Photometric and spectroscopic analysis of YY CrB

Essam, A.; Saad, S. M.; Nouh, M. I.; Dumitrescu, Alexandru; Elkhateeb, M. M.; Haroon, A. A.

doi:10.1016/j.newast.2009.07.006

Cited by 15 publications

(10 citation statements)

References 13 publications

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“…The stars seem not to be coeval to each other. However, it is well known that there are several binaries such as YY CrB (Essam et al 2010), BS Cas (Yang, Wei, & He 2008), VZ Tri (Yang 2010). All these samples exhibit the same behaviour.…”

Section: Dal and Sipahimentioning

confidence: 99%

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

Dal

Sipahi

2013

Publ. Astron. Soc. Aust.

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Taking into account the results obtained from the models and analyses of the BVRI light curves, we discuss the nature of V1464 Aql. The analyses indicated that the mass ratio of the system is q = 0.71 ± 0.02, while the inclination of the system (i) is 38°.45 ± 0°.22. Taking the primary component's temperature as 7 420 ± 192 K, we found that the temperature of the secondary is 6 232 ± 161 K. The mass of the primary component was found to be 1.74 ± 0.05 M ࣻ , while it is 1.23 ± 0.01 M ࣻ for the secondary. The primary component's radius was found to be 2.10 ± 0.05 R ࣻ , while it was found as 1.80 ± 0.01 R ࣻ for the secondary. Revealing that the system should not exhibit any eclipses, we demonstrated that the main variation with large amplitude should be caused due to the ellipsoidal effect. Indeed, the Fourier analysis also supported the result. For the first time in the literature, we revealed that the primary component is a δ Scuti star. The period of pulsation was found to be 58.482 ± 0.002, 58.482 ± 0.001, 60.966 ± 0.002, and 60.964 ± 0.003 min in BVRI bands, respectively. We plotted V1464 Aql in the log(P orb )-log (P pulse ) plane. Using more than 160 binaries, whose one or both components are pulsating, we derived a new linear fit in the log (P orb )-log (P pulse ) plane for each type of binary. Using the linear fit of each group, we obtained new calibrations between log (P orb ) and log (P pulse ) for different types of pulsating stars. In addition, a calibration has been obtained for the first time for the pulsating stars with spectral types O and B. V1464 Aql seems to be located near the other ellipsoidal and close binaries. Thus, we listed V1464 Aql as a new candidate for the ellipsoidal variables with a δ Scuti component.

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Section: Dal and Sipahimentioning

confidence: 99%

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

Dal

Sipahi

2013

Publ. Astron. Soc. Aust.

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“…We adjusted the orbital period as 0 d .318666. It is well known that several binaries of W UMa type such as YY CrB (Essam et al, 2010), BS Cas (Yang et al, 2008), VZ Tri (Yang, 2010), exhibit large the period variation due to the large mass transfer.…”

Section: Discussionmentioning

confidence: 99%

“…In the literature, there are several systems similar to HH Boo (Essam et al, 2010). In this study, we obtained multi-colour light curves.…”

Section: Introductionmentioning

confidence: 99%

Absolute properties of the overcontact binary HH Boo

Dal

Sipahi

2013

New Astronomy

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“…Yu, Xiang, & Xiao (2015) studied the orbital period changes and implied that the decreased period rate and concluded that the sinusoidal oscillatory can be interrupted as magnetic activity. Essam et al (2010) and Yu, Xiang, & Xiao (2015) on the rate of period decrease demonstrate that the value of reduced rate is lowering progressively, indicating that this system was going through an orbital expansion stage of thermal relaxation oscillation (TRO) cycles. Also, understanding the evolutionary status of this target could prove invaluable.…”

mentioning

confidence: 97%

“…Gazeas et al (2005) analyzed the light curve and derived the geometric and photometric parameters and concluded that this target is a contact binary with weak magnetic activity. Essam et al (2010) combined photometric and spectroscopic solutions and calculated the fill-out factor approximately equal to 64 percent and mass ratio of 0.241. In addition, they studied the changes in the orbital period using the O-C diagram and concluded that the orbital period is decreasing.…”

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confidence: 99%