Magnetic activity and orbital parameters of CC Com based on photometric data, LAMOST low- and medium-resolution spectra

Zhu, Zong-Hong; Zhang, Liyun; Meng, Gang; Cheng, Yao; Long, Lijuan; Han, Xianming L.; Pi, Qingfeng; Jiang, Liqiao

doi:10.1088/1674-4527/21/4/84

Cited by 5 publications

(3 citation statements)

References 44 publications

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“…Among such systems, there are only five spectroscopically confirmed ones. This includes CC Com, the first USPCB identified system with P = 0.2207 day (Rucinski et al 1977;Pribulla et al 2007;Zhu et al 2021), and the most recent one, 1SWASP J093010.78+533859.5, which is a doubly eclipsing quintuple system containing a EW with P = 0.2277 day and a detached binary with probably a fifth companion (Lohr et al 2015). The shortest-period system is the M dwarf EW SDSS J200011.19+003806.5, with P = 0.19856 day, discovered by Becker et al (2011) and confirmed spectroscopically by Davenport et al (2013).…”

Section: Discussionmentioning

confidence: 99%

Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys

Παπαγεωργίου

Christopoulou

Lopes

et al. 2023

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We present the photometric analysis of three ultra-short-period total eclipsing binaries in contact configuration, CRTS_J172718.0+431624, OGLE-BLG-ECL-000104, and OGLE-BLG-ECL-000012, mined from massive astronomical surveys. Using the available archival light curves (LCs) from Vista Variables in the Vía Láctea (VVV), Optical Gravitational Lensing Experiment (OGLE), Zwicky Transient Facility, and Catalina Sky Survey in different passbands and new multiband photometric observations with the 2.3 m Aristarchos telescope at Helmos Observatory, their relative physical parameters were derived. We explored the parameter space by using the PIKAIA genetic algorithm optimizer. The best photometric solution and error budget estimation were adopted for each system through Markov Chain Monte Carlo sampling of the global optimum. The approximate absolute parameters were derived for each contact system adopting an empirical mass–luminosity relation. All three systems have a mass ratio lower than 0.5. The exchange between the primary and secondary depths of CRTS_J172718.0+431624 during 2016–2022 may be due to spot activity. In addition, we present a detailed analysis of the first well-characterized shortest-period contact eclipsing binary with total eclipses known so far (OGLE-BLG-ECL-000104). Thanks to VVV and OGLE LCs, new distances were derived for OGLE-BLG-ECL-000104 and OGLE-BLG-ECL-000012 using empirical period–luminosity relations. The origin and evolutionary status of all three ultra-short-period contact binaries are thoroughly discussed in the context of the detached binary formation channel.

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Section: Discussionmentioning

confidence: 99%

Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys

Παπαγεωργίου

Christopoulou

Lopes

et al. 2023

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“…However, the cyclic variation in the orbital period can be reasonably explained via the presence of a third body. Many such binaries are known to harbor third bodies (Fang et al 2019;Devarapalli et al 2020;Zhu et al 2021), which can be detected by their contribution to total light in the light curve analysis using the WD method where M bin and m 3 are the total mass of the binary and the third body respectively, and G is the gravitational constant. The derived third body parameters are expressed in Table 3.…”

Section: Discussionmentioning

confidence: 99%

The First Photometric and Spectroscopic Study of Contact Binary V2840 Cygni

POTHUNENI¹,

Devarapalli²,

Rukmini³

2023

Res. Astron. Astrophys.

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The first photometric, spectroscopic, and period variation studies of neglected short-period eclipsing binary V2840 Cygni are presented. High Mass Ratio Contact Binaries, especially those in the weak-contact configuration are vital while probing into the evolutionary models of CBs using stellar parameters. The photometric solutions reveal the weak-contact nature of V2840 Cygni with a high mass ratio ($\sim1.36$), motivating us to investigate the nature of such binaries. The period variation study of V2840 Cygni spanning for 15 years shows a secular period decrease at a rate of \begin{math}\sim5.5\times10^{-7}\end{math}d/yr indicating mass transfer between the components. The superimposed cyclic variation provides a basic understanding of the possible third body (\emph{P$_3$}$\sim8$ yr, \emph{m$_3$}$\sim0.51$M$_\odot$). Following the derived parameters, the evolution of the system is discussed based on Thermal Relaxation Oscillation (TRO) model. It is found that V2840 Cygni falls in a special category of HMRCBs, that validates TRO. To characterise the nature of HMRCBs, a catalog of 114 CBs with high mass ratios has been compiled along with their derived parameters from the literature. For all the HMRCBs in the study, a possible correlation between their contact configuration and observed period variations for relative log\emph{J$_{rel}$} is discussed. The spectroscopic study of V2840 Cygni provides evidence of the presence of magnetic activity in the system and the existence of ongoing mass transfer which is additionally deduced from the period variation study. The LAMOST spectra of 30 HMRCBs are collected to interpret the stellar magnetic activity in such systems.

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“…The follow-up LAMOST spectroscopic observations in the Kepler field, such as the lowresolution LAMOST-Kepler (LK) project (De Cat et al 2015;Zong et al 2018b;Fu et al 2020) and the time-domain LAMOST-Kepler Medium Resolution Spectroscopic Survey (LK-MRS; Zong et al 2020), provide reliable atmospheric parameters and RVs for these EBs. By combing LAMOST spectra and photometric light curves, several works of orbital parameters and magnetic activity of EBs have been studied (e.g., Lu et al 2020;Pan et al 2020;Zhu et al 2021;Niu et al 2022). Therefore, the combination between Kepler photometry and LAMOST spectroscopy gives an opportunity to measure physical parameters and explore starspot activity of triple-lined systems.…”

Section: Introductionmentioning

confidence: 99%

The Physical Properties and Starspot Activity of the Triple System KIC 6525196

Pan¹,

Fu²,

Zhang³

et al. 2022

Res. Astron. Astrophys.

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We present the results of photometric and spectroscopic analysis for the triplelined system KIC 6525196, an eclipsing binary accompanied by a third star. By modeling the Kepler light curves and radial velocities from LAMOST and HIDES observations, absolute parameters of the system are determined. Both components of the eclipsing binary are found to be solar-like stars with masses and radii of M1 = 1.0286 ± 0.0026M⊙, R1 = 1.127 ± 0.008R⊙, and M2 = 0.9667 ± 0.0024M⊙, R2 = 0.963 ± 0.007R⊙. The mass of the third star is determined to be M3 = 0.772 ± 0.010M⊙. With the out-of-eclipse light residuals, we measure rotation period and decay timescale of active region by using the autocorrelation function. In comparison to the Sun, the activity level of the system is significantly stronger. In addition, a possible short photometric activity cycle of ∼ 244 days is detected.

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Magnetic activity and orbital parameters of CC Com based on photometric data, LAMOST low- and medium-resolution spectra

Cited by 5 publications

References 44 publications

Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys

Three Ultra-short-period Contact Eclipsing Binary Systems Mined from Massive Astronomical Surveys

The First Photometric and Spectroscopic Study of Contact Binary V2840 Cygni

The Physical Properties and Starspot Activity of the Triple System KIC 6525196

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