astronomical Union , Volume 189: Fundamental Stellar Properties: The Interaction Between Observation and Theory , 1997 , pp. 209 - 216
Copyright
Copyright © Kluwer 1997 

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