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Absolute physical parameters of three poorly studied detached eclipsing binaries

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Research in Astronomy and Astrophysics 2021年第1期21卷 220-228页

作者： Dao-Ye Yang Li-Fang Li Quan-Wang Han Yunnan Observatories Chinese Academy of SciencesKunming 650216China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650216China University of Chinese Academy of Sciences Beijing 100049China Center for Astronomical Mega-Science Chinese Academy of SciencesBeijing 100012China Key Lab of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 10101China School of Physics and Electronics Qiannan Normal University for NationalitiesDuyun 558000China

The photometric and spectroscopic data for three double-lined detached eclipsing binaries were collected from the photometric and spectral *** light and radial velocity curves of each binary system were simultaneously analyzed using Wilson-Devinney(WD)code,and the absolute physical and orbital parameters of these binaries were *** masses of both components of ASASSN-V J063123.82+192341.9 were found to be M1=1.088±0.016 and M20.883±0.016 M⊙;those of ASAS J011416+0426.4 were determined to be M1=0.934±0.046 and M2=0.754±0.043 M⊙;and those of MW Aur were derived to be M1=2.052±0.196 and M21.939±0.193 M⊙.Finally,the evolutionary status of these detached binaries was discussed based on their absolute parameters and the theoretical stellar models.

关键词： stars:binaries:eclipsing stars:fundamental parameters stars:evolution stars:individual:ASASSN-V J063123.82+192341.9,ASAS J011416+0426.4 and MW Aur

Photometric investigation of the eclipsing binary TX Herculis observed by LUT

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Research in Astronomy and Astrophysics 2019年第7期19卷 47-52页

作者： Li-Ying Zhu Xiao-Man Tian Xiao Zhou Lin-Jia Li Zhi-Hua Wang Yunnan Observatories Chinese Academy of SciencesKunming 650216China Center for Astronomical Mega-Science Chinese Academy of SciencesBeijing 100101China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650216China University of the Chinese Academy of Sciences Beijing 100049China

The lander of China’s Chang’E-3 spacecraft is equipped with a 15-cm telescope that is very useful for monitoring celestial objects in the ultraviolet(UV) band(245–340 nm).The Lunar-based Ultraviolet Telescope(LUT) is the first long-term lunar-based astronomical observatory,that can make uninterrupted observations of a target from the *** we present the continuous complete UV light curve of the eclipsing binary TX Herculis(TX Her).The analysis of the light curve suggests that TX Her is a detached *** dip in the light curve was explained by the emergence of a stellar dark spot on the less massive F0 type *** cyclic change of arrival eclipse times for the system reveals that it contains an additional stellar companion with a minimal mass of 0.35 M⊙ and a period of 48.92 yr,which is supported by the detected light contribution of the third body from light curve *** third body may play an important role in the formation of the present short-period system TX Her.

关键词： stars:binaries:close stars:binaries:eclipsing stars:individuals (TX Herculis) stars:multiple system stars:activity

Mass transfer and possible third-body effect on the period variations of the near-contact binary CN And

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Research in Astronomy and Astrophysics 2019年第8期19卷 3-10页

作者： Jin-Ting Cai Yun-Xia Yu Ke Hu Fu-Yuan Xiang Department of Physics Xiangtan University

We present a period analysis of the near-contact binary CN And using all available times of light minima. It is revealed that the orbital period exhibits a long-term decrease as well as a small-amplitude cyclic oscillation. This result suggests that the secular period decrease at the rate of d P/dt =-1.4017 ×10-7 d yr-1 is caused by a combination of mass transfer and angular momentum loss due to magnetic braking. The periodic variation with an amplitude of A = 0.0036 d and a period of Pmod = 28.3542 yr should be rooted in the light-time effect of a third body, rather than cyclic magnetic activity.

