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Extended Main-sequence Turnoffs in the Double Cluster h and χ Persei: The Complex Role of Stellar Rotation
Li,Chengyuan1,2,3; Sun,Weijia4,5; Grijs,Richard de1,2,6; Deng,Licai3,7; Wang,Kun7,8; Cordoni,Giacomo9; Milone,Antonino P.9
2019-05-06
Source PublicationThe Astrophysical Journal
ISSN0004-637X
Volume876Issue:1
AbstractAbstract Using Gaia Data Release 2 photometry, we report the detection of extended main-sequence turnoff (eMSTO) regions in the color–magnitude diagrams (CMDs) of the ~14 Myr old double clusters h and χ Persei (NGC 869 and NGC 884). We find that stars with masses below ~1.3 M⊙ in both h and χ Persei populate narrow main sequences (MSs), while more massive stars define the eMSTO, closely mimicking observations of young Galactic and Magellanic Cloud clusters (with ages older than ~30 Myr). Previous studies based on clusters older than ~30 Myr found that rapidly rotating MS stars are redder than slow rotators of similar luminosity, suggesting that stellar rotation may be the main driver of the eMSTO. By combining photometry and projected rotational velocities from the literature of stars in h and χ Persei, we find no obvious relation between the rotational velocities and colors of non-emission-line eMSTO stars, in contrast with what is observed in older clusters. Similar to what is observed in Magellanic Cloud clusters, most of the extremely rapidly rotating stars, identified by their strong Hα emission lines, are located in the red part of the eMSTOs. This indicates that stellar rotation plays a role in the color and magnitude distribution of MSTO stars. By comparing the observations with simulated CMDs, we find that a simple population composed of coeval stars that span a wide range of rotation rates is unable to reproduce the color spread of the cluster’s MSs. We suggest that variable stars, binary interactions, and stellar rotation affect the eMSTO morphology of these very young clusters.
KeywordHertzsprung–Russell and C–M diagrams open clusters and associations: individual (NGC 869 and NGC 884)
DOI10.3847/1538-4357/ab15d2
Language英语
WOS IDIOP:0004-637X-876-1-ab15d2
PublisherThe American Astronomical Society
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/28873
Collection中国科学院国家天文台
Affiliation1.Department of Physics and Astronomy, Macquarie University, Sydney, NSW 2109, Australia; chengyuan.li@mq.edu.au
2.Centre for Astronomy, Astrophysics and Astrophotonics, Macquarie University, Sydney, NSW 2109, Australia
3.Key Laboratory for Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Beijing 100012, People’s Republic of China
4.Department of Astronomy, Peking University, Yi He Yuan Lu 5, Hai Dian District, Beijing 100871, People’s Republic of China
5.Kavli Institute for Astronomy and Astrophysics, Peking University, Yi He Yuan Lu 5, Hai Dian District, Beijing 100871, People’s Republic of China
6.International Space Science Institute–Beijing, 1 Nanertiao, Zhongguancun, Hai Dian District, Beijing 100190, People’s Republic of China
7.Department of Astronomy, China West Normal University, Nanchong 637002, People’s Republic of China
8.Instituto de Astrof?isica de Canarias, E-38200 La Laguna, Tenerife, Spain
9.Dipartimento di Fisica e Astronomia “Galileo Galilei,” Università di Padova, Vicolo dell’Osservatorio 3, I-35122 Padova, Italy
First Author AffilicationNational Astronomical Observatories, Chinese Academy of Sciences
Recommended Citation
GB/T 7714
Li,Chengyuan,Sun,Weijia,Grijs,Richard de,et al. Extended Main-sequence Turnoffs in the Double Cluster h and χ Persei: The Complex Role of Stellar Rotation[J]. The Astrophysical Journal,2019,876(1).
APA Li,Chengyuan.,Sun,Weijia.,Grijs,Richard de.,Deng,Licai.,Wang,Kun.,...&Milone,Antonino P..(2019).Extended Main-sequence Turnoffs in the Double Cluster h and χ Persei: The Complex Role of Stellar Rotation.The Astrophysical Journal,876(1).
MLA Li,Chengyuan,et al."Extended Main-sequence Turnoffs in the Double Cluster h and χ Persei: The Complex Role of Stellar Rotation".The Astrophysical Journal 876.1(2019).
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