Orbital and physical parameters of the close binary system GJ 9830(HIP 116259)
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摘要
We present the complete set of physical and geometrical parameters of the visual close binary system GJ 9830 for the first time by applying Al-Wardat's complex method. This method combines magnitude difference from speckle interferometry, synthetic spectral energy distributions of the binary components which are constructed based on grids of Kurucz blanketed models(ATLAS9), and the orbital solution using Tokovinin's dynamical method to estimate the parameters of individual components. The analysis of the system by employing synthetic photometry resulted in the following set of parameters:Teff= 6220 ± 100 K, log g = 4.30 ± 0.12, R = 1.10 ± 0.08 R_⊙for the primary component and Teff= 4870 ± 100 K, log g = 4.60 ± 0.11, R = 0.709 ± 0.07 R_⊙for the secondary component. The recently published dynamical parallax from the Gaia space mission was used to calculate the total mass of the binary system as 1.75 ± 0.06 M_⊙, which coincides with those estimated using Al-Wardat's method as MA= 1.18 ± 0.10 M_⊙, MB= 0.75 ± 0.08 M_⊙. The analysis of the system reveals that both components are characteristic of main sequence stars and have an age of around 1.4 ± 0.50 Gyr. The evolutionary tracks and isochrones of the system's components are discussed, and the fragmentation process is suggested as the most likely process for the formation of the system.
We present the complete set of physical and geometrical parameters of the visual close binary system GJ 9830 for the first time by applying Al-Wardat's complex method. This method combines magnitude difference from speckle interferometry, synthetic spectral energy distributions of the binary components which are constructed based on grids of Kurucz blanketed models(ATLAS9), and the orbital solution using Tokovinin's dynamical method to estimate the parameters of individual components. The analysis of the system by employing synthetic photometry resulted in the following set of parameters:Teff= 6220 ± 100 K, log g = 4.30 ± 0.12, R = 1.10 ± 0.08 R_⊙for the primary component and Teff= 4870 ± 100 K, log g = 4.60 ± 0.11, R = 0.709 ± 0.07 R_⊙for the secondary component. The recently published dynamical parallax from the Gaia space mission was used to calculate the total mass of the binary system as 1.75 ± 0.06 M_⊙, which coincides with those estimated using Al-Wardat's method as MA= 1.18 ± 0.10 M_⊙, MB= 0.75 ± 0.08 M_⊙. The analysis of the system reveals that both components are characteristic of main sequence stars and have an age of around 1.4 ± 0.50 Gyr. The evolutionary tracks and isochrones of the system's components are discussed, and the fragmentation process is suggested as the most likely process for the formation of the system.
We present the complete set of physical and geometrical parameters of the visual close binary system GJ 9830 for the first time by applying Al-Wardat's complex method. This method combines magnitude difference from speckle interferometry, synthetic spectral energy distributions of the binary components which are constructed based on grids of Kurucz blanketed models(ATLAS9), and the orbital solution using Tokovinin's dynamical method to estimate the parameters of individual components. The analysis of the system by employing synthetic photometry resulted in the following set of parameters:Teff= 6220 ± 100 K, log g = 4.30 ± 0.12, R = 1.10 ± 0.08 R_⊙for the primary component and Teff= 4870 ± 100 K, log g = 4.60 ± 0.11, R = 0.709 ± 0.07 R_⊙for the secondary component. The recently published dynamical parallax from the Gaia space mission was used to calculate the total mass of the binary system as 1.75 ± 0.06 M_⊙, which coincides with those estimated using Al-Wardat's method as MA= 1.18 ± 0.10 M_⊙, MB= 0.75 ± 0.08 M_⊙. The analysis of the system reveals that both components are characteristic of main sequence stars and have an age of around 1.4 ± 0.50 Gyr. The evolutionary tracks and isochrones of the system's components are discussed, and the fragmentation process is suggested as the most likely process for the formation of the system.
引文
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Masda,S.G.,Al-Wardat,M.A.,Neuha¨user,R.,&Al-Naimiy,H.M.2016,RAA(Research in Astronomy and Astrophysics),16,112
Masda,S.G.,Al-Wardat,M.A.,&Pathan,J.M.2018,Journal of Astrophysics and Astronomy,39,58
Mason,B.D.,Hartkopf,W.I.,Raghavan,D.,et al.2011,AJ,142,176
