2006
DOI: 10.1071/as06016
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Abstract: New photoelectric BV light curves of three close eclipsing binaries XY Leo, EE Cet and AQ Psc were observed and studied with the aim to derive the physical parameters of these systems. The following results were obtained: (a) the W-type contact binary system XY Leo is in a marginal overcontact configuration ( f over * 2.4%) with a relatively large temperature difference between the components (*330 K); (b) due to the proximity of the companion of EE Cet in the visual binary ADS 2163, the light curves of EE Cet… Show more

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Cited by 21 publications
(5 citation statements)
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“…The mass function f ( M ) in all the three cases is quite similar. However, the absolute parameters determined using the ASAS light curve are different from those of Djurašević et al (2006). This disagreement might be caused because of slightly noisy ASAS data and/or estimation of different values of third light contribution in the two analyses.…”
Section: Results and Comparison With The Literaturementioning
confidence: 93%
See 1 more Smart Citation
“…The mass function f ( M ) in all the three cases is quite similar. However, the absolute parameters determined using the ASAS light curve are different from those of Djurašević et al (2006). This disagreement might be caused because of slightly noisy ASAS data and/or estimation of different values of third light contribution in the two analyses.…”
Section: Results and Comparison With The Literaturementioning
confidence: 93%
“…They assigned a spectral class F8V to the system and classified it as a W‐type W UMa binary with a mass ratio q sp = 0.315(5). A photometric study of this star was carried out by Djurašević et al (2006) using q = 0.315, who obtained the parameters as listed in Table 7. They obtained i (°) = 78.5 ± 0.2, M 1 + M 2 = 1.80 M ⊙ , L 3 ∼ 0.54 and mass function f ( M ) = 1.694 M ⊙ .…”
Section: Results and Comparison With The Literaturementioning
confidence: 99%
“…From the early years of its discovery, XY Leo was known to be bright in X‐rays (Cruddace & Dupree 1984) and radio waves, being chromospherically active and prominent by its UV and Mg ii emission (Rucinski 1985; Vilhu & Rucinski 1985; Vilhu, Caillault & Heise 1987, 1988). Extensive studies of the period changes and the light time effect (LITE) were done by Gehlich, Prolss & Wehmeyer (1972) and followed by Kaluzny & Pojmanski (1983), Hrivnak et al (1983), Hrivnak (1985), Pan & Cao (1998), Yakut et al (2003), Pribulla & Rucinski (2006) and Djuraŝeviĉ et al (2006). Struve & Zebergs (1959) obtained the first spectroscopic orbit for the contact binary and noticed a strong Ca ii emission, which was considered to originate on the surface of the more massive component.…”
Section: Introductionmentioning
confidence: 99%
“…Karami & Mohebi (2007) using their own velocity curve analysis method, arrived at almost identical results for the mass ratio. Djurašević et al (2006) presented the first model, resulting in orbital inclination of i = 78.5 • and a fill-out factor of f = 32.69 per cent, T2 = 6314 K and T1 = 6095 K, when spots were added. Their no-spot model resulted in very close value for the fill-out factor but slightly different geometrical and orbital parameters.…”
Section: Ee Cetmentioning
confidence: 99%