643 citations
- Ludwig-Maximilians-Universität MünchenDE115 papers
- Centre National de la Recherche ScientifiqueFR7 papers
- Instituto de Astrofísica de CanariasES7 papers
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- Universidad de La LagunaES6 papers
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- University of BonnDE5 papers
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17 papers · 1 filter
X-Shooting ULLYSES: Massive stars at low metallicity. IV. Spectral analysis methods and exemplary results for O stars
A. A. C. Sander, J. -C. Bouret, M. Bernini-Peron +26
CONTEXT: The spectral analysis of hot, massive stars is a fundamental astrophysical method to obtain their intrinsic properties and their feedback. Quantitative spectroscopy for ho…
To clump or not to clump The impact of wind inhomogeneities on the optical and NIR spectroscopic analysis of massive OB stars
K. Rübke, A. Herrero, J. Puls
Winds of massive stars have density inhomogeneities (clumping) that may affect the formation of spectral lines in different ways, depending on their formation region. Most of previ…
A model of anisotropic winds from rotating stars for evolutionary calculations
Ben Hastings, Norbert Langer, Joachim Puls
Context: The surface properties of rotating stars can vary from pole to equator, resulting in anisotropic stellar winds which are not included in the currently available evolutiona…
Quantitative spectroscopy of late O-type main-sequence stars with a hybrid non-LTE method
Patrick Aschenbrenner, Norbert Przybilla, Keith Butler
Context. Late O-type stars at luminosities show weak winds with mass-loss rates lower than 10 yr. This implies that their photos…
The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities
Z. Keszthelyi, A. de Koter, Y. Götberg +12
Magnetic fields can drastically change predictions of evolutionary models of massive stars via mass-loss quenching, magnetic braking, and efficient angular momentum transport, whic…
Probing Red Supergiant dynamics through photo-center displacements measured by Gaia
A. Chiavassa, R. Kudritzki, B. Davies +2
Red supergiant (RSGs) are cool massive stars in a late phase of their evolution when the stellar envelope becomes fully convective. They are the brightest stars in the universe at…