关键词： stars:binaries:close stars:binaries:eclipsing stars:individual:CN And

1SWASP J034439.97+030425.5:a short-period eclipsing binary system with a close-in stellar companion

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Research in Astronomy and Astrophysics 2020年第4期20卷 31-38页

作者： Bin Zhang Sheng-Bang Qian Jing-Jing Wang Qi-Jun Zhi Ai-Jun Dong Wei Xie Li-Ying Zhu Lin-Qiao Jiang School of Physics and Electronic Science Guizhou Normal UniversityGuiyang 550001China Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal UniversityGuiyang 550001China Yunnan Observatories Chinese Academy of SciencesKunming 650216China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of SciencesKunming 650216China University of Chinese Academy of Sciences Beijing 100049China Center for Astronomical Mega-Science Chinese Academy of SciencesBeijing 100101China China University of Petroleum-Beijing at Karamay Karamay 834000China School of Physics and Electronic Engineering Sichuan University of Science and EngineeringZigong 643000China

First multi-wavelength photometric light curves(LCs)of the short-period eclipsing binary(EB)1 SWASP J034439.97+030425.5(hereafter J0344)are presented and analyzed by using the 2013 version of the Wilson-Devinney(W-D)*** explain the asymmetric LCs of J0344,a cool star-spot on the less massive component was *** photometric solutions suggest that J0344 is a W-subtype shallow contact EB with a contact degree of f=4.9%±3.0%and a mass ratio of q=2.456±***,an obvious third light was detected in our *** calculated the average luminosity contribution of the third light to the total light,and that value reaches up to 49.78%.Based on the O-C method,the variations of the orbital period were studied for the first *** O-C diagram reveals a secular decrease superimposed on a cyclic *** orbital period decreases at a rate of d P/dt=-6.07×10-7 d yr-1,which can be explained by the mass transfer from the more massive component to the less massive ***,its O-C diagram also shows a cyclic oscillation with an amplitude of 0.0030 d and a period about 7.08 yr,which can be explained by the presence of a third body with a minimum mass of M3 min=0.15±0.02 M⊙.The third component may play an important role in the formation and evolution of J0344 by drawing angular momentum from the central system.

关键词： stars:binaries:close stars:binaries:eclipsing stars:individual(1SWASP J034439.97+030425.5)

The first photometric analysis and period investigation of the K-type W UMa type binary system V0842 Cep

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Research in Astronomy and Astrophysics 2021年第5期21卷 201-206页

作者： Yu-Yang Li Kai Li Yuan Liu Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment Institute of Space SciencesShandong UniversityWeihai 264209China Qilu Institute of Technology Jinan 250200China

V0842 Cep is a W UMa-type binary star that has been neglected since its *** analysed the V RcIc light curves,obtained by the 1 m telescope at Weihai Observatory of Shandong University,using the Wilson-Devinney code.V0842 Cep was found to be a shallow contact binary system(f=8.7%)with a mass ratio of *** its orbital inclination is greater than 80◦,the photometric results are reliable.A period study is included which reveals a continually decreasing orbital period(dp/dt=1.50(±0.42)×10^(−7)d y^(r−1)).This trend could be attributed to the angular momentum loss via stellar wind.

关键词： stars:binaries:close stars:binaries:eclipsing stars:individual(V0842 Cep)

New photometric investigation of the low-mass-ratio contact binary star V1853 Orionis

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Research in Astronomy and Astrophysics 2019年第4期19卷 77-88页

作者： Jia-Jia He Sheng-Bang Qian Boonrucksar Soonthornthum Amornrat Aungwerojwit Niang-Ping Liu Thawicharat Sarotsakulchai 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 National Astronomical Research Institute of Thailand 191 Siriphanich Bldg.2nd Fl.Huay Kaew Rd.Suthep DistrictMuang Department of Physics Faculty of Science Naresuan University

Four-color charge-coupled device(CCD) light curves in the B, V, Rc and I c bands of the totaleclipsing binary system V1853 Orionis(V1853 Ori) are presented. By comparing our light curves with those published by previous investigators, it is determined that the O'Connell effect on the light curves has disappeared. By analyzing those multi-color light curves with the Wilson-Devinney code(W-D code),it is discovered that V1853 Ori is an A-type intermediate-contact binary with a degree of contact factor of f = 33.3%(3.7%) and a mass ratio of q = 0.1896(0.0013). Combining our 10 newly determined times of light minima together with others published in the literature, the period changes of the system are investigated. We found that the general trend of the observed minus calculated(O-C) curve shows a downward parabolic variation that corresponds to a long-term decrease in the orbital period with a rate of d P/dt =-1.96(0.46)×10^(-7) d yr^(-1). The long-term period decrease could be explained by mass transfer from the more-massive component to the less-massive one. By combining our photometric solutions with data from Gaia DR_2, absolute parameters were derived as M_1 = 1.20 M⊙, M_2 = 0.23 M⊙, R_1 = 1.36 R⊙and R_2 = 0.66 R⊙. The long-term period decrease and intermediate-contact configuration suggest that V1853 Ori will evolve into a high fill-out overcontact binary.

