Two almost-contact semidetached systems - ZZ Aurigae and AX Virginis

Leung, K. C.; Zhai, D. S.; Liu, Q.; Yang, Yisi

doi:10.1086/113717

Cited by 6 publications

(6 citation statements)

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“…The systems of this group seem to be contact or semidetached or even marginally detached (Lazaro et al 1995). It is for this reason that several authors (Leung et al 1985; Barone et al 1991; Terrell et al 1992) report different Roche configurations for ZZ Aur.…”

Section: Light‐curve Analysismentioning

confidence: 96%

“…The bolometric albedos were set to A 1 = 1.0 and A 2 = 0.5. Other initial parameters were taken from the results of Leung et al (1985).…”

Section: Light‐curve Analysismentioning

confidence: 99%

“…Therefore, the model of the cool spot on the cooler star is the preferred choice for ZZ Aur. The photometric parameters of the spot model are listed with the previous results of Leung et al (1985) and Barone et al (1991) in Table 6.…”

Section: Light‐curve Analysismentioning

confidence: 99%

“…Koch et al (1979) included ZZ Aur in their list of photoelectrically neglected eclipsing binaries. Its more detailed history until 1985 has been described by Leung et al (1985).…”

Section: Introductionmentioning

confidence: 99%

“…In their solution, the hot star of ZZ Aur very nearly fills its Roche lobe, and the primary minimum is a partial transit. To find a more reliable solution, Leung et al (1985) reanalysed the BV light curves with the Wilson–Devinney method and came to a semidetached configuration for which the cool component exactly fills its Roche lobe while the hot primary nearly fills its lobe. Later, Barone et al (1991) reanalysed the same light curves and Terrell, Mukherjee & Wilson (1992) included the light curves of ZZ Aur in their Pictorial Atlas.…”

Section: Introductionmentioning

confidence: 99%

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BVR observations and period variation of the near-contact binary ZZ Aurigae

Kim

Lee

et al. 2006

Monthly Notices of the Royal Astronomical Society

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BVR light curves of ZZ Aurigae were obtained with the 60‐cm Cassegrain reflector at the Sobaek Observatory, Korea, between 2000 February and 2001 February. All collected times of minimum light, including our observations, were used for the period study. The period variation could be of quasi‐sinusoidal form superposed on an upward parabola. A continuous period increase of dP/dt=+2.3 × 10−8 d yr−1 was determined for ZZ Aur. The period of quasi‐sinusoidal variation is about ∼26–31 yr. Photometric solutions were found using the Wilson–Devinney method. The Roche configuration of ZZ Aur is that of an Algol‐type semidetached system where the primary star nearly fills its Roche lobe and the secondary star fills its lobe. The spot model was used to explain the asymmetry in the light curve known as the O'Connell effect.

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Section: Light‐curve Analysismentioning

confidence: 96%

“…The bolometric albedos were set to A 1 = 1.0 and A 2 = 0.5. Other initial parameters were taken from the results of Leung et al (1985).…”

Section: Light‐curve Analysismentioning

confidence: 99%

Section: Light‐curve Analysismentioning

confidence: 99%

“…Koch et al (1979) included ZZ Aur in their list of photoelectrically neglected eclipsing binaries. Its more detailed history until 1985 has been described by Leung et al (1985).…”

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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