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Stellar rotation bifurcation caused by tidal locking in the open cluster NGC 2287?

Published online by Cambridge University Press:  11 March 2020

Weijia Sun Open the ORCID record for Weijia Sun [Opens in a new window] ,
Chengyuan Li ,
Licai Deng  and
Richard de Grijs
Weijia Sun
Affiliation:
Kavli Institute for Astronomy & Astrophysics and Department of Astronomy, Peking University, Yi He Yuan Lu 5, Hai Dian District, Beijing100871, China email: [email protected] Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing100012, China
Chengyuan Li
Affiliation:
Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing100012, China School of Physics and Astronomy, Sun Yat-sen University, Zhuhai519082, China
Licai Deng
Affiliation:
Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing100012, China School of Astronomy and Space Science, University of the Chinese Academy of Sciences, Huairou101408, China Department of Astronomy, China West Normal University, Nanchong637002, China
Richard de Grijs
Affiliation:
Department of Physics and Astronomy, Macquarie University, Balaclava Road, Sydney, NSW 2109, Australia Research Centre for Astronomy, Astrophysics and Astrophotonics, Macquarie University, Balaclava Road, Sydney, NSW 2109, Australia International Space Science Institute–Beijing, 1 Nanertiao, Hai Dian District, Beijing100190, China
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Abstract

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We present a detailed analysis of the projected stellar rotational velocities of the well-separated double main sequence (MS) in the young, ∼200 Myr-old Milky Way open cluster NGC 2287 and suggest that stellar rotation may drive the split MSs in NGC 2287. We find that the observed distribution of projected stellar rotation velocities could result from a dichotomous distribution of stellar rotation rates. We discuss whether our observations may reflect the effects of tidal locking affecting a fraction of the cluster’s member stars in stellar binary systems. The slow rotators are likely stars that initially rotated rapidly but subsequently slowed down through tidal locking induced by low-mass-ratio binary systems. However, the cluster may have a much larger population of short-period binaries than is usually seen in the literature, with relatively low secondary masses.

Keywords

stars: rotationopen clusters and associations: individual: NGC 2287galaxies: star clusters: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S351: Star Clusters: From the Milky Way to the Early Universe , May 2019 , pp. 228 - 232
Copyright
© International Astronomical Union 2020

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