Abstract
In this paper we describe the status of a continuing effort to calculate NLTE models of rapidly expanding hot star atmospheres including the hydrodynamics selfconsistently. In order to test our theoretical concept, we calculated a wind model for the O4I(n)f star ζ-Pup. An additional test was performed by calculating stationary wind models along evolutionary tracks. The fact that such models satisfactorily reproduce the observed luminosity dependence of the Si IV resonance line indicates that the theory can soon be used for quantitative analysis of stellar wind lines. We show further that the calculated dynamical parameters can already be used for a direct spectroscopic determination of stellar masses and radii. This is done not only for massive stars in our galaxy, but also for an O-star in the SMC.
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Pauldrach, A.W.A., Puls, J. (1990). Radiation Driven Winds of Hot Luminous Stars. Applications of Stationary Wind Models. In: Klare, G. (eds) Accretion and Winds. Reviews in Modern Astronomy, vol 3. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-76238-3_10
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DOI: https://doi.org/10.1007/978-3-642-76238-3_10
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