A radial-velocity study of V523 Cassiopeiae

Milone, Eugene F.; Hrivnak, Bruce J.; Fisher, W. A.

doi:10.1086/113739

Cited by 21 publications

(15 citation statements)

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“…The Tycho distance is almost certainly incorrect. An 11 mag star at the Tycho distance would have to be of type M, nearly an entire spectral type cooler than what it is known from both spectroscopy (Milone et al 1985) and our photometry. If there is a third member of this system, as we suggest here, then from Figure 3 it would appear that the companion should be near the greatest separation now.…”

Section: Light Curve Solutionsmentioning

confidence: 75%

“…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). The author (R. G. S.) found that, even with the use of a simultaneous Roche lobe treatment, it is impossible to get a good fit to the light curve and the radial velocity curves.…”

Section: Introductionmentioning

confidence: 86%

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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: Light Curve Solutionsmentioning

confidence: 75%

Section: Introductionmentioning

confidence: 86%

The Physical Nature and Orbital Behavior of V523 Cassiopeiae

Samec

Faulkner

Williams³

2004

Astron J

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“…Mass ratios produced by photometric solutions of V523 Cas are q ph = 0.59 by Bradstreet (1981), 0.571 by Samec et al (1989), 0.53 by Lister et al (2000), 0.56 by Kim & Jeong (2002), and 0.52 by Samec et al (2004). Those values disagreed with the spectroscopic mass ratio, q sp = 0.42, derived directly from radial velocity curves by Milone et al (1985). Niarchos & Duerbeck (1991) had proposed that a circulation effect of sideward convection may affect the radial velocity curves in a systematic way, causing the discrepancy in q ph and q sp .…”

Section: Introductionmentioning

confidence: 64%

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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“…High levels of Ca II H and K emission in optical band and Mg II h+k emission lines in UV indicate high levels of magnetic activity (Wolff et al 1965;Hrivnak et al 1995). The asymmetry and variation of light curve of VZ Psc were reported by several authors (e.g., Eggen 1967;Bradstreet 1985;Davidge & Milone 1984;Milone et al 1985 andSamec 1989). The…”

Section: Introductionmentioning

confidence: 65%

Possible connection between period change and magnetic activity of the very short‐period binary VZ Piscium

et al. 2004

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Abstract. New times of light minimum of the short-period (P = 0 d .26) close binary system, VZ Psc, are presented. A period investigation of the binary star, by combining the three new eclipse times with the others collected from the literatures, shows that the variation of the period might be in an alternate way. Under the hypothesis that the variation of the orbital period is cyclic, a period of 25 years and an amplitude of 0.d 0030 for the cyclic change are determined. If this periodic variation is caused by the presence of a third body, the mass of the third body (m3) should be no less than 0.081 M . Since both components of VZ Psc are strong chromospherically active and the level of activity of the secondary component is higher than that of the primary one, the period may be more plausibly explained by cyclic magnetic activity of the less massive component.

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A radial-velocity study of V523 Cassiopeiae

Cited by 21 publications

References 0 publications

The Physical Nature and Orbital Behavior of V523 Cassiopeiae

The Physical Nature and Orbital Behavior of V523 Cassiopeiae

Photometric Observations of the Contact Binary System V523 Cassiopeiae

Possible connection between period change and magnetic activity of the very short‐period binary VZ Piscium

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