Photometric and Spectroscopic Analysis of Four Contact Binaries

Panchal, Alaxender; Joshi, Y. C.

doi:10.3847/1538-3881/abea0c

Cited by 15 publications

(13 citation statements)

References 44 publications

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“…(2) The light variability of KW Psc (=ASAS J225832 +0552.4) was noticed as an EW-type binary by Zickgraf et al (2003), who determined its orbital period of 0.234276 days. Panchal & Joshi (2021) observed this binary on 2018 October 11, 12, and 20, November 26, December 1 and 27, and 2019 October 12. For the discontinuous observations, they derived the photometric solution with a mass ratio of q = 0.42 ± 0.01.…”

Section: Introductionmentioning

confidence: 89%

“…We obtained two sets of new LCs, i.e., LC 2000 and LC 2021 for V0576 Peg and KW Psc, respectively. Panchal & Joshi (2021) For FY Boo, Samec et al (2009) published BVRI LCs that we designate as LC 2009 . For this star, we also use LC 2020 from the TESS database.…”

Section: Observations and Data Reductionsmentioning

confidence: 99%

“…When modeling the LCs, q = 0.42 (Panchal & Joshi 2021) is adopted to be an initial input parameter. We obtained two sets of spotted solutions from the BV LCs of LC 2020 and LC 2021 , which are listed in Table 9.…”

Section: Kw Pscmentioning

confidence: 99%

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Magnetic Activity on Four Short-period Contact Binaries: V0576 Peg, KW Psc, V0873 Per, and FY Boo

Yang¹,

Yuan²,

Wang³

et al. 2022

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We presented new photometry for four short-period late-type binaries, observed by three small telescopes in China from 2020 September to 2021 December. Seven sets of light curves (including the TESS data for FY Boo) were analyzed by using the W-D method. Three binaries (V0576 Peg, V0873 Per, and FY Boo) are W-type binaries with q ≃ 2.5, while KW Psc is an A-type binary with q ≃ 0.43. Max.I−Max.II is up to 10% of variable light amplitude for the asymmetric light curves, which are modeled by a dark spot on the surface of the more massive component. Photometric results imply the existence of movement and evolution of the cool spot. From the temperature−luminosity and mass–luminosity diagrams, the more massive components are a bit evolved main-sequence stars, while the less massive ones are oversized and overluminous owing to energy exchange. Orbital period analyses indicate that the cyclic oscillations occur in the (O − C) curves. Their modulated periods approach 11 yr, which may preferably result from the magnetic activity cycle for four late-type contact binaries. With angular momentum loss through magnetic braking, these short-period contact binaries may evolve into deep-contact configurations.

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Section: Introductionmentioning

confidence: 89%

Section: Observations and Data Reductionsmentioning

confidence: 99%

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Magnetic Activity on Four Short-period Contact Binaries: V0576 Peg, KW Psc, V0873 Per, and FY Boo

Yang¹,

Yuan²,

Wang³

et al. 2022

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“…According to Kepler's third law (Panchal & Joshi 2021), the total mass of the system (M 1 + M 2 ), in terms of M ⊙ , is acquired from relation 8. The separation a is the average value of a 1 and a 2 calculated for each component individually by their radius (R) and the mean fractional radius (r) using relation 7.…”

Section: Calculation Of the Absolute Parametersmentioning

confidence: 99%

Investigation of the Orbital Period and Mass Relations for W UMa-type Contact Systems

Poro,

Sarabi,

Zamanpour

et al. 2021

Preprint

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New relationships between the orbital period and some parameters of W Ursae Majoris (W UMa) type systems are presented in this study. To investigate the relationships, we calculated the absolute parameters of a sample of 118 systems. For this purpose, we used the parallax values obtained from the Gaia Early Data Release 3 (Gaia EDR3) star catalog for more precise calculations. The other required parameters, including the light curve solutions and the orbital period were derived from previous research. For some relationships, we added 86 systems from another study with an orbital period of less than 0.6 days to our sample, allowing

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“…The primary and secondary masses were determined using q. The detailed procedure and equations involved in the parameter determination can be seen in Liu et al (2020) and Panchal & Joshi (2021). The physical parameters for all the systems are given in Table 7.…”

Section: )mentioning

confidence: 99%

Long-term photometric and low-resolution spectroscopic analysis of five contact binaries

Panchal,

Joshi,

De Cat

et al. 2021

Preprint

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A photometric and spectroscopic investigation is performed on five W Ursae Majoris eclipsing binaries (EWs) J015818.6+260247 (hereinafter as J0158b), J073248.4+405538 (hereinafter as J0732), J101330.8+494846 (hereinafter as J1013), J132439.8+130747 (hereinafter as J1324) and J152450.7+245943 (hereinafter as J1524). The photometric data are collected with the help of the 1.3 m Devasthal Fast Optical Telescope (DFOT), the 1.04 m Sampurnanand Telescope (ST) and the TESS space mission. The low-resolution spectra of the 4 m Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) are used for spectroscopic analysis. The orbital period change of these systems is determined using our and previously available photometric data from different surveys. The orbital period of J1013 and J1524 is changing with a rate of −2.552(±0.249) × 10 −7 days yr −1 and −6.792(±0.952) × 10 −8 days yr −1 , respectively, while others do not show any orbital period change. The orbital period change of J1013 and J1524 corresponds to a mass transfer rate of 2.199 × 10 −7 M yr −1 and 6.151 × 10 −8 M yr −1 from the primary to the secondary component in these systems. It is likely that angular momentum loss via magnetic braking may also be responsible for the observed orbital period change in the case of J1524. All systems have a mass-ratio lower than 0.5, except J0158b with a mass-ratio of 0.71. All the systems are shallow type contact binaries. The J0158b and J1524 are A-subtype while others are W-subtype. The H α emission line region is compared with template spectra prepared using two inactive stars with the help of STARMOD program. The J0158, J1324 and J1524 systems show excess emission in the residual spectra after subtraction of the template.

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Photometric and Spectroscopic Analysis of Four Contact Binaries

Cited by 15 publications

References 44 publications

Magnetic Activity on Four Short-period Contact Binaries: V0576 Peg, KW Psc, V0873 Per, and FY Boo

Magnetic Activity on Four Short-period Contact Binaries: V0576 Peg, KW Psc, V0873 Per, and FY Boo

Investigation of the Orbital Period and Mass Relations for W UMa-type Contact Systems

Long-term photometric and low-resolution spectroscopic analysis of five contact binaries

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