Contact binary stars

Mochnacki, S. W.

doi:10.1086/158841

Cited by 234 publications

(155 citation statements)

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“…The intial solutions (Abrami 1959;Binnendijk 1969) used the classic RussellMerrill method. After Mauder (1972) showed that a more sophisticated approach is needed for contact systems such as AM Leo, Hutchings & Hill (1973), Twigg (see Mochnacki 1981), Jabbar & Kopal (1983), and Binnendijk (1984) modeled the system using the light curve synthesis approach. All the light curve synthesis solutions have been based on Binnendijk's (1969) observations, except that Binnendijk (1984) also considered Abrami's (1959) unfiltered combined-light measures after applying a correction for the light of the companion.…”

Section: Light Curve Solutionmentioning

confidence: 99%

New Light Curves and Orbital Solution for AM Leonis

Hiller

Osborn

Terrell

2004

PUBL ASTRON SOC PAC

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ABSTRACT. New UBVRI photometry has been obtained for the W UMa eclipsing system AM Leonis. The data have been used to derive nine times of minimum and to construct light curves. The minimum timings show that the system recently had a significant period increase. Modeling of the light curves shows AM Leo to be an overcontact system with a mass ratio of 2.51. Both Rucinski & Duerbeck's absolute magnitude calibration for W UMa stars applied to our photometry and the radial velocity curve combined with our derived parameters indicate a distance near 125 pc, larger than the 77 pc from the Hipparcos parallax.

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Section: Light Curve Solutionmentioning

confidence: 99%

New Light Curves and Orbital Solution for AM Leonis

Hiller

Osborn

Terrell

2004

PUBL ASTRON SOC PAC

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“…The more massive secondary component is under-luminous, while the less massive primary component is over-luminous and over-sized with the respect to their ZAMS masses. This might be the consequence of the assumption that the more massive component is transferring energy to the less massive component (e.g., Mochnacki, 1981;Yakut & Eggleton 2005).…”

Section: Discussionmentioning

confidence: 99%

The active W UMa type binary star V781 Tau revisited

Gao

et al. 2016

Astrophys Space Sci

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In this paper, new determined BV R c I c light curves and radial velocities of V781 Tau are presented. By analyzing the light curves and radial velocities simultaneously, we found that V781 Tau is a W-subtype medium contact binary star with a mass ratio of q = 2.207 ± 0.005 and a contact degree of f = 21.6(±1.0)%. The difference between the two light maxima was explained by a dark spot on the less massive primary component. The orbital period change of V781 Tau was also investigated. A secular decrease at a rate of −6.01(±2.28)×10−8 d/yr and a cyclic modulation with a period of 44.8±5.7 yr and an amplitude of 0.0064 ± 0.0011 day were discovered. The continuous period decrease may be caused by angular momentum loss due to magnetic stellar wind. Applegate mechanism failed to explain the cyclic modulation. It is highly possible that the cyclic oscillation is the result of the light travel time effect by a third companion.

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“…parameters of these systems are also listed in Table 7, in which the density of the secondary component, D 2 in g/cm 3 , is (Mochnacki 1981)…”

Section: Discussionmentioning

confidence: 99%

UY Ursae Majoris: A W-subtype W UMa system with a small mass ratio

Leung

2001

A&A

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Abstract. We present light curves and photometric solutions of the contact binary UY UMa in this paper. The light curves appear to exhibit a typical O'Connell effect, with Maximum I being 0.034 mag(V ) and 0.030 mag(B) brighter than Maximum II, respectively, and Maximum I shifting to phase 0.26. The light curves are analyzed by means of the latest version of the WD program. The results show that UY UMa is a W-subtype contact binary with a small mass ratio q = 0.134. The asymmetry of the light curves is explained by star spot models. From the collected data of 9 UMa contact systems with a smaller mass ratio than 0.20, the nature of the secondaries is analyzed. The results show that the luminosities and densities of the secondaries could be controlled by the primaries and that the smaller the mass ratio, the stronger the control.

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Contact binary stars

Cited by 234 publications

References 0 publications

New Light Curves and Orbital Solution for AM Leonis

New Light Curves and Orbital Solution for AM Leonis

The active W UMa type binary star V781 Tau revisited

UY Ursae Majoris: A W-subtype W UMa system with a small mass ratio

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