High Fill-Out, Extreme Mass Ratio Overcontact Binary Systems. X. The Newly Discovered Binary Xy Leonis Minoris

Qian, S.‐B.; Liu, L.; Zhu, L.-Y.; He, Jiajia; Yang, Yisi; Bernasconi, L.

doi:10.1088/0004-6256/141/5/151

Cited by 34 publications

(5 citation statements)

References 31 publications

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“…Roughly 13 per cent of low-mass stellar systems contain three or more stars (Tokovinin 2014 ;Fuhrmann et al 2017 ). Low-mass binaries with periods of less than three days are expected to exist in hierarchical systems at a fraction of ∼ 96 per cent (Tokovinin et al 2006 ;Qian et al 2011 ). The predicted detection rate of these systems by LISA is uncertain; ho we ver, it is reasonable to expect these systems to play a large role in the observed GB population.…”

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confidence: 79%

Bayesian characterization of circumbinary sub-stellar objects with LISA

Katz

Danielski

Karnesis

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The Laser Interferometer Space Antenna (LISA) will detect and characterize ∼104 Galactic Binaries consisting predominantly of two White Dwarfs (WD). An interesting prospect within this population is a third object–another WD star, a Circumbinary Exoplanet (CBP), or a Brown Dwarf (BD)–in orbit about the inner WD pair. We present the first fully Bayesian detection and posterior analysis of sub-stellar objects with LISA, focusing on the characterization of CBPs. We used an optimistic astrophysically motivated catalogue of these CBP third-body sources, including their orbital eccentricity around the inner binary for the first time. We examined Bayesian Evidence computations for detectability, as well as the effects on the posterior distributions for both the inner binary parameters and the third-body parameters. We find that the posterior behavior bifurcates based on whether the third-body period is above or below half the observation time. Additionally, we find that undetectable third-body sources can bias the inner binary parameters whether or not the correct template is used. We used the information retrieved from the study of the CBP population to make an initial conservative prediction for the number of detectable BD systems in the original catalogue. We end with commentary on the predicted qualitative effects on LISA global fitting and Galactic Binary population analysis. The procedure used in this work is generic and can be directly applied to other astrophysical effects expected within the Galactic Binary population.

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confidence: 79%

Bayesian characterization of circumbinary sub-stellar objects with LISA

Katz

Danielski

Karnesis

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…Borkovits et al (2013) measured eclipse timing variations (ETVs) of close binary HD 181068 from the Kepler observations to prove the cyclic variation of O-C curve result from the gravitational perturbations of the third body. Meanwhile, as discussed in some binaries, e.g., IK Per (Zhu et al 2005), AD Cnc (Qian et al 2007b), RZ Com (Qian & He 2005), DD Com (Zhu et al 2010), GSC 03526-01995 (Liao et al 2012), and XY LMi (Qian et al 2011b), their light curves in different seasons indicate that there are stellar dark spots on the surface of at least one component. The Kepler Space Telescope provides a good chance to understand the third body, magnetic activity of close binaries in unbroken time.…”

Section: Introductionmentioning

confidence: 88%

Is There a Substellar Object Orbiting the Solar-like Stable Contact Binary V2284 Cyg?

Wang

Jiang

Zhang

et al. 2017

PASP

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V2284 Cyg is a neglected W UMa-type binary star for photometric investigations. Monitored by the Kepler Space Telescope from 2009 to 2013, its light curves are continuously stable, suggesting that both components are inactive during this time interval. Based on the short-cadence observations, we determined the photometric solutions by using the 2013 version of the Wilson-Devinney code. These parameters reveal that V2284 Cyg is a W-type system with a degree of contact factor of f=39.23% and a mass ratio of q=2.90. Meanwhile, hundreds of times of minimum light were obtained and applied to analyze the orbital period changes. In the O-C diagram, a smallamplitude cyclic oscillation (A 3 =0.00030 days and T 3 =2.06 years) superimposed on a secular decreasing was found. The continuous decreasing may be a result from the mass transfer from the more massive component to the less massive one. With the long-term decreasing of the orbital period, this binary will evolve into a deeper contact system. Because the light curve is stable, the cyclic variation is plausibly explained as the light-travel time effect (LTTE) due to the presence of an additional body. The mass of the companion is. If the orbital plane inclination is a random distribution, it is a brown dwarf with 66.7% probability. Therefore, the companion of V2284 Cyg is possibly the first candidate of the brown dwarf orbiting around contact binary, where both component are sharing a common convective envelope.

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“…Since AH Tauri is a G-type binary, both component stars have a deep convective envelope along with rapid rotation. It is expected that stellar dark spots should be observed on photospheres of this kind of binary stars (e.g., Qian et al 2007Qian et al , 2011Qian et al , 2014Zhu et al 2010;Liu et al 2011a). Tables 5 and 6 -are shown in the bottom panel of Figure 3.…”

Section: Photometric Studymentioning

confidence: 97%

CCD Photometric Study and Period Investigation of Ah Tauri

Xiang¹,

Xiao²,

Yu³

2015

The Astronomical Journal

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In this paper, we present new CCD photometric observations of AH Tauri in the R band observed in 2006 at the Yunnan Observatory. Two new times of light minima were derived from these observations. We modeled the light curves using the 2003 version of the Wilson-Devinney program. The results show that the variations of the light curves can be expained by a cool spot on the primary star. The fill-out factor is about 6.6%, indicating that AH Tauri is a shallow-contact system. The mass ratio was determined to be about 0.505. In addition, the orbital period variations of AH Tauri were investigated based on all of the photoelectric and CCD light minimum times, including our two new data. It was found that the orbital period exhibits a possible periodic variation with a period of P 54.62 ( 0.20) mod =  years and a secular period decrease of dP dt (1.823 0.215) 10 days yr 7 1= -´--. Since AH Tauri is an overcontact solar-like system, we discuss three mechanisms of the mass transfer, the lighttime effect of the third body, and magnetic activity responsible for the orbital period changes.

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High Fill-Out, Extreme Mass Ratio Overcontact Binary Systems. X. The Newly Discovered Binary Xy Leonis Minoris

Cited by 34 publications

References 31 publications

Bayesian characterization of circumbinary sub-stellar objects with LISA

Bayesian characterization of circumbinary sub-stellar objects with LISA

Is There a Substellar Object Orbiting the Solar-like Stable Contact Binary V2284 Cyg?

CCD Photometric Study and Period Investigation of Ah Tauri

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