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Radiation Driven Atmospheres of O-type stars: Constraints on the Mass–Luminosity Relation of Central Stars of Planetary Nebulae

Published online by Cambridge University Press:  26 May 2016

A.W.A. Pauldrach ,
T.L. Hoffmann  and
R.H. Méndez
A.W.A. Pauldrach
Affiliation:
Institut für Astronomie und Astrophysik der Universität München, Scheinerstraße 1, 81679 München, Germany
T.L. Hoffmann
Affiliation:
Institut für Astronomie und Astrophysik der Universität München, Scheinerstraße 1, 81679 München, Germany
R.H. Méndez
Affiliation:
Institut für Astronomie und Astrophysik der Universität München, Scheinerstraße 1, 81679 München, Germany

Abstract

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Recent advances in the modelling of stellar winds driven by radiation pressure make it possible to fit many wind-sensitive features in the UV spectra of hot stars, opening the way for a hydrodynamically consistent determination of stellar radii, masses, and luminosities from the UV spectrum alone. It is thus no longer necessary to assume a theoretical mass–luminosity relation. As the method has been shown to work for massive O stars, we are now able to test predictions from the post-AGB evolutionary calculations quantitatively for the first time. Here we present the first rather surprising consequences of using the new generation of model atmospheres for the analysis of a sample of central stars of planetary nebulae.

Type
Part IV: Central Stars and their Atmospheres
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 177 - 186
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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