New Photometric Investigation of the Solar-Type Shallow-Contact Binary HH Bootis

He, J.-J.; Qian, S.‐B.; Soonthornthum, Boonrucksar; Aungwerojwit, A.; Liu, Niang-Ping; Sarotsakulchai, Thawicharat

doi:10.1155/2019/5641518

Cited by 3 publications

(2 citation statements)

References 34 publications

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“…Orbital period variations are quite common among close binary systems due to the possible angular momentum loss (ALM) from binary systems or mass transfer between the primary or secondary stars (Zhang et al 2018a;Liu et al 2018). Thus, the O − C method was widely used in correcting orbital period or calculating orbital period variations of close binaries (Pi et al 2017;He & Wang…”

Section: Orbital Period Investigationmentioning

confidence: 99%

Orbital period correction and light curve modeling of the W-subtype shallow contact binary OW Leo

Xiao

Qian

2021

Res. Astron. Astrophys.

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Orbital period and multi-color light curves′ investigation of OW Leo are presented for the first time. The orbital period of OW Leo is corrected from P = 0.325545 days to P = 0.32554052 days in our work, and the observational data from the All-Sky Automated Survey for SuperNovae (ASAS-SN) are used to test the newly determined orbital period. Then, the phased light curves are calculated with the new period and the Wilson-Devinney program is applied to model the light curves, which reveal that OW Leo is a W-subtype shallow contact binary system (q = 3.05, f = 12.8 %). The absolute physical parameters of the two component stars are estimated to be M 1 = 0.31(1)M ⊙, M 2 = 0.95(3)M ⊙, R 1 = 0.63(1)R ⊙, R 2 = 1.04(1)R ⊙, L 1 = 0.43(1)L ⊙ and L 2 = 1.01(2)L ⊙. The evolutionary status shows that the more massive star is less evolved than the less massive star. OW Leo has very low metal abundance, which means its formation and evolution are hardly influenced by any additional component. It is formed from an initially detached binary system through nuclear evolution and angular momentum loss via magnetic braking, and has passed a very long time of main sequence evolution.

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Section: Orbital Period Investigationmentioning

confidence: 99%

Orbital period correction and light curve modeling of the W-subtype shallow contact binary OW Leo

Xiao

Qian

2021

Res. Astron. Astrophys.

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show abstract

“…( Liu et al 2018). Thus, the O -C method was widely used in correcting orbital period or calculating orbital period variations of close binaries (Pi et al 2017;He & Wang 2019). For analysis the orbital period of OW Leo, all available mid-eclipse times are gathered and listed Table 4.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Orbital period correction and light curve modeling of the W-subtype shallow contact binary OWLeo

Zhou,

Qian

2020

Preprint

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Orbital period and multi-color light curves' investigation of OW Leo are presented for the first time. The orbital period of OW Leo is corrected from P = 0.325545 days to P = 0.32554052 days in our work, and the observational data from the All-Sky Automated Survey for SuperNovae (ASAS-SN) are used to test the newly determined orbital period. Then, the phased light curves are calculated with the new period and the Wilson-Devinney program is applied to model the light curves, which reveal that OW Leo is a W-subtype shallow contact binary system (q = 3.05, f = 12.8 %). The absolute physical parameters of the two component stars are estimated to be MThe evolutionary status show that the more massive star is less evolved than the less massive star. OW Leo has very low metal abundance, which means its formation and evolution are hardly influenced by any additional component. It is formed from an initially detached binary systems through nuclear evolution and angular momentum loss via magnetic braking, and have passed a very long time of main sequence evolution.

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The first photometric investigations of the G-type shallow contact binary IO Cnc

Liao

Xiao

et al. 2021

Res. Astron. Astrophys.

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IO Cnc was classified to be a new G-type (G0) W UMa-type eclipsing binary system. Our first multicolor photometric solutions show that IO Cnc is a new W-subtype shallow contact binary with a fill-out factor of f = 16.1% and a low mass ratio of q = 3.12 (or 1/q = 0.32). During orbital period investigations, a cyclic variation and a downward parabolic variation with a rate of (−1.28 ± 0.43) × 10−7 d yr−1 was discovered in the observed–calculated (O − C) curve. The cyclic variation was analyzed by the light travel time effect (LTTE) via a potential red dwarf companion star, an orbital semi-major axis shorter than 4.88 ± 0.82 AU was obtained. Finally, we collect physical parameters of a sample of 50 G-type shallow contact binaries (f ≤ 20%), it is suggested that most of the G-type shallow contact binaries are undergoing a long-term and periodic orbital period changes, especially more systems show long-term decreases. The long-term orbital period decrease indicates that IO Cnc is in a mass transferring from the more massive component to the less massive one. With the long-term decrease of the orbital period, this shallow contact binary will evolve into a deeper contact one.

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New Photometric Investigation of the Solar-Type Shallow-Contact Binary HH Bootis

Cited by 3 publications

References 34 publications

Orbital period correction and light curve modeling of the W-subtype shallow contact binary OW Leo

Orbital period correction and light curve modeling of the W-subtype shallow contact binary OW Leo

Orbital period correction and light curve modeling of the W-subtype shallow contact binary OWLeo

The first photometric investigations of the G-type shallow contact binary IO Cnc

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