The photometric study of the low-mass-ratio contact binary EK Aqr

Gao, Xin-Yi; Cai, Ya-Wen; Li, Kai; Gao, Ao; Shao, Yan-Dan

doi:10.1016/j.newast.2022.101800

Cited by 3 publications

(1 citation statement)

References 28 publications

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“…Long term changes of the orbital period in contact binary systems are very common phenomena. According to the investigations, the period of a contact binary is not constant in many cases (Qian 2001;Qian et al 2007;Xiao et al 2016;Yang et al 2022aYang et al , 2022bPanchal et al 2022;Gao et al 2022;Hu et al 2022;Xu et al 2022). However, there are also cases with unchanged periods, such as LQ Com (Hu et al 2022) and PZ UMa (Zhou & Soonthornthum 2019).…”

Section: Secular Period Changesmentioning

confidence: 99%

Period Investigation on Two W UMa Binaries HH UMa and V1175 Her

Chang¹,

Zhu²,

Meng³

2023

Res. Astron. Astrophys.

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HH UMa and V1175 Her are two W UMa contact binary systems whose periods were reported as undergoing secular increase. In this paper, we improved their period analyses with a more extensive database of eclipse timings, finding that both periods show cyclic variation. The cyclic variation could be attributed to a Light Travel Time Effect (LTTE) induced by a third body. Both circular orbit and eccentric orbit cases were considered. For HH UMa, A cyclic variation with a period of around 20 yr has been detected, which may be caused by a third body with the mass larger than 0.23 M⊙. However, no parabolic variation was detected in its O-C curve, implying the balance of the mass transfer between the two components and the angular momentum loss from the binary system. As to V1175 Her, a long-term period increase superposed on a periodic oscillation was detected. The period increase at a rate of about dP/dt = 2×10−7d · yr−1 indicates the mass transfer from the less massive component to its companion. And the cyclic variation of about 7.5 yr could be caused by a hierarchical third body with a minimal mass exceeding 0.46M⊙ orbiting around the central binary. This mass is larger than that of the less massive component of the binary, which means that the secondary component was not replaced by the third body during early stellar interactions, implying it keeps original dynamical information. By removing angular momentum from the central binary system, the tertiary component has played a significant role in the formation of contact binaries.

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Section: Secular Period Changesmentioning

confidence: 99%

Period Investigation on Two W UMa Binaries HH UMa and V1175 Her

Chang¹,

Zhu²,

Meng³

2023

Res. Astron. Astrophys.

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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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Photometric and Spectroscopic Studies of the Long-Period Low-Mass-Ratio Deep-Contact Binary KN Per

Gao¹,

Li²,

Cai³

et al. 2022

PASP

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Photometric analysis and spectroscopic study of the long-period low-mass-ratio deep-contact binary KN Per were performed. The light curves of the BV(RI) c band were from the Ningbo Bureau of Education and Xinjiang Observatory Telescope at the Xingming Observatory. Through the analysis of the Wilson–Devinney program, KN Per was found as an A-type low-mass-ratio deep-contact binary (q = 0.236; f = 53.4%). A cool spot applied on the primary component was introduced to explain the unequal maxima of the light curve. Based on the O − C analysis, we found that the rate of the increasing orbital period is P ̇ = 5.12 ± (0.30) × 10−7 day yr−1, meaning the mass transfer from the secondary component to the primary one. By analyzing the spectroscopic data, we detected chromospheric activity emission line indicators, which correspond to the light-curve analysis. Seventy-one long-period (P > 0.5 day) contact binaries, including our target, were collected. The evolutionary states of all collected stars were investigated by the illustrations of mass–radius, mass–luminosity, and log M T –log J o . The relations of some physical parameters were also determined. With the instability parameters of KN Per, we determined that it is a stable contact binary system at present.

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The photometric study of the low-mass-ratio contact binary EK Aqr

Cited by 3 publications

References 28 publications

Period Investigation on Two W UMa Binaries HH UMa and V1175 Her

Period Investigation on Two W UMa Binaries HH UMa and V1175 Her

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

Photometric and Spectroscopic Studies of the Long-Period Low-Mass-Ratio Deep-Contact Binary KN Per

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