Binary Star Fractions from the LAMOST DR4
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摘要
Stellar systems composed of single, double, triple or higher-order systems are rightfully regarded as the fundamental building blocks of the Milky Way. Binary stars play an important role in formation and evolution of the Galaxy. Through comparing the radial velocity variations from multiepoch observations, we analyze the binary fraction of dwarf stars observed with LAMOST. Effects of different model assumptions, such as orbital period distributions on the estimate of binary fractions,are investigated. The results based on log-normal distribution of orbital periods reproduce the previous complete analyses better than the power-law distribution. We find that the binary fraction increases with Teff and decreases with [Fe/H]. We first investigate the relation between α-elements and binary fraction in such a large sample as provided by LAMOST. The old stars with high [α/Fe] dominate with a higher binary fraction than young stars with low [α/Fe]. At the same mass, earlier forming stars possess a higher binary fraction than newly forming ones, which may be related with evolution of the Galaxy.
Stellar systems composed of single, double, triple or higher-order systems are rightfully regarded as the fundamental building blocks of the Milky Way. Binary stars play an important role in formation and evolution of the Galaxy. Through comparing the radial velocity variations from multiepoch observations, we analyze the binary fraction of dwarf stars observed with LAMOST. Effects of different model assumptions, such as orbital period distributions on the estimate of binary fractions,are investigated. The results based on log-normal distribution of orbital periods reproduce the previous complete analyses better than the power-law distribution. We find that the binary fraction increases with Teff and decreases with [Fe/H]. We first investigate the relation between α-elements and binary fraction in such a large sample as provided by LAMOST. The old stars with high [α/Fe] dominate with a higher binary fraction than young stars with low [α/Fe]. At the same mass, earlier forming stars possess a higher binary fraction than newly forming ones, which may be related with evolution of the Galaxy.
Stellar systems composed of single, double, triple or higher-order systems are rightfully regarded as the fundamental building blocks of the Milky Way. Binary stars play an important role in formation and evolution of the Galaxy. Through comparing the radial velocity variations from multiepoch observations, we analyze the binary fraction of dwarf stars observed with LAMOST. Effects of different model assumptions, such as orbital period distributions on the estimate of binary fractions,are investigated. The results based on log-normal distribution of orbital periods reproduce the previous complete analyses better than the power-law distribution. We find that the binary fraction increases with Teff and decreases with [Fe/H]. We first investigate the relation between α-elements and binary fraction in such a large sample as provided by LAMOST. The old stars with high [α/Fe] dominate with a higher binary fraction than young stars with low [α/Fe]. At the same mass, earlier forming stars possess a higher binary fraction than newly forming ones, which may be related with evolution of the Galaxy.
引文
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1Kepler Eclipsing Binary Catalog:http://keplerebs.villanova.edu
Badenes,C.,Mazzola,C.,Thompson,T.A.,et al.2017,ar Xiv:1711.00660
Basu,S.,Chaplin,W.J.,&Elsworth,Y.2010,Ap J,710,1596
Borucki,W.J.,Koch,D.,Basri,G.,et al.2010,Science,327,977
Cui,X.-Q.,Zhao,Y.-H.,Chu,Y.-Q.,et al.2012,RAA(Research in Astronomy and Astrophysics),12,1197
Demarque,P.,Woo,J.-H.,Kim,Y.-C.,&Yi,S.K.2004,Ap JS,155,667
Deng,L.-C.,Newberg,H.J.,Liu,C.,et al.2012,RAA(Research in Astronomy and Astrophysics),12,735
Duquennoy,A.,&Mayor,M.1991,A&A,248,485
ESA,ed.1997,ESA Special Publication,1200,The HIPPARCOS and TYCHO Catalogues.Astrometric and Photometric Star Catalogues Derived from the ESAHIPPARCOS Space Astrometry Mission
Gaia Collaboration,Prusti,T.,de Bruijne,J.H.J.,et al.2016,A&A,595,A1
Gao,S.,Liu,C.,Zhang,X.,et al.2014,Ap J,788,L37
Gao,S.,Zhao,H.,Yang,H.,&Gao,R.2017,MNRAS,469,L68
Gaulme,P.,Mc Keever,J.,Jackiewicz,J.,et al.2016,Ap J,832,121
Gorynya,N.A.,&Tokovinin,A.2014,MNRAS,441,2316
Hettinger,T.,Badenes,C.,Strader,J.,Bickerton,S.J.,&Beers,T.C.2015,Ap J,806,L2
Holberg,J.B.,Oswalt,T.D.,Sion,E.M.,&Mc Cook,G.P.2016,MNRAS,462,2295
Koch,D.G.,Borucki,W.J.,Basri,G.,et al.2010,Ap J,713,L79
Liu,X.-W.,Yuan,H.-B.,Huo,Z.-Y.,et al.2014,in IAUSymposium,298,Setting the Scene for Gaia and LAMOST,eds.S.Feltzing,G.Zhao,N.A.Walton,&P.Whitelock,310
Majewski,S.R.,Schiavon,R.P.,Frinchaboy,P.M.,et al.2017,AJ,154,94
Maoz,D.,Badenes,C.,&Bickerton,S.J.2012,Ap J,751,143
Matijeviˇc,G.,Prˇsa,A.,Orosz,J.A.,et al.2012,AJ,143,123
¨Opik,E.1924,Publications of the Tartu Astrofizica Observatory,25,1
Prˇsa,A.,Conroy,K.E.,Horvat,M.,et al.2016,Ap JS,227,29
Raghavan,D.,Mc Alister,H.A.,Henry,T.J.,et al.2010,Ap JS,190,1
Ruiz-Lara,T.,P′erez,I.,Gallart,C.,et al.2015,A&A,583,A60
Salpeter,E.E.1955,Ap J,121,161
Shan,Y.,Yee,J.C.,Bowler,B.P.,et al.2017,Ap J,846,93
Tokovinin,A.2014a,AJ,147,86
Tokovinin,A.2014b,AJ,147,87
Toonen,S.,Hollands,M.,G¨ansicke,B.T.,&Boekholt,T.2017,A&A,602,A16
Wu,Y.,Luo,A.-L.,Li,H.-N.,et al.2011,RAA(Research in Astronomy and Astrophysics),11,924
Xiang,M.S.,Liu,X.W.,Yuan,H.B.,et al.2015,MNRAS,448,822
Xiang,M.-S.,Liu,X.-W.,Shi,J.-R.,et al.2017,MNRAS,464,3657
York,D.G.,Adelman,J.,Anderson,Jr.,J.E.,et al.2000,AJ,120,1579
Yuan,H.-B.,Liu,X.-W.,Huo,Z.-Y.,et al.2015a,MNRAS,448,855
Yuan,H.,Liu,X.,Xiang,M.,et al.2015b,Ap J,799,135
Zhang,F.,Han,Z.,&Li,L.2007,in IAU Symposium,241,Stellar Populations as Building Blocks of Galaxies,ed.A.Vazdekis&R.Peletier,205
Zhao,G.,Zhao,Y.-H.,Chu,Y.-Q.,Jing,Y.-P.,&Deng,L.-C.2012,RAA(Research in Astronomy and Astrophysics),12,723
1Kepler Eclipsing Binary Catalog:http://keplerebs.villanova.edu
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