Absolute Properties of the Binary System BB Pegasi

Kalomeni, B.; Yakut, K.; Keskin, V.; Değirmenci, Ö. L.; Ulaş, B.; Kose, O.

doi:10.1086/519493

Cited by 37 publications

(18 citation statements)

References 23 publications

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“…In Figure 6, we show the geometrical configurations of the binary star at phases 0.25, 0.50, 0.75 and 1.0. From the photometric light curves, we have not seen any O'Connell effect in the binary star which, in general, is linked with the existence of cool spots on any component of the binary system (Kalomeni et al, 2007).…”

Section: Geometric Solutionsmentioning

confidence: 67%

Long-term photometric study of a faint W UMa binary in the direction of M31

Joshi

Rukmini

2017

Res. Astron. Astrophys.

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We carry out a re-analysis of the photometric data in R c I c bands which was taken under the Nainital Microlensing Survey during 1998 to 2002 with the aim to detect gravitational microlensing events in the direction of M31. Here, we do photometric analysis of a faint W UMa binary CSS J004259.3 + 410629 identified in the target field. The orbital period of this star is found to be 0.266402±0.000018 day. The photometric mass ratio, q, is found to be 0.28 ± 0.01. The photometric light curves are investigated using the Wilson-Devinney (WD) code and absolute parameters are determined using empirical relations which provide masses and radii of the binary as M 1 = 1.19 ± 0.09M ⊙ , M 2 = 0.33 ± 0.02M ⊙ and R 1 = 1.02 ± 0.04R ⊙ , R 2 = 0.58 ± 0.08R ⊙ based on the R c band data. Almost similar values are found by analysing I c band data. From the photometric light curve examination, the star is understood to be a low mass-ratio overcontact binary of A-subtype with a high fill-out factor of about 47%. The binary system is found to be located approximately at a distance of 2.64 ± 0.03 kpc having a separation of 2.01 ± 0.05 R ⊙ between the two components.

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Section: Geometric Solutionsmentioning

confidence: 67%

Long-term photometric study of a faint W UMa binary in the direction of M31

Joshi

Rukmini

2017

Res. Astron. Astrophys.

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“…There is no evidence of emission at the H α , H β , and H γ lines, which indicate that V1101 Her does not have obvious chromospheric activity. The period increase and physical models of V1101 Her are similar to LY And (Lu et al 2017), BB Peg (Kalomeni et al 2007;Lu & Rucinski 1999), DD Indus (Samec et al 2016), DD Com (Zhu et al 2010), and V453 Mon (Köse et al 2009). …”

Section: Absolute Geometrical and Starspot Parametersmentioning

confidence: 72%

Magnetic Activity and Period Variation Studies of the Short-period Eclipsing Binaries. II. V1101 Her, AD Phe, and NSV 455 (J011636.15–394955.7)

Zhang

et al. 2017

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In this paper, we present new BVRI light curves of short-period contact eclipsing binaries V1101 Her and AD Phe from our observations carried out from 2014 to 2015 using the SARA KP and SARA CT telescopes. There is an eclipsing binary located at α(2000)=01 h 16 m 36 15 and δ(2000)=−39°49′55 7 in the field of view of AD Phe. We derived an updated ephemeris and found there a cyclic variation overlaying a continuous period increase (V1101 Her) and decrease (AD Phe). This kind of cyclic variation may be attributed to the light time effect via the presence of the third body or magnetic activity cycle. The orbital period increase suggests that V1101 Her is undergoing a mass-transfer from the primary to the secondary component (dM 1 /dt=2.64(±0.11)×10−6 M e yr −1) with the third body (P 3 =13.9(±1.9) years), or 2.81(±0.07)×10−6 M e yr −1 for an increase andmagnetic cycle (12.4(±0.5) years). The long-term period decrease suggests that AD Phe is undergoing a mass-transfer from the secondary component to the primary component at a rate of −8.04(±0.09)×10 −8 M e yr −1 for a period decrease and the third body (P 3 =56.2(±0.8) years), or −7.11(±0.04)×10 −8 M e yr −1 for a decrease and magnetic cycle (50.3(±0.5) years). We determined their orbital and geometrical parameters. For AD Phe, we simultaneously analyzed our BVRI light curves and the spectroscopic observations obtained by Duerbeck & Rucinski. The spectral type of V1101 Her was classified as G0±2V by LAMOST stellar spectra survey. The asymmetry of the R-band light curve of AD Phe obtained by McFarlane & Hilditch in 1987 is explained by a cool spot on the primary component.

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“…This time is quite long to see any variation in the (O-C) diagram. However, it is apparent from Figure 5(a) that the upward parabola is not so clear as seen in binaries with nondegenerate components (e.g., Kalomeni et al 2007). If the period variation is due to the conservative mass transfer, the mass transfer rate between the components isṀ = 7.6 × 10 −9 M yr −1 .…”

Section: Resultsmentioning

confidence: 92%

VARIATION OF THE LIGHT AND PERIOD OF THE MAGNETIC CATACLYSMIC VARIABLE AM Her

Kalomeni

Yakut

2008

The Astronomical Journal

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Ground-based, long-term optic variability of AM Her, covering the period between 2003-2008, has been conducted to study the features seen in both low and high states of the system. Low-state analysis shows the presence of short-term, low-amplitude light variations of about 0.02-0.03 mag with a mean power time between 16 s and 226 s. Brightness variations on the order of 0.7-2 mag, which could be due to the stellar activity of the component in the system, are also detected. A total of 30 years' times of minimum light given in the literature are combined with nine times of minima obtained in this study. We represented the (observed-calculated) diagram by a parabolic curve and also by two broken lines. Under the assumption of a parabolic variation, we estimate an increase in period, dP dt = 7.5(1.2) × 10 −9 days yr −1 , with a mass transfer rate ofṀ = 8(2) × 10 −9 M yr −1 , in agreement with the previous findings by a different method.

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Absolute Properties of the Binary System BB Pegasi

Cited by 37 publications

References 23 publications

Long-term photometric study of a faint W UMa binary in the direction of M31

Long-term photometric study of a faint W UMa binary in the direction of M31

Magnetic Activity and Period Variation Studies of the Short-period Eclipsing Binaries. II. V1101 Her, AD Phe, and NSV 455 (J011636.15–394955.7)

VARIATION OF THE LIGHT AND PERIOD OF THE MAGNETIC CATACLYSMIC VARIABLE AM Her

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