UBVRcIcANALYSIS OF THE RECENTLY DISCOVERED TOTALLY ECLIPSING EXTREME MASS RATIO BINARY V1853 ORIONIS, AND A STATISTICAL LOOK AT 25 OTHER EXTREME MASS RATIO SOLAR-TYPE CONTACT BINARIES

Samec, R. G.; Labadorf, C. M.; Hawkins, N. C.; Faulkner, D. R.; Hamme, W. Van

doi:10.1088/0004-6256/142/4/117

Cited by 18 publications

(19 citation statements)

References 20 publications

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“…The temperature difference is 629 K (Yang et al 2013a) andthe degree of fillout is only 5.8%, while the difference is 57 K in 2010 andthe corresponding contact is 25.7%. It is suggested that the contact with greater ΔT will be at the lowest fill-out, which agrees with the statistical relation between the fill-out and the temperature difference presented by Samec et al (2011). The variable degree of the fill-out in such a short timeimplies that it would evolve with a dynamic timescale.…”

Section: Intrinsic Activities Of the Componentsupporting

confidence: 77%

A Comprehensive Photometric Study of the Contact Binary Gn Boo With Possible Magnetic Activities

Wang

Qian

Zhang

et al. 2015

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Multi-color photometric data of GN Boo observed from 2010 to 2013 are presented. The intrinsic variations of the light curves are remarkable, and their phenomena are probable evidence of stronger magnetic activities on the surfaces of the components. Based on all CCD times of minimum light, a secular increase superimposed on a cyclic oscillation is found. The orbital period increases at a rate of dP/dt = +1.74 × 10 −7 days yr −1 , which can be explained by mass transfer from the less massive component to the more massive one. The period and amplitude of the cyclic variation are P = 9.5632 yr and A = 0.0046 days, respectively, which correspond to the previous published results. Using the 2010 version of the W-D code, five sets of photometric solutions were derived from our new data. The results imply that the stellar spot, the degree of fill-out, and the temperature difference ΔT between the components of GN Boo are variable. It is inferred that the magnetic activities perhaps influence the outer radius of the component, causing the temperature of the component star and the level of contact to change.

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Section: Intrinsic Activities Of the Componentsupporting

confidence: 77%

A Comprehensive Photometric Study of the Contact Binary Gn Boo With Possible Magnetic Activities

Wang

Qian

Zhang

et al. 2015

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“…1 in the paper by Tylenda et al (2011)). Some low-mass-ratio and deep contact binary stars were discovered by Qian et al (2005aQian et al ( , 2011, Yang et al (2012Yang et al ( , 2013, Samec et al(2011) and Zhu et al (2005Zhu et al ( , 2011 where the fill-out factor (f ) is higher than 50 %. The orbital periods of some targets are decreasing continuously.…”

Section: Discussionmentioning

confidence: 99%

A low-mass-ratio and deep contact binary as the progenitor of the merger V1309 Sco

Zhu

Zhao

Xiao

2016

Res. Astron. Astrophys.

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Nova Sco 2008 (=V1309 Sco) is one of the V838 Mon type eruptions rather than a typical classical nova. This enigmatic object was recently shown to have resulted from the merger of the two stars in a contact binary. It is the first stellar merger that was undergoing a common envelope transient. To understand the properties of its binary progenitor, the pre-outburst light curves were analyzed by using the W-D (Wilson and Devinney) method. The photometric solution of the 2002 light curve shows that it is a deep contact binary (f = 89.5(±40.5) %) with a mass ratio of 0.094. The asymmetry of the light curve is explained by the presence of a dark spot on the more massive component. The extremely high fill-out factor suggests that the merging of the contact binary is driven by dynamical mass loss from the outer Lagrange point. However, the analysis of the 2004 light curve indicates that no solutions were obtained even at an extremely low mass ratio of q=0.03. This suggests that the common convective envelope of the binary system disappeared and the secondary component has spiraled in the envelope of the primary in 2004. Finally, the ejection of the envelope of the primary produced the outburst.

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“…Since the variable was discovered by Gettel et al (2006), the period changes were study only by Samec et al (2011), and their study shows no variation. Diethelm (2011) and Diethelm (2012) With the quadratic term of this ephemeris, a continuous period decrease, at a rate of dP/dt = −1.96(0.46)× 10 −7 d yr −1 is determined.…”

Section: Orbital Period Investigationmentioning

confidence: 99%

“…Therefore, it is a progenitor candidate of luminous red novae (e.g., Zhu et al 2016). Samec et al (2011) revised the linear ephemeris as, M in.I(HJD) = 2454066.57858 + 0 d .38300155 × E.…”

Section: Introductionmentioning

confidence: 99%

“…PHOT (measure magnitudes for a list of stars) of the aperture photometry package of the IRAF was used to reduce the observed images. The photometric data in B, V , Rc and Ic bands together with their Heliocentric Julian dates are listed in Table 3, Table 4, Table 5 and Table 6, 3) is obtained by us and the period is from Samec et al (2011).…”

Section: Introductionmentioning

confidence: 99%

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New photometric investigation of the low-mass-ratio contact binary star V1853 Orionis

Qian

Soonthornthum

et al. 2019

Res. Astron. Astrophys.

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Four-color charge-coupled device (CCD) light curves in B, V , Rc and Ic bands of the total-eclipsing binary system, V1853 Ori, are presented. By comparing our light curves with those published by previous investigators, it is detected that the O'Connell effect on the light curves is disappeared. By analyzing those multi-color light curves with the Wilson-Devinney code (W-D code), it is discovered that V1853 Ori is an A-type intermediatecontact binary with a degree of contact factor of f = 33.3%(3.7%) and a mass ratio of q = 0.1896(0.0013). Combining our 10 new determined times of light minima together with the others published in the literature, the period changes of the system is investigated. We found that the general trend of the observed-calculated (O − C) curve shows a downward parabolic variation that corresponds to a long-term decrease in the orbital period with a rate of dP/dt = −1.96(0.46) × 10 −7 d yr −1 . The long-term period decrease could be explained by mass transfer from the more-massive component to the less-massive one. By combining our photometric solutions with the Gaia DR 2 data, absolute parameters were derived as M 1 = 1.20 M ⊙ , M 2 = 0.23 M ⊙ , R 1 = 1.36 R ⊙ , and R 2 = 0.66 R ⊙ . The long-term period decrease and the intermediate-contact configuration suggest that V1853 Ori will evolve into a high fill-out overcontact binary. 2 J.-J. He et al.

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UBVR_cI_cANALYSIS OF THE RECENTLY DISCOVERED TOTALLY ECLIPSING EXTREME MASS RATIO BINARY V1853 ORIONIS, AND A STATISTICAL LOOK AT 25 OTHER EXTREME MASS RATIO SOLAR-TYPE CONTACT BINARIES

Cited by 18 publications

References 20 publications

A Comprehensive Photometric Study of the Contact Binary Gn Boo With Possible Magnetic Activities

A Comprehensive Photometric Study of the Contact Binary Gn Boo With Possible Magnetic Activities

A low-mass-ratio and deep contact binary as the progenitor of the merger V1309 Sco

New photometric investigation of the low-mass-ratio contact binary star V1853 Orionis

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