Photometric study of eclipsing binaries in the Large Magellanic Cloud — I. W UMa type binaries in the Large Magellanic Cloud

Devarapalli, Shanti Priya; Sriram, K.; Rao, P. Vivekananda

doi:10.1088/1674-4527/11/2/005

Cited by 7 publications

(4 citation statements)

References 20 publications

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“…Throughout the study, mass ratio is defined as q = M c /M h , where M c is mass of the cooler component and M h is mass of the hotter component. As no mass ratio was determined for V2840 Cygni in previous literature, a q-search was conducted to obtain the value of "q" (Rukmini et al 2001;Priya et al 2011Priya et al , 2013Priya et al , 2020. The adjustable parameters were iterated for a range of "q" values varying in the range from 0.1 to higher values in steps of 0.1, using the differential correction (DC) routine until a minimum residual was obtained at q = 1.3.…”

Section: Light Curve Analysismentioning

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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Section: Light Curve Analysismentioning

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 fitting of the light curve was done using mode 2 of the WD code since neither of the stars is in contact with its Roche lobe. The photometric parameters were set as either fixed or adjustable as per convention generally followed while using WD code (Priya et al 2011;Schaffenroth et al 2013). The effective temperature (T 1 ) of the primary component (sdB star) was adopted from Kawka et al (2010) and fixed at 27,990 K. The gravitydarkening coefficients g 1 , g 2 were fixed to 1 (Von Zeipel 1924) and 0.32 (Lucy 1967), respectively.…”

Section: Photometrymentioning

confidence: 99%

Probing TYC 3315-1807-1, An sdB+dM Binary Displaying Strong Period Variation and Reflection Effect

Devarapalli

Rukmini

Gundeboina

et al. 2022

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Subdwarf (sdB) stars include core helium-burning stars with a very thin hydrogen envelope that lies at the blue end of the horizontal branch (or extreme horizontal branch). Among them, short-period sdB binaries especially with cool companions are significant to test and constrain binary evolution. We discuss one such sdB+dM type binary, TYC 3315-1807-1 (V1), which was first reported by Kawka. Results of the photometric analysis on Transiting Exoplanet Survey Satellite data are being reported. Light variation in the light curve suggests that the system displays a large reflection effect with no eclipses. Spectroscopic observations of the object were also carried out to probe into the nature of secondary companion as well as to understand the post-common-envelope evolution of such objects. The variability in Balmer, He, and Na line profiles as a function of phase, probably caused by observed reflection effect was identified and studied. Period variation study of the object was done using times of minima obtained from the literature and the O − C plot was produced, which points to a decrease in the period (dp/dt = −1.36315 × 10−7 day yr−1), and the possible scenario of evolution is discussed. From the evolutionary models, we constrain the possible mass of the sdB to be 0.274 M ⊙ and that of the secondary is 0.113 M ⊙, and we conclude that V1 may evolve directly as a helium-core white dwarf.

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“…For all systems in this study, these parameters were fitted until a minimum weighted square deviation of W (O − C) 2 spanned over a selected range of 'q'. We applied the qsearch method to determine the value of 'q' (Priya et al 2011(Priya et al , 2013Rukmini et al 2001). After that, we executed differential correction (DC) until we obtained a minimum , and checked the fitted parameters for the presence of third light by freeing the L 3 parameter for all the systems in this study.…”

Section: Photometric Analysismentioning

confidence: 99%

Photometric investigation of eight ultra-short period eclipsing binaries from OGLE

Devarapalli

Raja

Rukmini

et al. 2020

Res. Astron. Astrophys.

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We performed a detailed photometric analysis of eight ultra-short period eclipsing binaries (USPEBs) using the Wilson-Devinney method. We present the modeled light curves and derived photometric solutions. The USPEBs with period (P)≤0.21 d considered in our study belong to W-subtype having shallow contact factor (f) <∼20%, high mass ratio (q) >∼0.7 and later spectral types. The absolute parameters for these short-period binaries were derived applying empirical relations. We discuss the evolutionary stage of these USPEBs using the mass-radius, color-density and period-color diagrams. The objects showed poor metallicities, and some objects were even found to be existing around fully convective limits. The period distribution of USPEBs exhibited a sharp cut-off at 0.22 d; however, we observed significant deficits for our objects in the literature. We examined the statistics of USPEBs studied to date (in terms of the distribution of period, mass ratio and component temperatures of USPEBs) and observed that a dominant distribution of component temperatures for these USPEBs was towards lower temperatures.

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Photometric study of eclipsing binaries in the Large Magellanic Cloud — I. W UMa type binaries in the Large Magellanic Cloud

Abstract: Eclipsing binaries are among the most important sources of information on stellar parameters like radii, masses, luminosities, etc. We present the analysis of six W UMa systems discovered in the Large Magellanic Cloud using the Wilson-Devinney method.

Cited by 7 publications

References 20 publications

The First Photometric and Spectroscopic Study of Contact Binary V2840 Cygni

The First Photometric and Spectroscopic Study of Contact Binary V2840 Cygni

Probing TYC 3315-1807-1, An sdB+dM Binary Displaying Strong Period Variation and Reflection Effect

Photometric investigation of eight ultra-short period eclipsing binaries from OGLE

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