Photometric Study and Absolute Parameter Estimation of Six Totally Eclipsing Contact Binaries

Li, Kai; Xia, Qi-Qi; Kim, Chun-Hwey; Gao, Xing; Hu, Shaoming; Guo, Dadong; Gao, Dong-Yang; Chen, Xu; Guo, Ya-Ni

doi:10.3847/1538-3881/abfc53

Cited by 65 publications

(55 citation statements)

References 241 publications

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“…We carried out a project on the analysis of ELMRCBs. Statistical and simulation studies have indicated that the photometric mass ratios are consistent with the spectroscopic ones for totally eclipsing contact binaries (Rucinski 2001;Pribulla et al 2003;Terrell & Wilson 2005;Li et al 2021b). Rucinski (2001) determined the relationship between the maximum amplitude, the mass ratio, and the contact degree for contact binaries, and found that the smaller the amplitude, the smaller the mass ratio.…”

Section: Introductionmentioning

confidence: 73%

“…The relationship between the mean residual and mass ratio q is shown in Figure 1. It is clearly seen that all the q − search curves have very deep and sharp minima, indicating very precise mass ratio can be obtained (e.g., Zhang et al 2017;Li et al 2019Li et al , 2021bTerrell 2022). The mass ratio corresponding to the minimum of the mean residual was chosen as the initial value and an adjustable parameter, new solutions were started to obtain a convergent result, then the errors of mass ratio can be determined.…”

Section: Light-curve Investigationmentioning

confidence: 99%

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Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems

Gao

Liu

et al. 2022

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The photometric and spectroscopic investigations of ten contact binaries were presented for the first time. It is discovered that the mass ratios of all the ten targets are smaller than 0.15, they are extremely low mass ratio contact binaries. Seven of them are deep contact binaries, two are medium contact binaries, while only one is a shallow contact system. Five of them show the O’Connell effect, and a dark spot on one of the two components can lead to a good fit of the asymmetric light curves. The orbital period studies of the ten binaries reveal that they all exhibit long-term period changes, six of them are increasing, while the others are shrinking. The LAMOST spectra were analyzed by the spectral subtraction method, and all the ten targets exhibit excess emissions in the H α line, indicating chromospheric activity. The evolutionary states of the two components of the ten binaries were studied, and it is found that their evolutionary states are identical to those of the other contact binaries. Based on the study of the relation between orbital angular momentum and total mass, we discovered the ten systems may be at the late evolutionary stage of a contact binary. The initial masses of the two components and the ages of them were obtained. By calculating the instability parameters, we found that the ten contact binaries are relatively stable at present.

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Section: Introductionmentioning

confidence: 73%

Section: Light-curve Investigationmentioning

confidence: 99%

Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems

Gao

Liu

et al. 2022

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“…Terrell & Wilson (2005) showed that the photometric mass ratio accuracy decreases as the system geometry changes from full eclipse to partial eclipse. Among 101 systems (59 total eclipsing and 42 partially eclipsing) collected by Li et al (2021), almost half of the partial eclipsing binary photometric mass ratios were found to differ from the ones determined from RV curves. The mismatch was as big as 0.4 in some cases where the orbital inclination angle was less than 70 • .…”

Section: Resultsmentioning

confidence: 88%

Long-term photometric and low-resolution spectroscopic analysis of five contact binaries

Panchal,

Joshi,

De Cat

et al. 2021

Preprint

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A photometric and spectroscopic investigation is performed on five W Ursae Majoris eclipsing binaries (EWs) J015818.6+260247 (hereinafter as J0158b), J073248.4+405538 (hereinafter as J0732), J101330.8+494846 (hereinafter as J1013), J132439.8+130747 (hereinafter as J1324) and J152450.7+245943 (hereinafter as J1524). The photometric data are collected with the help of the 1.3 m Devasthal Fast Optical Telescope (DFOT), the 1.04 m Sampurnanand Telescope (ST) and the TESS space mission. The low-resolution spectra of the 4 m Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) are used for spectroscopic analysis. The orbital period change of these systems is determined using our and previously available photometric data from different surveys. The orbital period of J1013 and J1524 is changing with a rate of −2.552(±0.249) × 10 −7 days yr −1 and −6.792(±0.952) × 10 −8 days yr −1 , respectively, while others do not show any orbital period change. The orbital period change of J1013 and J1524 corresponds to a mass transfer rate of 2.199 × 10 −7 M yr −1 and 6.151 × 10 −8 M yr −1 from the primary to the secondary component in these systems. It is likely that angular momentum loss via magnetic braking may also be responsible for the observed orbital period change in the case of J1524. All systems have a mass-ratio lower than 0.5, except J0158b with a mass-ratio of 0.71. All the systems are shallow type contact binaries. The J0158b and J1524 are A-subtype while others are W-subtype. The H α emission line region is compared with template spectra prepared using two inactive stars with the help of STARMOD program. The J0158, J1324 and J1524 systems show excess emission in the residual spectra after subtraction of the template.

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“…The primary component of TIC 0349294422 is bigger as well as hotter, which suggests TIC 0349294422 is an A-subtype system, and the bigger component of TIC 0155968973 is cooler, suggesting that TIC 0155968973 is a W-subtype one. Thus they may be formed from distinct formation channels (e.g., Li et al 2021).…”

Section: Discussionmentioning

confidence: 99%

“…In the diagram of log L−log T in Figure 8, we can see that both components of detached binaries are within or very close to the MS band (the area between ZAMS and TAMS). In the log R −log M and log L−log M diagrams, the more massive primary of the W UMa-type contact binary TIC 0349294422 is close to the ZAMS, while its less massive secondary is out of TAMS, which indicates that the more massive primary in the binary should be less evolved than the less massive secondary (e.g., Yakut & Eggleton 2005;Li et al 2021). The detached system TIC 0122446076 may begin to leave the TAMS since the primary and the secondary are located on the TAMS loci in all the diagrams.…”

Section: Discussionmentioning

confidence: 99%

Analysis of Five Double-lined Spectroscopic Eclipsing Binaries Observed with TESS and LAMOST

Lei¹,

Li²,

Zhou³

et al. 2022

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Based on analysis of high-precision photometry from the Transiting Exoplanet Survey Satellite combining with spectroscopy from the medium-resolution spectra of the Large Sky Area Multi-Object Fiber Spectroscopic Telescope, we investigated five double-lined spectroscopic eclipsing binaries (TIC 0165626871, TIC 0159105847, TIC 0122446076, TIC 0349294422, and TIC 0155968973). With the help of Wilson–Devinney program, we accurately derived their absolute stellar parameters. TIC 0165626871, TIC 0159105847, and TIC 0122446076 were identified as detached binaries, while TIC 0349294422 and TIC 0155968973 were recognized as A-subtype and W-subtype W UMa-type systems, respectively. Especially, absolute parameters of four binaries except for TIC 0122446076 were obtained for the first time. TIC 0165626871 also shows light variations of out-of-eclipse phases, which are probably contributed by starspots. The light pulsations of TIC 0122446076 could originate from the primary star that is located in the classical Cepheid instability strip. Evolutionary states of all stars were also discussed.

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Photometric Study and Absolute Parameter Estimation of Six Totally Eclipsing Contact Binaries

Cited by 65 publications

References 241 publications

Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems

Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems

Long-term photometric and low-resolution spectroscopic analysis of five contact binaries

Analysis of Five Double-lined Spectroscopic Eclipsing Binaries Observed with TESS and LAMOST

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