The R136 star cluster dissected with Hubble Space Telescope/STIS: III. The most massive stars and their clumped winds

Sarah A. Brands*, Alex De Koter, Joachim M. Bestenlehner, Paul A. Crowther, Jon O. Sundqvist, Joachim Puls, Saida M. Caballero-Nieves, Michael Abdul-Masih, Florian A. Driessen, Miriam García, Sam Geen, Götz Gräfener, Calum Hawcroft, Lex Kaper, Zsolt Keszthelyi, Norbert Langer, Hugues Sana, Fabian R.N. Schneider, Tomer Shenar, Jorick S. Vink

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

Abstract

Context. The star cluster R136 inside the Large Magellanic Cloud hosts a rich population of massive stars, including the most massive stars known. The strong stellar winds of these very luminous stars impact their evolution and the surrounding environment. We currently lack detailed knowledge of the wind structure that is needed to quantify this impact. Aims. Our goal is to observationally constrain the stellar and wind properties of the massive stars in R136, in particular the wind-structure parameters related to wind clumping. Methods. We simultaneously analyse optical and ultraviolet spectroscopy of 53 O-type and three WNh-stars using the Fastwind model atmosphere code and a genetic algorithm. The models account for optically thick clumps and effects related to porosity and velocity-porosity, as well as a non-void interclump medium. Results. We obtain stellar parameters, surface abundances, mass-loss rates, terminal velocities, and clumping characteristics and compare them to theoretical predictions and evolutionary models. The clumping properties include the density of the interclump medium and the velocity-porosity of the wind. For the first time, these characteristics are systematically measured for a wide range of effective temperatures and luminosities. Conclusions. We confirm a cluster age of 1.0 2.5 Myr and derived an initial stellar mass of ¥250 Ma for the most massive star in our sample, R136a1. The winds of our sample stars are highly clumped, with an average clumping factor of fcl = 29 ± 15. We find tentative trends in the wind-structure parameters as a function of the mass-loss rate, suggesting that the winds of stars with higher mass-loss rates are less clumped. We compare several theoretical predictions to the observed mass-loss rates and terminal velocities and find that none satisfactorily reproduce both quantities. The prescription of Krticka & Kubát (2018) matches the observed mass-loss rates best.

Original languageEnglish
Article numberA36
JournalAstronomy and Astrophysics
Volume663
DOIs
StatePublished - 1 Jul 2022
Externally publishedYes

Funding

FundersFunder number
Belgian Research Foundation Flanders
Deutsche Luft-und Raumfahrt50 OR 2009
Horizon 2020 Framework Programme945806
H2020 Marie Skłodowska-Curie Actions101024605
European Research Council
Deutsche ForschungsgemeinschaftEXC 2181/1-390900948
Fonds Wetenschappelijk OnderzoekG0H9218N
Nederlandse Organisatie voor Wetenschappelijk Onderzoek

    Keywords

    • Galaxies: star clusters: individual: R136
    • Magellanic Clouds
    • Outflows
    • Stars: fundamental parameters
    • Stars: mass-loss
    • Stars: massive
    • Stars: winds

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