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

Liao, Wuping; Li, Linjia; Xiao, Zhi Yu; Wang, Qishan

doi:10.1088/1674-4527/21/2/41

Cited by 3 publications

(2 citation statements)

References 71 publications

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“…In this paper, two sets of high-precision BVRI-band light curves for TU Boo observed in 2020 and 2021 respectively. As displayed in Figure 1, the symmetric light curves are first obtained, and significant for understanding the structure and Liao et al (2021) suggest most of G-type shallow contact binaries are undergoing a long-term and periodic orbital period changes, and there are more systems show long-term decrease. In the O−C diagram of Figure 5, the long-term decreasing superposed the cyclic oscillation were found for TU Boo.…”

Section: Discussionmentioning

confidence: 87%

New Photometric Investigations of G-type Contact Binary TU Boo

Wang

Meng

Jiang

et al. 2023

Res. Astron. Astrophys.

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Two sets of CCD photometric observations for contact binary TU Boo were obtained in 2020 and 2021, respectively. Different from its asymmetric light curves published from the literature, our BV RcIc-band curves show that the heights of maximum are almost equal. These distortions of light curves possibly indicate that the components have been active in past 25 yr, but they are stable in the last two years. For total-eclipse binary TU Boo, due to some star-spots on the surface of the components, the physical structure obtained by many investigators are different. Therefore, the symmetric multi-color light curves in 2020, 2021are important for understanding configuration and evolution for this system. By using the Wilson–Devinney (2013) program, it is confirmed that TU Boo is an A-type shallow-contact binary with the temperature difference of ∆T = 152K and fill-out of f = 14:67%. In the O–C diagram of orbital period analysis, a cyclic oscillation superimposed on a continuous decrease was determined. The long-term decreasing is often explained by the mass transfer from the more massive star to less massive one, this system will evolve into a deeper contact binary with time. The cyclic oscillations computed from much more CCD times of light minimum maybe result from the light-travel time effect via the presence of a third body. These characters of structure, evolution and ternary belong to typical A-type W UMa binaries with spectral G.

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Section: Discussionmentioning

confidence: 87%

New Photometric Investigations of G-type Contact Binary TU Boo

Wang

Meng

Jiang

et al. 2023

Res. Astron. Astrophys.

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“…Their period decrease rates are dP = −1.66(±0.02) × 10 −7 day yr −1 for V724 And and dP = −3.98(±0.17) × 10 −7 day yr −1 for QR Com, respectively. This situation occurs in several short-period contact binaries, such as EI CVn (Yang 2011), IU Cnc (Yuan et al 2019), V1007 Cas (Li et al 2018), BN Ari (Alton et al 2018) and IO Cnc (Liao et al 2021). For contact binaries, the period decrease may be attributed the mass transfer from the less massive component to the more massive one, accompanied by mass and angular momentum inevitably losing from the centering binary systems, which can be seen from Equation (9) of Yang et al (2013).…”

Section: Interpreting Period Decreasingmentioning

confidence: 99%

Photometric and Spectroscopic Studies for Two Magnetic-activity Contact Binaries: V724 And and QR Com

Wang¹,

Michel²,

Yuan³

et al. 2022

Res. Astron. Astrophys.

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We presented new CCD photometry for two contact binaries, V724 And and QR Com, which were observed during the 2020-2022 observing seasons. By using the W-D method, the photometric solutions were deduced from new observed data and TESS ones. Their asymmetric light curves were modeled by a dark spot on the more massive component. Results indicate that the starspot may immigrate or disappear on the surface of the active component. From the TESS observations of QR Com, it is discovered that the difference between light maxima exhibits a 29.5-d oscillation, which implies the continuous evolution of spot feathers on the time-scale of several weeks. Their mass ratio and fill-out factor are q = 2.308 and f = 11.55% for V724 And, and q = 0.624 and f = 12.77% for QR Com, respectively. From the (O − C) curve, the orbital period secularly decrease at a rate of dP/dt = −1.66 × 10^{−7} d yr^{−1} for V724 And and dP/dt = −3.98 × 10^{−7} d yr^{−1} for QR Com, which was interpreted by mass transfer from the less massive component to the more massive one. With mass transferring, this kind of shallow-contact binaries, V724 And and QR Com, will evolve into the broken-contact configurations.

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A photometric study of a total-eclipse contact binary V458 Mon

Zubairi,

Ergang,

et al. 2024

New Astronomy

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

Cited by 3 publications

References 71 publications

New Photometric Investigations of G-type Contact Binary TU Boo

New Photometric Investigations of G-type Contact Binary TU Boo

Photometric and Spectroscopic Studies for Two Magnetic-activity Contact Binaries: V724 And and QR Com

A photometric study of a total-eclipse contact binary V458 Mon

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