Hostname: page-component-7c8c6479df-5xszh Total loading time: 0 Render date: 2024-03-28T12:00:59.581Z Has data issue: false hasContentIssue false

Why should we compare Wolf-Rayet codes?

Published online by Cambridge University Press:  25 May 2016

Orsola De Marco
Affiliation:
Institute of Astronomy, Federal Institute of Technology, Zürich, Switzerland
Werner Schmutz
Affiliation:
Institute of Astronomy, Federal Institute of Technology, Zürich, Switzerland
Lars Koesterke
Affiliation:
Department of Physics, University of Potsdam, Germany
Wolf-Rainer Hamann
Affiliation:
Department of Physics, University of Potsdam, Germany
Alex de Koter
Affiliation:
Astronomical Institute Anton Pannekoek, University of Amsterdam, the Netherlands

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We have modeled the spectrum of WR135 with a co-moving frame code and then used identical input parameters with a Sobolev-approximation code. Helium lines compare well in strength and shape, while carbon lines are found to be much stronger in the co-moving frame code. The reason for this discrepancy is being investigated. The present comparison shows that tests have to be extended to more complex atomic models and compatibility between different codes should not be taken yet for granted.

Type
Part 2. Models for single star evolution of massive stars: wind + atmosphere + interior
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

de Koter, A., Schmutz, W., Lamers, H. 1993, A&A 277, 561 Google Scholar
de Koter, A., Heap, S.R., Hubeny, I. 1997, ApJ 477, 792 Google Scholar
Hamann, W.-R., Schmutz, W., Wessolowski, U. 1988, A&A 194, 190 Google Scholar