000006558 001__ 6558
000006558 005__ 20240110144205.0
000006558 0247_ $$2DOI$$a10.1051/0004-6361/202345950
000006558 037__ $$aSCART-2024-0015
000006558 100__ $$aBodensteiner, J
000006558 245__ $$aThe young massive SMC cluster NGC 330 seen by MUSE. III. Stellar parameters and rotational velocities
000006558 260__ $$c2023
000006558 520__ $$aContext. The origin of the initial rotation rates of stars, and how a star's surface rotational velocity changes during the evolution, either by internal angular momentum transport or due to interactions with a binary companion, remain open questions in stellar astrophysics.  Aims: Here, we aim to derive the physical parameters and study the distribution of (projected) rotational velocities of B-type stars in the ∼35 Myr-old, massive cluster NGC 330 in the Small Magellanic Cloud. NGC 330 is in an age range where the number of post-interaction binaries is predicted to be high near the cluster turnoff (TO).  Methods: We developed a simultaneous photometric and spectroscopic grid-fitting method adjusting atmosphere models on multiband Hubble Space Telescope (HST) photometry and Multi Unit Spectroscopic Explorer (MUSE) spectroscopy. This allowed us to homogeneously constrain the physical parameters of over 250 B and Be stars (i.e., B-type stars with emission lines), brighter than mF814W = 18.8 mag.  Results: The rotational velocities of Be stars in NGC 330 are significantly higher than the ones of B-type stars. The rotational velocities vary as a function of the star's position in the color-magnitude diagram, qualitatively following predictions of binary population synthesis. A comparison to younger clusters shows that stars in NGC 330 rotate more rapidly on average.  Conclusions: The rotational velocities of the ∼35 Myr old population in NGC 330 quantitatively agree with predictions for a stellar population that underwent significant binary interactions: the majority of the B-type stars could be single stars or primaries in pre-interaction binaries. The rapidly spinning Be stars could be mass and angular momentum gainers in previous interactions, while those Be stars close to the TO may be spun-up single stars. The slowly rotating, apparently single stars above the TO could be merger products. The different v sin i characteristics of NGC 330 compared to younger populations can be understood in this framework.
000006558 594__ $$aNO
000006558 6531_ $$astars: early-type
000006558 6531_ $$astars: emission-line
000006558 6531_ $$aBe stars
000006558 6531_ $$astars: fundamental parameters: Hertzsprung-Russell and C-M diagrams
000006558 6531_ $$aMagellanic Clouds
000006558 6531_ $$aAstrophysics - Solar and Stellar Astrophysics
000006558 6531_ $$aAstrophysics - Astrophysics of Galaxies
000006558 700__ $$aSana, H
000006558 700__ $$aDufton, P L
000006558 700__ $$aWang, C
000006558 700__ $$aLanger, N
000006558 700__ $$aBanyard, G
000006558 700__ $$aMahy, L
000006558 700__ $$ade Koter, A
000006558 700__ $$ade Mink, S E
000006558 700__ $$aEvans, C J
000006558 700__ $$aGötberg, Y
000006558 700__ $$aHénault-Brunet, V
000006558 700__ $$aPatrick, L R
000006558 700__ $$aSchneider, F R N
000006558 773__ $$c18$$nA32$$pAstronomy & Astrophysics$$v680$$y2023
000006558 8560_ $$flaurent.mahy@ksb-orb.be
000006558 8564_ $$s2508771$$uhttp://publi2-as.oma.be/record/6558/files/Bodensteiner_2023.pdf
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000006558 8564_ $$s7083$$uhttp://publi2-as.oma.be/record/6558/files/Bodensteiner_2023.jpg?subformat=icon-180$$xicon-180
000006558 905__ $$apublished in
000006558 980__ $$aREFERD