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Hydrodynamic model atmospheres for hot stars

Published online by Cambridge University Press:  26 May 2016

Götz Gräfener  and
Wolf-Rainer Hamann
Götz Gräfener
Affiliation:
Lehrstuhl Astrophysik, Institut für Physik, Universität Potsdam, Am Neuen Palais 10, D-14469 Potsdam, BRD
Wolf-Rainer Hamann
Affiliation:
Lehrstuhl Astrophysik, Institut für Physik, Universität Potsdam, Am Neuen Palais 10, D-14469 Potsdam, BRD

Abstract

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Recent non-LTE models for expanding atmospheres, accounting for iron group line-blanketing and clumping, show a radiative acceleration which supplies a large part of the driving force of WR and O star winds. Aiming at the calculation of fully consistent wind models, we developed a method to include the solution of the hydrodynamic equations into our atmosphere code, taking into account the radiation pressure from the CMF radiation transport. In the present work we discuss the resulting wind acceleration for ‘standard’ WR and O-type star model atmospheres, and present a hydrodynamically consistent non-LTE model for the O4I(n)f star ζ Pup. In addition we demonstrate the effect of clumping on the radiative acceleration.

Type
Part 1. Atmospheres of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 190 - 191
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Gräfener, G., Koesterke, L., Hamann, W.-R. 2002, A&A 387, 244.Google Scholar
Koesterke, L., Hamann, W.-R., Gräfener, G. 2002, A&A 384, 562.Google Scholar