Minima Times of Three Selected Systems in Cancer

Gökay, G.; Derman, Emanuel; Güral, B.

doi:10.22444/ibvs.6206

Cited by 2 publications

(2 citation statements)

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“…As mentioned earlier, KW Psc was not observed in any of the surveys except ASAS. From previous studies (Gokay et al 2010;Diethelm 2010Diethelm , 2011Diethelm , 2012Diethelm , 2013, 23 TOMs were collected for KW Psc. From these values, the updated linear ephemeris is estimated as: In present analysis, differential corrections minimization algorithm was used.…”

Section: Kw Pscmentioning

confidence: 99%

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Photometric and Spectroscopic analysis of four contact binaries

Panchal,

Joshi

2021

Preprint

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We present the photometric and spectroscopic analysis of four W UMa binaries J015829.5+260333 (hereinafter as J0158), J030505.1+293443 (hereinafter as J0305), J102211.7+310022 (hereinafter as J1022) and KW Psc. The V R c I c band photometric observations are carried out with the 1.3-m Devasthal Fast Optical Telescope (DFOT). For low resolution spectroscopy, we used 2-m Himalayan Chandra Telescope (HCT) as well as the archival data from 4-m LAMOST survey. The systems J0158 and J0305 show a period increase rate of 5.26(±1.72) × 10 −7 days yr −1 and 1.78(±1.52) × 10 −6 days yr −1 , respectively. The period of J1022 is found to be decreasing with a rate of 4.22(±1.67) × 10 −6 days yr −1 . The period analysis of KW Psc displays no change in its period. PHOEBE package is used for the light curve modeling and basic parameters are evaluated with the help of GAIA parallax. The asymmetry of light curves is explained with the assumption of cool spots at specific positions on one of the components of the system. On the basis of temperatures, mass ratios, fill-out factors and periods, the system J1022 is identified as W-subtype systems while the others show some mixed properties. To probe the chromospheric activities in these W UMa binaries, their spectra are compared with the known inactive stars spectra. The comparison shows emission in H α , H β and Ca II.To understand the evolutionary status of these systems, the components are plotted in mass-radius and mass-luminosity planes with other well characterized binary systems. The secondary components of all the systems are away from ZAMS which indicates that secondary is more evolved than the primary component.

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Section: Kw Pscmentioning

confidence: 99%

“…Here [1],[2] and [3] show TOMs estimated by SuperWASP,Gokay et al (2010) andDiethelm (2010). This is only sample table.…”

mentioning

confidence: 99%