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Synthetic line profiles in early-type stellar winds. I. H and He+

Published online by Cambridge University Press:  14 August 2015

P. B. Kunasz
P. B. Kunasz*
Affiliation:
High Altitude Observatory, National Center for Atmospheric Research* and Joint Institute for Laboratory Astrophysics, University of Colorado and National Bureau of Standards, Boulder, Colorado 80309 USA

Extract

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Statistical equilibrium calculations for the first ten levels of H and He+ were carried out for several model atmospheres of a star with Teff = 40,000 K and log g = 3.5, using the method of Mihalas and Kunasz (1978). Atomic level populations and line profiles were computed for “model C” calculated by Klein and Castor (1978) and for variants of this model in which material density and mass loss rates were scaled down by factors of 2.0, 2.2, 2.5 and 4.0. We will refer to these variant models as D, E, F, and G. The resulting line profiles are discussed. Two variants of the Klein-Castor model C are generally successful and produce He II λ4686 in emission with λ3204 in absorption. All normal Of stars observed with He II λ4686 in emission have λ3204 in absorption. In one of the models, Hα is in emission, while Hβ and the higher Balmer lines remain in absorption, as is commonly observed in Of spectra.

Type
Session 5: Theory and Mass Loss Rates Binary Stars - Miscellaneous Topics
Information
Symposium - International Astronomical Union , Volume 83: Mass Loss and Evolution of O-Type Stars , 1979 , pp. 243 - 247
Copyright
Copyright © Reidel 1979 

References

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