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New empirical mass-loss rates and clumping properties of massive stars

Published online by Cambridge University Press:  29 August 2024

Calum Hawcroft Open the ORCID record for Calum Hawcroft [Opens in a new window] ,
Hugues Sana Open the ORCID record for Hugues Sana [Opens in a new window] ,
Laurent Mahy Open the ORCID record for Laurent Mahy [Opens in a new window] ,
J. O. Sundqvist Open the ORCID record for J. O. Sundqvist [Opens in a new window] ,
M. Abdul-Masih Open the ORCID record for M. Abdul-Masih [Opens in a new window] ,
J. C. Bouret ,
S. A. Brands Open the ORCID record for S. A. Brands [Opens in a new window] ,
A. de Koter ,
F. A. Driessen Open the ORCID record for F. A. Driessen [Opens in a new window]  and
J. Puls
Calum Hawcroft*
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
Hugues Sana
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
Laurent Mahy
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium Royal Observatory of Belgium, Avenue Circulaire 3, B-1180 Brussels, Belgium
J. O. Sundqvist
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
M. Abdul-Masih
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
J. C. Bouret
Affiliation:
Aix Marseille Univ, CNRS, CNES, LAM, Marseille, France
S. A. Brands
Affiliation:
Astronomical Institute Anton Pannekoek, Amsterdam University, Science Park 904, 1098 XH Amsterdam, The Netherlands
A. de Koter
Affiliation:
Astronomical Institute Anton Pannekoek, Amsterdam University, Science Park 904, 1098 XH Amsterdam, The Netherlands
F. A. Driessen
Affiliation:
Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium
J. Puls
Affiliation:
LMU München, Universitätssternwarte, Scheinerstr. 1, 81679 München, Germany
*
email: calum.hawcroft@kuleuven.be
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Abstract

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Hot, massive stars are known to host unstable, radiation-driven outflowing winds, giving rise to dense clumps of material which severely affect the diagnostic techniques used to derive wind properties of massive stars. Most of the current diagnostic models account for wind inhomogeneities by assuming a one-component medium consisting of optically thin clumps, and maintaining a smooth velocity-field. However, this neglects important light-leakage effects through porous channels in-between the clumps. These light-leakage effects have recently been incorporated in the stellar atmosphere modelling code FASTWIND, and here we will present quantitative mass-loss results from a combined Ultraviolet-Optical wind analysis of O-supergiants in the Galaxy. Using a genetic-algorithm fitting-approach, we systematically investigate the impact the wind physics has on derived stellar and wind parameters, and how this depends on metallicity and spectral type. We compare our findings with earlier results (which do not take into account such light-leakage effects), to standard mass-loss rates usually included in evolution model studies of massive stars, and with theoretical predictions of clumping properties. We will also present the first systematic empirical constraints on the new wind parameters, associated with light-leakage, and compare these with theoretical predictions.

Keywords

stars: mass lossstars: early-typestars: atmospheres
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S361: Massive Stars Near and Far , May 2022 , pp. 168 - 173
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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