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Advances in radiatively driven wind models

Published online by Cambridge University Press:  26 May 2016

Joachim Puls ,
Tamara Repolust ,
Tadziu L. Hoffmann ,
Alexander Jokuthy  and
Roberto O.J. Venero
Joachim Puls
Affiliation:
Universitätssternwarte, Ludwich-Maximilians-Universität, Scheinerstraße 1, D-81679 München, BRD
Tamara Repolust
Affiliation:
Universitätssternwarte, Ludwich-Maximilians-Universität, Scheinerstraße 1, D-81679 München, BRD
Tadziu L. Hoffmann
Affiliation:
Universitätssternwarte, Ludwich-Maximilians-Universität, Scheinerstraße 1, D-81679 München, BRD
Alexander Jokuthy
Affiliation:
Universitätssternwarte, Ludwich-Maximilians-Universität, Scheinerstraße 1, D-81679 München, BRD
Roberto O.J. Venero
Affiliation:
Observatorio Astronómico, Paseo del Bosque, La Plata, Argentina

Abstract

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We report on a re-analysis of the Galactic O-type star sample presented by Puls et al. (1996) by means of non-LTE model atmospheres including line-blocking and line-blanketing. In particular, we concentrate on the question concerning the dependence of the wind-momentum luminosity relation (WLR) on luminosity class. Owing to the line-blanketing, the derived effective temperatures become significantly lower when compared to previous results, whereas the so-called ‘modified wind-momentum rates’ remain roughly at their former values. Therefore, we obtain a new WLR for O-type stars. By comparing these ‘observational’ results with new theoretical predictions and simulations, we conclude that the Hα forming region for objects with Hα in emission might be considerably clumped and thus a larger mass-loss rate than actually present is mimicked. We suggest that the previously found dependence of the WLR on luminosity class is an artefact.

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. 61 - 69
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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