Simultaneous light and velocity curve solution and probable starspot activities for the W UMa system U Pegasi

Zhai, D. S.; Lü, Wei; Zhang, Xiaoyu

doi:10.1007/bf00656975

Cited by 7 publications

(2 citation statements)

References 9 publications

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“…1. Zhai et al (1988) explained such an asymmetry is due to the spot activity on the secondary component. The variation in the light curves of V523 Cas takes place in terms of days, weeks, and months.…”

Section: Observations and Light Curvesmentioning

confidence: 98%

“…Since Weber (1958) discovered the light variability of V523 Cas, many investigations in photometry and spectroscopy have been carried out (Zhukov 1972, Haussler 1974, Lavrov & Zhukov 1975, Bradstreet 1981, Hoffmann 1981, Samec & Bookmyer 1987, Zhai et al 1988, Samec et al 1989, Kim & Jeong 2002, Samec et al 2004, Genet et al 2005, Jeong et al 2006. In results, some facts about V523 Cas are known: 1) its orbital period of about 336 minutes is one of the shortest among late type contact binaries.…”

Section: Introductionmentioning

confidence: 99%

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Photometric Observations of the Contact Binary System V523 Cassiopeiae

Jeong¹,

Kim²,

Lee³

2010

Journal of Astronomy and Space Sciences

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A total of 583 observations (193 in Δb, 190 in Δv, 200 in Δr) for V523 Cas was made on 9 nights from September to December in 2008 using the 100 cm telescope with 2K CCD camera of the Chungbuk National University Observatory. With our data BVR light curves were constructed and 9 times of minimum light were determined. We also obtained physical parameters of the V523 Cas system by analysis of the BVR light curves using the Wilson-Devinney code.

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Section: Observations and Light Curvesmentioning

confidence: 98%

Section: Introductionmentioning

confidence: 99%

Photometric Observations of the Contact Binary System V523 Cassiopeiae

Jeong¹,

Kim²,

Lee³

2010

Journal of Astronomy and Space Sciences

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New observations, photometric study and preliminary elements of the W UMa system DF CVn

Acerbi¹,

Barani²,

Martignoni³

2005

Astron. Nachr.

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Abstract. CCD (V) light curve of the EW-type eclipsing variable DF CVn was obtained during seven nights in April-May, 2004. With our data we were able to determine 4 new times of minimum light. The light curve appears to exhibit a typical O'Connell effect, with Maximum I brighter than Maximum II by 0.013 mag. in V. Two Wilson-Devinney (WD) code working sessions, using the V light curve, were done with and without spots. The analysis of the results shows that the best fit was obtained with the spotted solution and indicates contact geometry. The photometric mass ratio of the system is found to be q = 0.347 and its inclination i = 72• , the primary minimum shows a transit. The star may be classified as an A-type W UMa system. Assuming a reasonable value for the mass of the primary component an estimate of the absolute elements of DF CVn has been made, with the assumption that the primary has a mass corresponding to its spectral type according to Straizys and Kuriliene (1981).

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A photometric study of the W UMa-type system U Pegasi

Djurašević

Rovithis‐Livaniou²,

Rovithis

et al. 2001

A&A

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Abstract. In the present study, the activity of the eclipsing binary of the W UMa-type system U Peg is examined by analysing the photoelectric observations covering the period from 1950 to 1989. During this period, the light curves show significant differences and asymmetries. The analysis of the corresponding light curves is made using Djurašević's inverse problem method. To explain the light-curve asymmetries and variations, we used a Roche model that involved regions containing spots on the components. The analysis shows that the system U Peg is in an overcontact configuration (f over ∼ 14.9%). The Roche model with spotted areas on the cooler component yields a good fit of the observations for the whole set of the analysed light curves without any changes of the basic system parameters. This indicates that the complex nature of the light-curve variations during the examined period can be explained by the evolution and motion of spotted areas on the cooler component. According to the obtained results, the spotted areas cover a significant part of the stellar surface; the changes in their location and size with time are examined.

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Simultaneous light and velocity curve solution and probable starspot activities for the W UMa system U Pegasi

Cited by 7 publications

References 9 publications

Photometric Observations of the Contact Binary System V523 Cassiopeiae

Photometric Observations of the Contact Binary System V523 Cassiopeiae

New observations, photometric study and preliminary elements of the W UMa system DF CVn

A photometric study of the W UMa-type system U Pegasi

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