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Long-period eclipsing binaries:towards the true mass-luminosity relation.I.the test sample,observations and data analysis

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Research in Astronomy and Astrophysics 2020年第8期20卷 169-176页

作者： Alexei Yu.Kniazev Oleg Yu.Maikov Ivan Yu.Katkov Leonid N.Berdnikov South African Astronomical Observatory P.O.Box 9ObservatoryCape Town7935South Africa Southern African Large Telescope P.O.Box 9ObservatoryCape Town7935South Africa Sternberg Astronomical Institute Lomonosov Moscow State UniversityMoscow119992Russia Institute of Astronomy of RAS Moscow 119017Russia New York University Abu Dhabi PO Box 129188Abu DhabiUAE Center for Astro Particleand Planetary PhysicsNYU Abu DhabiPO Box 129188Abu DhabiUAE

The mass-luminosity relation is a fundamental law of astrophysics.We have suggested that the currently used mass-luminosity relation is not correct for the M/M⊙>2.7 range of mass since it was created utilizing double-lined eclipsing binaries,where the components are synchronized and consequently change each other's evolutionary path.To exclude this effect,we have started a project to study longperiod massive eclipsing binaries in order to construct radial velocity curves and determine masses for the components.We outline our project and present the selected test sample together with the first HRS/SALT spectral observations and the software package,FITTING BINARY stars(FBS),that we developed for the analysis of our spectral data.As the first result,we present the radial velocity curves and best-fit orbital elements for the two components of the FP Car binary system from our test sample.

关键词： stars:luminosity function mass function stars:binaries:spectroscopic

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Research on the HIP 18856 binary system

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Research in Astronomy and Astrophysics 2021年第3期21卷 69-72页

作者： Polina Efremova Arina Mitrofanova Vladimir Dyachenko Anatoly Beskakotov Alexander Maksimov Denis Rastegaev Yury BalegaSergey Komarinsky Kazan Federal University Kazan 420008Russia Special Astrophysical Observatory of the Russian Academy of Sciences Nizhnij ArkhyzRussia 369167

The results of a study on the binary HIP 18856 and construction of its orbit are presented.New observational data were obtained at the BTA of SAO RAS in 2007-2019.Earlier,Cvetkovic et al.constructed the orbit for this system.However,it is based on six measurements,which cover a small part of the orbit.The positional parameters of the ESA astrometric satellite Hipparcos published speckle interferometric data(Mason et al.,Balega et al.,Horch et al.)and new ones were used in this study.Based on the new orbital parameters,the mass sum was calculated and the physical parameters of the components were found.The obtained orbital and fundamental parameters were compared with the data from the study by Cvetkovic et al..The comparison shows that the new orbital solution is better than the old one,since it fits new observational data accurately.Also based on a qualitative evaluation performed by Worley&Heintz,the new orbit was classified as"reliable",which means data cover more than half of the orbit with sufficient quantities of residuals of measurements.

关键词： techniques:high angular resolution,speckle interferometry stars:low-mass,fundamental parameters stars:binaries:spectroscopic stars:individual:HIP 18856

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Physical properties of γ Doradus pulsating stars and their relationship with long-period δ Scuti variables

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Research in Astronomy and Astrophysics 2019年第1期19卷 1-20页

作者： Sheng-Bang Qian Lin-Jia Li Jia-Jia He Jia Zhang Li-Ying Zhu Zhong-Tao Han Yunnan Observatories Chinese Academy of Sciences Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Center for Astronomical Mega-Science Chinese Academy of Sciences University of Chinese Academy of Sciences

We present LAMOST data on 168 γ Doradus(γ Dor) pulsating stars including stellar atmospheric parameters of 137 variables and spectral types for all of the samples. The distributions of period(P), temperature(T), gravitational acceleration(log(g)) and metallicity [Fe/H] are shown. It is found that most γ Dor variables are main-sequence stars with early F spectral types and temperatures from 6880 K to7280 K. They are slightly more metal poor than the Sun with a metallicity range from-0.4 to 0. On the H-R and log g-T diagrams, both the γ Dor and δ Scuti(δ Sct) stars occupy in the same region and some are beyond the borders predicted by current stellar pulsation theories. It is discovered that the physical properties of γ Dor stars are similar to those of long-period δ Sct(P > 0.3 d) stars. The stellar atmospheric parameters are all correlated with the pulsation period for short-period δ Sct variables(P stars. These results reveal that γ Dor and long-period δ Sct are the same group of pulsating stars and they are different from short-period δ Sct variables. Meanwhile, 33γ Dor stars are identified as candidates of binary or multiple systems.

关键词： stars:fundamental parameters stars:oscillations stars:binaries:spectroscopic stars:variables:other

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