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Investigating the impact of different velocity fields on the spectral appearance of Wolf-Rayet stars

Published online by Cambridge University Press:  29 August 2024

R. R. Lefever Open the ORCID record for R. R. Lefever [Opens in a new window] ,
T. Shenar ,
A. A. C. Sander ,
L. Poniatowski ,
K. Dsilva  and
H. Todt
R. R. Lefever*
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12-14, 69120 Heidelberg, Germany Institute for Astronomy (IvS), KU Leuven, Celestijnenlaan 200D, 3000 Leuven, Belgium
T. Shenar
Affiliation:
Institute for Astronomy (IvS), KU Leuven, Celestijnenlaan 200D, 3000 Leuven, Belgium Anton Pannekoek Institute for Astronomy, Science Park 904, 1098 XH, Amsterdam, The Netherlands
A. A. C. Sander
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
L. Poniatowski
Affiliation:
Institute for Astronomy (IvS), KU Leuven, Celestijnenlaan 200D, 3000 Leuven, Belgium
K. Dsilva
Affiliation:
Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
H. Todt
Affiliation:
Institut für Physik und Astronomie, Universität Potsdam, Karl-Liebknecht-Str. 24/25, D-14476 Potsdam, Germany
*
email: roel.lefever@uni-heidelberg.de
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Abstract

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The emission line spectra of WR stars are often formed completely in the optically thick stellar wind. Hence, any assumption on the wind velocity law in a spectral analysis has a profound impact on the determination of the stellar parameters. By comparing Potsdam Wolf-Rayet (PoWR) model spectra calculated with different β laws, we show that the velocity field heavily influences the spectra: by using the appropriate β laws, the entire range of late and early types can be covered with the same stellar model.

Keywords

SpectropolarimetryX-raysWR starsbinary systems
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 505 - 506
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Creative Commons
Creative Common License - CCCreative Common License - BY
This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution, and reproduction in any medium, provided the original work is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Ekström, Sylvia and Georgy, Cyril and Eggenberger, Patrick and Meynet, Georges and Mowlavi, Nami and Wyttenbach, Aurélien and Granada, Anah and Decressin, Thibaut and Hirschi, Raphael and Frischknecht, Urs 2006, A&A, 537, A146 CrossRefGoogle Scholar
Gräfener, G. and Koesterke, L. and Hamann, W-R 2002, A&A, 387, 244–257 Google Scholar
Grassitelli, L. and Langer, N. and Grin, N. J. and Mackey, J. and Bestenlehner, J. M. and Gräfener, G. 2018, A&A, 614, A86 Google Scholar
Hamann, W-R and Gräfener, G. 2003, A&A, 410, 993–1000 Google Scholar
Hamann, W-R and Gräfener, G. and Liermann, Adriane 2006, A&A, 457, 1015–1031 CrossRefGoogle Scholar
Lépine, Sébastien and Moffat, Anthony F.J. 1999, ApJ, 514, 909 Google Scholar
Petrovic, J. and Pols, O. and Langer, N. 2006, A&A, 450, 219–225 CrossRefGoogle Scholar
Prinja, Raman K. and Barlow, M. J. and Howarth, Ian D. 1990, ApJ, 361, 607 Google Scholar
Sander, Andreas and Shenar, Tomer and Hainich, Rainer and Gmenez-Garca, Angel and Todt, Helge and Hamann, W-R 2015, A&A, 577, A13 Google Scholar
Smith, Lindsey F. and Shara, Michael M. and Moffat, Anthony F.J. 1996, MNRAS, 281, 163–191 Google Scholar