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Science China(Physics,Mechanics & Astronomy) 2012年第4期55卷 706-716页

作者： SONG Fen HUANG RunQian Department of Astronomy Beijing Normal UniversityBeijing 100875China National Astronomical Observatories/Yunnan Observatory Chinese Academy of SciencesKunming 650011China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650011China

The W UMa-type contact binaries have been observed for several *** construct the evolutionary model for W UMa-type contact binaries,many difficulties were encountered due to the existence of complicated physical processes in such *** model introduced by Huang,Song and Bi includes some special and unique understandings of the physical processes of contact *** is necessary to test whether this model can be used for W UMa-type contact *** best way to test a theoretical model is to know whether this model can explain the observational phenomena of such *** this aim,a comparison is performed for the relations of mass-luminosity,mass-radius,and the distribution in the HR diagram obtained from the model introduced by Huang et *** those from the astronomical *** result of the comparison indicates that this model can be applied to W UMa-type contact binaries and can explain the observational phenomena of such binaries.

关键词： binaries: close stars: evolution stars: fundamental parameters stars: rotation

A test of an early-type contact binary model by comparing the relations obtained from theory with those from observations

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Science China(Physics,Mechanics & Astronomy) 2012年第2期55卷 320-328页

Contact binary systems,including massive,middle-mass and low-mass systems,have been *** is necessary to construct the evolutionary model for contact binary systems with all different *** model introduced by Huang,Song and Bi indicates some special and unique understandings of the physical processes occurring in the contact *** is necessary to test whether this model can be applied to the early-type contact *** best way to test a theoretical model is to know whether this model can explain the observational phenomena of such *** this aim,a comparison is performed for the relations of mass-luminosity,mass-radius,and the distribution in the HR diagram obtained from the model introduced by Huang et *** those from the astronomical observations.A good result is obtained by the *** means the model can be used in calculating the evolution of early-type contact binaries,and can explain the observational phenomena of such binaries.

关键词： binaries: eclipsing stars: evolution stars: fundamental parameters stars: rotation

The Near-Contact Binary FU Ara:New Observations,a Photometric Study and Preliminary Elements

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Chinese Journal of Astronomy and Astrophysics 2008年第6期8卷 707-713页

作者： A. Paschke F. Acerbi C. Barani Weierstr 30 8630 Rueti Switzerland Via Zoncada 51 26845 Codogno （LO） Italy Via Molinetto 35 26845 Triulza di Codogno （LO） Italy

A new CCD （V） light curve is presented for the semi-detached binary system FU Ara. The light curve, obtained in 2007, is the first one since the last 50 years. With our data we were able to determine six new times of minimum light and refined the period of the system to 0.8645049 days. A Wilson-Devinney analysis leads to a solution of a semi- detached configuration, composed of a main-sequence primary component of spectral type F5, fractionally smaller than its Roche lobe, and an evolved secondary component of spectral type K1 which fills its Roche lobe, and which is overluminous and oversized as compared with the main-sequence. The two components of FU Ara differ considerably in effective temperature. It is classified as an FO Virginis type of near-contact binary system. Assuming a reasonable value for the mass of the primary component, an estimate of the absolute elements of FU Ara has been made, on the assumption that the primary has a mass corresponding to its spectral type according to Svechnikov ＆ Taidakova.

关键词： binaries: eclipsing stars: fundamental parameters stars: individual:FU Ara

Physical and geometrical parameters of VCBS XIII: HIP 105947

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Research in Astronomy and Astrophysics 2018年第6期18卷 109-120页

作者： Suhail Gumaan Masda Mashhoor Ahmed Al-Wardat Jiyaulla Khan Moula Khan Pathan Physics Department Dr. Babasaheb Ambedkar Marathwada University Aurangabad-431001 Maharashtra India Physics Department Hadhramout University PO Box 50511 Mukalla Yemen Dept. of Physics and Institute of Astronomy and Space Sciences A1 al-Bayt University PO Box 130040 Mafraq25113 Jordan Physics Department Maulana Azad College Aurangabad-431001 Maharashtra India

The best physical and geometrical parameters of the main sequence close visual binary system(CVBS), HIP 105947, are presented. These parameters have been constructed conclusively using Al-Wardat’s complex method for analyzing CVBSs, which is a method for constructing a synthetic spectral energy distribution(SED) for the entire binary system using individual SEDs for each component star. The model atmospheres are in its turn built using the Kurucz(ATLAS9) line-blanketed plane-parallel models. At the same time, the orbital parameters for the system are calculated using Tokovinin’s dynamical method for constructing the best orbits of an interferometric binary system. Moreover, the mass-sum of the components, as well as the ?θ and ?ρ residuals for the system, is introduced. The combination of Al-Wardat’s and Tokovinin’s methods yields the best estimations of the physical and geometrical parameters. The positions of the components in the system on the evolutionary tracks and isochrones are plotted and the formation and evolution of the system are discussed.

关键词： binaries: close binaries: visual stars: fundamental parameters stars: individual(HIP 105947)

What Can the Redshift Observed in EXO 0748-676 Tell Us?

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Chinese Journal of Astronomy and Astrophysics 2003年第1期3卷 33-37页

作者： Ren-Xin XuDepartment of Astronomy, School of Physics, Peking University, Beijing 100871 rxxu@*** Department of Astronomy School of Physics Peking University Beijing 100871 China

The mass-radius relations for bare and crusted strange stars are calculated with the bag model. Comparing these relations with the observed one derived from the redshift of EXO 0748–676, we come to the conclusion that it is incorrect to say that EXO 0748–676 cannot be a strange star. Various strange star models can show that EXO 0748–676 could have a mass of (1.3 ~ 1.7)M☉ and a radius of (8.4 ~ 11.4) km. It is proposed that a proportion of nascent strange stars could be bare and have masses ~ 0.1M☉, and their masses increased over a long period of accretion.

关键词： stars: fundamental parameters dense matter stars: neutron