Synthetic light-curve analysis of the very short period binaries TY Bootis, AD Cancri, and V523 Cassiopeiae

Samec, R. G.; Hamme, W. Van; Bookmyer, B. B.

doi:10.1086/115299

Cited by 26 publications

(36 citation statements)

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“…The eclipses are relatively deep and are probably total. Samec & Bookmyer (1987) and Samec et al (1989) reviewed the early history of this system. Photometric solutions of V523 Cas in the contact mode have produced mass ratios of about q ph ¼ 0:6 (Samec et al 1989; q ¼ m 2 =m 1 ).…”

Section: Introductionmentioning

confidence: 99%

“…Samec & Bookmyer (1987) and Samec et al (1989) reviewed the early history of this system. Photometric solutions of V523 Cas in the contact mode have produced mass ratios of about q ph ¼ 0:6 (Samec et al 1989; q ¼ m 2 =m 1 ). This disagreed with the mass ratio, q sp ¼ 0:42, derived directly from radial velocity curves (Milone et al 1985).…”

Section: Introductionmentioning

confidence: 99%

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The Physical Nature and Orbital Behavior of V523 Cassiopeiae

Samec

Faulkner

Williams³

2004

Astron J

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V523 Cassiopeiae is a dwarf contact binary with one of the shortest orbital periods among the nondegenerate systems. Its orbital history is marked by large period changes. The photometrically determined mass ratios have historically been inconsistent with those calculated from radial velocity curves. In 1998 we acquired highprecision and standardized Johnson-Cousins UBV light curves. Our simultaneous BV light curve/radial velocity curve solutions provided good fits to both the light curves and the radial velocity curves using standard gravity darkening coefficients with a mass ratio of $0.5. Seven precision mean epochs of minimum light were determined from these observations. We combine these with all available published times of minimum light, along with 50 times of low light found from a search of the archival Harvard plate stacks in the interval 1901-1942 to give us 567 eclipse timings. Our period study covers nearly 160,000 orbits, or $102 yr. We find a high-amplitude sinusoidal variation with a period of 101 AE 7 yr, overlaid on a strong continuous period increase. The quadratic term is common in contact binaries, but a sinusoidal one is not. This suggests a hierarchical three-star system. Assuming that this is the case and that the inclination from our orbital solution for the close pair is the same as the larger orbit, we obtain a mass for the third star of 0.41 M . This is similar to the masses of the stars that comprise the contact binary. If this scenario is correct, V523 Cas consists of a trio of late K and early M-type dwarfs having a total mass of $1.6 M . We show that high-resolution imaging can confirm this suggestion.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Physical Nature and Orbital Behavior of V523 Cassiopeiae

Samec

Faulkner

Williams³

2004

Astron J

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“…Light curve analysis by Samec et al (1989) shows that the system has a spectral type range between G4 and G8. Rainger et al (1990) combined their spectroscopic observations together with photometric observations by Samec and Bookmyer (1987) to compute the masses and absolute dimensions for the components.…”

Section: Light Curve Modelingmentioning

confidence: 99%

Modern comprehensive study of the W UMa system TY Boo

Elkhateeb

Nouh

Saad

2015

Res. Astron. Astrophys.

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“…6, which was made using the MAC version of Binary Maker (Bradstreet 1990). The present status of our understanding of the dynamic structure of contact binary systems has been reviewed in three recent papers (e.g., Samec et al 1991;Samec 1990;Samec et al 1989b) so we will not repeat that information here.…”

Section: Preliminary Photometric Solutionmentioning

confidence: 99%

CCD photometry and preliminary analysis of V865 Cygni

Samec¹,

Herr²,

Zetzl³

et al. 1992

PASP

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ABSTRACT. CCD images of the thirteenth-magnitude variable V865 Cygni were taken on four consecutive nights in the summer of 1990. The 1.1-m Hall reflector telescope at Lowell Observatory was used in conjunction with an RCA CCD camera system. Four times of minimum light were determined and improved linear and quadratic ephemerides were calculated. A period study, spanning over a fortyyear interval, may indicate that the system is undergoing a continuous period increase of5.4xlO"~8 day yr -1 . In a conservative scenario, this would be an indication of a mass accretion by the primary, more massive, component. The V t R, and / light curves formed by the first precision photometry to be obtained on V865 Cygni show that it is an A-type W UMa system. However, the curves are somewhat incomplete since the maximum that follows the secondary eclipse was not covered. The first synthetic light-curve solution of V865 Cygni is also presented. This solution reveals that V865 Cygni is a contact binary consisting of two G spectral type components with a fillout of -18% and a mass ratio of ~0.45. The component temperature difference is only ~ 110 K. A substantial hot spot region of -34° diameter is proposed to model the asymmetry in the light curves following the observed maximum. We suggest that the origins of this region may be attributed to fluid dynamics rather than to the usual magnetic activity which is prevalent in late-type systems like V865 Cyg.

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Synthetic light-curve analysis of the very short period binaries TY Bootis, AD Cancri, and V523 Cassiopeiae

Cited by 26 publications

References 0 publications

The Physical Nature and Orbital Behavior of V523 Cassiopeiae

The Physical Nature and Orbital Behavior of V523 Cassiopeiae

Modern comprehensive study of the W UMa system TY Boo

CCD photometry and preliminary analysis of V865 Cygni

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