A Photometric Study of the Contact Binary Xz Leonis

Lee, Jae Woo; Lee, Chung-Uk; Kim, Chun-Hwey; Kang, Yong

doi:10.5303/jkas.2006.39.2.041

Cited by 9 publications

(4 citation statements)

References 20 publications

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“…An unequal quadrature light level, namely the O'Connell effect (O'Connell 1951), is found in many eclipsing binaries and explained by several physical mechanisms, such as the presence of additional orbital mass (also known as third light), a hot spot due to the impact from mass transfer between the components (Lee et al 2006), a cool spot that may be connected with magnetic activity with the same nature as solar magnetic spots (Mullan 1975) and the circulation effect (Zhou & Leung 1990).…”

Section: Star-spot Modelsmentioning

confidence: 99%

Photometric study and preliminary elements of the low-mass ratio W UMa system ASAS 021209+2708.3

Acerbi¹,

Barani²,

Martignoni³

2011

Res. Astron. Astrophys.

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We present CCD B and V light curves, obtained in the year 2006, and a photometric solution of the low-mass ratio contact binary ASAS 021209+2708.3. With our data we were able to determine six new times of minimum light and refine the orbital period of the system to 0.3181963 days. The light curves are analyzed using the 2003 version of the Wilson-Devinney program and the analysis was performed with and without adding a spot on the surface of one star because the light curves appear to exhibit a typical O'Connell effect, with Maximum I brighter than Maximum II. The results show that ASAS 021209+2708.3 may be classified as an A-subtype W Ursae Majoris system with a small mass ratio q = 0.1889, a large over-contact degree of f = 0.587, a very small difference between the component temperatures of ΔT = 53 K and an orbital inclination of i = 81 • . It is known that deep (f > 50%), low-mass ratio (q < 0.25) overcontact binary stars are a very important resource for understanding the phenomena of Blue Straggler/FK Com-type stars. The formations of Blue Straggler stars and FK Com-type stars are unsolved problems in stellar astrophysics. One of the possible explanations for their formation is from the coalescence of W UMa-type overcontact binary systems. The absolute dimensions of ASAS 021209+2708.3 are estimated and its dynamical evolution is inferred.

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Section: Star-spot Modelsmentioning

confidence: 99%

Photometric study and preliminary elements of the low-mass ratio W UMa system ASAS 021209+2708.3

Acerbi¹,

Barani²,

Martignoni³

2011

Res. Astron. Astrophys.

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“…The O'Connell effect (O'Connell 1951) that explains the different heights of the maxima, is visible; a cool spot on the secondary component of AF LMi and a cool spot on the primary component of CzeV188 (inverse O'Connell effect) were added to obtain the best fit to the light curves. The cool spot, in contrast to the hot spot, is connected with magnetic activity of the same nature as solar magnetic spots (Mullan 1975); the hot spot is generally due to the impact of the mass transferred between the components (Lee et al 2006). CzeV188, with its short orbital period (<0.3 days) and its spectral type K, suggests that it is near the shortest period limit.…”

Section: Af Lmi and Czev188mentioning

confidence: 99%

Photometric Study of Two Contact Binary Systems and a Detached Late Dwarf + M Dwarf Components

Michel¹,

Barani²,

Martignoni³

et al. 2023

RMxAA

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The results of our study of the eclipsing binary systems AF LMi, CzeV188 and CRTS J073333.0+302556 based on new CCD B, V, RC, IC complete light curves, are here presented. The short periods of these systems are confirmed and revised. The light curves were modeled using the latest version of the WilsonDevinney code and, as a result, we found that AF LMi (G3+G9) and CzeV188 (K0+K1) are W UMa-type contact binary systems belonging to the W subclass, showing a shallow degree of fill-out with components in good thermal contact. CRTS J073333.0+302556 is a detached binary system composed by a late dwarf (K8) and an M6 dwarf spectral type components. The asymmetries of the light curves were accounted for with a spot on the surface of one of the component. The absolute elements of the three objects were estimated.

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“…for SW Lyn;Lee et al 2006 for XZ Leo; Lee et al 2014 for V407 Peg; Tian & Zhu 2019 for V723 Per), or time-varying spot activity on the components (e.g. Kang et al 2002 for TY UMa; Qian & Yang 2005 for FG Hya).…”

mentioning

confidence: 99%

V608 Cassiopeiae: A W UMa-type eclipsing binary with two possible circumbinary companions

Park,

Lee

2022

Preprint

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We present the photometric properties of V608 Cas from detailed studies of light curves and eclipse timings. The light curve synthesis indicates that the eclipsing pair is an overcontact binary with parameters of ∆T = 155 K, q = 0.328, and f = 26 %. We detected the third light ℓ 3 , which corresponds to about 8 % and 5 % of the total systemic light in V and R bands, respectively. Including our 6 timing measurements, a total of 38 times of minimum light were used for a period study. It was found that the orbital period of V608 Cas has varied in some combination of an upward parabola and two periodic variations. The continuous period increase with a rate of +3.99×10 −7 d yr −1 can be interpreted as a mass transfer from the secondary component to the primary star at a rate of 1.51×10 −7 M ⊙ yr −1 . The periods and semi-amplitudes of the two periodic variations are about P 3 = 16.0 yr and P 4 = 26.3 yr, and K 3 = 0.0341 d and K 4 = 0.0305 d, respectively. The most likely explanation of both cycles is a pair of light-traveling time effects operated by the possible presence of third and fourth components with estimated masses of M 3 = 2.20 M ⊙ and M 4 = 1.27 M ⊙ in eccentric orbits of e 3 = 0.66 and e 4 = 0.52. Because the contribution of ℓ 3 is very low compared to the estimated masses of two circumbinary objects, they can be inferred as very faint compact objects.

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A Photometric Study of the Contact Binary Xz Leonis

Cited by 9 publications

References 20 publications

Photometric study and preliminary elements of the low-mass ratio W UMa system ASAS 021209+2708.3

Photometric study and preliminary elements of the low-mass ratio W UMa system ASAS 021209+2708.3

Photometric Study of Two Contact Binary Systems and a Detached Late Dwarf + M Dwarf Components

V608 Cassiopeiae: A W UMa-type eclipsing binary with two possible circumbinary companions

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