Metchev,S.A.,&Hillenbrand,L.A.2009,ApJ S,181,62Monet,D.G.1977,ApJ,214,L133
Monet,D.G.1979,ApJ,234,275
Olevi?,D.,&Cvetkovi?,Z.2004,A&A,415,259
Pluzhnik,E.A.2005,A&A,431,587
Roberts,Jr.,L.C.,Turner,N.H.,ten Brummelaar,T.A.,Mason,B.D.,&Hartkopf,W.I.2011,AJ,142,175
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Smart,W.M.1930,MNRAS,90,534
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Tokovinin,A.2018,VizieR Online Data Catalog,515
Tokovinin,A.,Mason,B.D.,&Hartkopf,W.I.2010,AJ,139,743
van Leeuwen,F.2007,A&A,474,653
Zinnecker,H.,&Mathieu,R.,eds.2001,IAU Symposium,200,The Formation of Binary Stars
Al-Wardat,M.2012,PASA,29,523
Al-Wardat,M.A.,Balega,Y.Y.,Leushin,V.V.,et al.2014a,Astrophysical Bulletin,69,58
Al-Wardat,M.A.,Balega,Y.Y.,Leushin,V.V.,et al.2014b,Astrophysical Bulletin,69,198
Al-Wardat,M.A.,Docobo,J.A.,Abushattal,A.A.,&Campo,P.P.2017,Astrophysical Bulletin,72,24
Al-Wardat,M.A.,El-Mahameed,M.H.,Yusuf,N.A.,Khasawneh,A.M.,&Masda,S.G.2016,RAA(Research in Astronomy and Astrophysics),16,166
Al-Wardat,M.A.,Widyan,H.S.,&Al-thyabat,A.2014c,PASA,31,e005
Balega,I.I.,Balega,A.F.,Maksimov,E.V.,et al.2006,Bulletin of the Special Astrophysics Observatory,59,20
Balega,I.I.,Balega,Y.Y.,Gasanova,L.T.,et al.2013,Astrophysical Bulletin,68,53
Balega,I.I.,Balega,Y.Y.,Hofmann,K.-H.,et al.2002,A&A,385,87
Balega,I.I.,Balega,Y.Y.,Maksimov,A.F.,et al.2007,Astrophysical Bulletin,62,339
Bessell,M.,&Murphy,S.2012,PASP,124,140
Bonnell,I.A.1994,MNRAS,269,837
Castelli,F.1999,A&A,346,564
Docobo,J.A.1985,Celestial Mechanics,36,143
Docobo,J.A.2012,in Orbital Couples:Pas de Deux in the Solar System and the Milky Way,eds.F.Arenou&D.Hestroffer,119
Docobo,J.A.,Tamazian,V.S.,&Campo,P.P.2018,MNRAS,476,2792
ESA,1997a,ESA Special Publication,1239,The HIPPARCOSand TYCHO Catalogues.Astrometric and Photometric Star Catalogues Derived from the ESA HIPPARCOS Space Astrometry Mission
ESA,1997b,ESA Special Publication,1200,The HIPPARCOSand TYCHO Catalogues.Astrometric and Photometric Star Catalogues Derived from the ESA HIPPARCOS Space Astrometry Mission
Gaia Collaboration.2018,VizieR Online Data Catalog,1345
Girardi,L.,Bressan,A.,Bertelli,G.,&Chiosi,C.2000a,A&AS141,371
Girardi,L.,Bressan,A.,Bertelli,G.,&Chiosi,C.2000b,VizieROnline Data Catalog,414,10371
Gray,D.F.2005,The Observation and Analysis of Stellar Photospheres(Cambridge,UK:Cambridge Univ.Press)
Gumaan Masda,S.,Al-Wardat,M.A.,&Pathan,J.K.M.K2018,RAA(Research in Astronomy and Astrophysics),18072
Hauck,B.,&Mermilliod,M.1998,A&AS,129,431
Heintz,W.D.1978,Geophysics and Astrophysics Monographs,15
H?g,E.,Fabricius,C.,Makarov,V.V.,et al.2000,A&A,355,L27
Horch,E.P.,Falta,D.,Anderson,L.M.,et al.2010,AJ,139,205
Horch,E.P.,Meyer,R.D.,&van Altena,W.F.2004,AJ,127,1727
Horch,E.P.,Robinson,S.E.,Meyer,R.D.,et al.2002,AJ,123,3442
Horch,E.P.,van Altena,W.F.,Cyr,Jr.,W.M.,et al.2008,AJ,136,312
Horch,E.P.,Casetti-Dinescu,D.I.,Camarata,M.A.,et al.2017,AJ,153,212
Kurucz,R.1994,Solar Abundance Model Atmospheres for0,1,2,4,8 km/s.Kurucz(Cambridge,Mass.:Smithsonian Astrophysical Observatory),19
Lang,K.R.1992,Astrophysical Data I.Planets and Stars.(Springer-Verlag Berlin Heidelberg New York),33
Linnell,A.P.,DeS tefano,P.,&Hubeny,I.2013,AJ,146,68
Ma′?z Apellańiz,J.2007,in Astronomical Society of the Pacific Conference Series,364,The Future of Photometric,Spectrophotometric and Polarimetric Standardization,ed.C.Sterken,227
Masda,S.G.,Al-Wardat,M.A.,Neuha¨user,R.,&Al-Naimiy,H.M.2016,RAA(Research in Astronomy and Astrophysics),16,112
Masda,S.G.,Al-Wardat,M.A.,&Pathan,J.M.2018,Journal of Astrophysics and Astronomy,39,58
Mason,B.D.,Hartkopf,W.I.,Raghavan,D.,et al.2011,AJ,142,176
Metchev,S.A.,&Hillenbrand,L.A.2009,ApJ S,181,62Monet,D.G.1977,ApJ,214,L133
Monet,D.G.1979,ApJ,234,275
Olevi?,D.,&Cvetkovi?,Z.2004,A&A,415,259
Pluzhnik,E.A.2005,A&A,431,587
Roberts,Jr.,L.C.,Turner,N.H.,ten Brummelaar,T.A.,Mason,B.D.,&Hartkopf,W.I.2011,AJ,142,175
Roberts,Jr.,L.C.,Turner,N.H.,Bradford,L.W.,et al.2005,AJ,130,2262
Schlafly,E.F.,&Finkbeiner,D.P.2011,ApJ,737,103
Smart,W.M.1930,MNRAS,90,534
Straizys,V.1996,Baltic Astronomy,5,459
Tokovinin,A.1992,in Astronomical Society of the Pacific Conference Series,32,IAU Colloq.135:Complementary Approaches to Double and Multiple Star Research,eds.H.A.McA lister,&W.I.Hartkopf,573
Tokovinin,A.2017,AJ,154,110
Tokovinin,A.2018,VizieR Online Data Catalog,515
Tokovinin,A.,Mason,B.D.,&Hartkopf,W.I.2010,AJ,139,743
van Leeuwen,F.2007,A&A,474,653
Zinnecker,H.,&Mathieu,R.,eds.2001,IAU Symposium,200,The Formation of Binary Stars