关键词： stars: binaries:close stars:binaries:eclipsing stars:individual(V1853 Ori)

Investigation of the shortest period Am type eclipsing binary TYC 6408–989–1

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Research in Astronomy and Astrophysics 2021年第3期21卷 107-116页

作者： Xiao-Man Tian School of Aeronautics Shandong Jiaotong University Jinan 250000China Center for Astronomical Mega-Science Chinese Academy of Sciences Beijing 100101China

The first BV bands photometric observations and the low-resolution spectrum of the shortest period Am type eclipsing binary TYC 6408-989-1 have been *** stellar atmospheric parameters of the primary star were obtained through the spectral fitting as follows:Teff=6990±117 K,log g=4.25±0.26 cm s^(-2),[Fe/H]=-0.45±0.03 *** original spectra obtained by European Southern Observatory(ESO)were processed with an IRAF package by *** on the ESO blue-violet spectra,TYC 6408-989-1 was concluded as a marginal Am(Am:)star with a spectral type of kA3 hF1 mA5Ⅳ-Ⅴidentified through the MKCLASS *** observed light curves were analyzed through the WilsonDevinney *** final photometric solutions show that TYC 6408-989-1 is a marginal contact binary with a low mass ratio(q=0.27).The temperature of the secondary component derived through the light curve analysis is significantly higher than main sequence *** addition,TYC 6408-989-1 is a poor thermal contact *** temperature differences between the two components is about 1800 ***6408-989-1 should be located in the oscillation stage predicted by the thermal relaxation oscillations theory(TRO)and will evolve into the shallow contact stage *** very short period(less than one day),marginal Am peculiarity and quite large rotational velocity(v sin i■160 km s^(-1))make TYC 6408-989-1 become a challenge to the cut-off of rotation velocities and periods of Am *** have collected the well known eclipsing Am binaries with absolute parameters from the literature.

关键词： stars:chemically peculiar stars:binaries:eclipsing stars:binaries:general(TYC 64089891) stars:evolution

Physical properties of three short period close binaries:KIC 2715417,KIC 6050116 and KIC 6287172

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Research in Astronomy and Astrophysics 2019年第2期19卷 111-124页

作者： Mahmoud AbdelFattah NegmEldin Ahmed Essam Elsayed Shahinaz Mostafa Yousef Astronomy Space Science and Meteorology Department Faculty of Science Cairo University Department of Astronomy National Research Institute of Astronomy and Geophysics(Egypt)

We present the physical parameters of three short period close binaries using data observed from the Kepler Space Telescope. All of these observations were taken in a single bandpass(which approximates the Johnson V-band). Our three systems are KIC 2715417, KIC 6050116 and KIC 6287172. The first system, KIC 2715417, is considered a semi-detached system with the secondary component filling its Roche lobe. The second system, KIC 6050116, is an overcontact system, while the third system, KIC 6287172, belongs to ellipsoidal variables as deduced from the Roche lobe geometry. For photometric analysis, we used the PHOEBE software package, which is based on the Wilson-Devinney code. Due to lack of spectroscopic data, the photometric mass ratios are determined from the analyses of light curves using the q-search method. The absolute parameters are determined using three different methods(Harmanec, Maceroni &Van'tVeer and Gazeas & Niarchos).

关键词： stars:binaries:eclipsing stars:fundamental parameters stars:luminosity function,mass function stars:individual(KIC 2715417,KIC 6050116 and KIC 6287172)

Photometric analysis of two extreme low mass ratio contact binary systems

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Research in Astronomy and Astrophysics 2021年第9期21卷 217-223页

作者： Surjit S.Wadhwa Nick F.H.Tothill Ain Y.De Horta Miroslav Filipovié School of Science Western Sydney UniversityLocked Bag 1797PenrithNSW 2751Australia

Multi-band photometry and light curve analysis for two newly recognized contact binary systems,TYC 6995-813-1 and NSVS 13602901,are *** were found to be of extreme low mass ratios 0.11 and 0.17,*** secondary components of both systems show evidence of considerable evolution with elevated densities as well as both luminosity and radii well above their main sequence *** in the absence of significant spot activity,at least one of the systems,TYC 6995-813-1,displays features of magnetic and chromospheric *** 6995-813-1 is also determined to be a potential merger candidate with its current separation near the theoretical instability separation.

关键词： stars:binaries:eclipsing stars:evolution stars:low-mass techniques:photometric