Orbital Period Variation Study of the Algol Eclipsing Binary Di Pegasi

Hanna, Magdy A.; Amin, S. M.

doi:10.5303/jkas.2013.46.4.151

Cited by 6 publications

(3 citation statements)

References 18 publications

(2 reference statements)

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“…Therefore, we choose weights 1, 3 and 10 for the whole group of observations obtained by vis, pg and PE or CCD techniques, respectively. This weighting method has been implemented by many authors (e.g., Zasche et al 2008;Hanna & Amin 2013;Ulas et al 2020).…”

Section: Period Studymentioning

confidence: 99%

Light Curve Analysis and Period Study of Two Eclipsing Binaries UZ Lyr and BR Cyg

Roobiat¹,

Pazhouhesh²

2022

Res. Astron. Astrophys.

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Two eclipsing binary systems UZ Lyr and BR Cyg are the semi-detached types whose secondary component fill its Roche lobe. Although radial velocity and light curves of these systems have already been investigated separately, both radial velocity and light curves of them are analyzed simultaneously for the first time in the present study . Also, the orbital period changes of these systems are studied. Our results show that the mass transfer between components have negligible effects on the orbital period changes of these systems, but two light-time effects are the reasons of the periodic behavior of the O-C curve for UZ Lyr. We could not remark more information about orbital period changes for BR Cyg, but we find a new orbital period for it. By radial velocity and light curves analysis we find a clod spot on the secondary components of BR Cyg. The new geometrical and physical parameters of both systems are obtained and their positions on H-R diagram demonstrated.

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Section: Period Studymentioning

confidence: 99%

Light Curve Analysis and Period Study of Two Eclipsing Binaries UZ Lyr and BR Cyg

Roobiat¹,

Pazhouhesh²

2022

Res. Astron. Astrophys.

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“…These weights were 1, 3 and 10 for visual data, photographic data and photoelectric/CCD data, respectively. This method of weighting the observational data is also common in the literature; for example, seeZasche et al (2008),Hanna & Amin (2013),Ulas et al (2020). Moreover, the linear ephemeris given in Equation (1) was used to calculate the epoch and O − C. In Figure…”

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confidence: 99%

Detection of Pulsation and Additional Components in Eclipsing Binary RS Sct

Abedi,

Roobiat

2023

Res. Astron. Astrophys.

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The eclipsing binary star RS Sct is a semi-detached system of the β Lyrae type. This system was photometered for six nights in 2019 August, and 2020 June and August. The light and radial velocity curves were simultaneously analyzed to obtain the absolute physical and orbital parameters of the system, and the system geometry was determined. In this system, the primary component has filled its inner Roche lobe and the secondary component is close to filling it. Moreover, the change in the orbital period of this system was investigated. The presence of the third or fourth components and the mass transfer between the two components affect the orbital period of the system. In addition, the pulsation of the primary component was detected. Also, several frequencies with high signal-to-noise ratios were identified. According to the position of the primary component in the H-R diagram and the value of the obtained frequencies, this component is likely a delta-Scuti pulsator.

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“…Many semi-detached Algol binary systems exhibit either long-term parabolic increase or decrease in their orbital periods during their evolution depending on whether the process of matter transfer is conservative or non-conservative; for examples see Hanna & Amin (2013). However, in case of binaries that show orbital period decrease many authors, e.g., Kreiner et al (1994b) and Pribulla (1998) have attributed such orbital period decrease to non-conservative mass loss from the primary component.…”

Section: Mass Lossmentioning

confidence: 99%

Period Variation Study of the Neglected Algol Eclipsing Binary System V346 Cygnius

Hanna¹

2014

Journal of The Korean Astronomical Society

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Abstract:We present the first period variation study for the Algol eclipsing binary V346 Cyg by constructing the (O − C) residual diagram using all the available precise minima times. We conclude that the period variation can be explained by a sine-like variation due to the presence of a third body orbiting the binary in about 68.89 ± 4.69 years, together with a long-term orbital period decrease (dP/dt = −1.23 × 10 −7 day/yr) that can be interpreted to be due to slow mass loss from the δ-Scuti primary component. The sinusoidal variation may also be explained by using the the Applegate (1992) mechanism involving cyclic magnetic activity due to star-spots on the secondary component. The present preliminary solution needs more precise photometric observations to be confirmed.

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Orbital Period Variation Study of the Algol Eclipsing Binary Di Pegasi

Cited by 6 publications

References 18 publications

Light Curve Analysis and Period Study of Two Eclipsing Binaries UZ Lyr and BR Cyg

Light Curve Analysis and Period Study of Two Eclipsing Binaries UZ Lyr and BR Cyg

Detection of Pulsation and Additional Components in Eclipsing Binary RS Sct

Period Variation Study of the Neglected Algol Eclipsing Binary System V346 Cygnius

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