Revised UBV photometric solution of the early-type contact system BH Centauri

Leung, K. C.; Sisteró, R. F.; Zhai, D. S.; Grieco, A.; Candellero, B.

doi:10.1086/113582

Cited by 13 publications

(6 citation statements)

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“…the mass transfer can be calculated to be Ṁ2 = 2.8 × 10 −6 M ⊙ per year by assuming the mass is the same as in Leung et al (1984). This indicates the binary is now undergoing Case A mass transfer.…”

Section: Discussionmentioning

confidence: 97%

“…From figure 1 of Leung & Schneider (1977), we can see that there were large scatters in all three bands. Subsequently, Leung et al (1984) reduced the number of points in these light curves and updated the analysis. From that time when the latest light curves were analyzed, more than thirty years have passed.…”

Section: New Observations and Period Analysis Of Bh Cenmentioning

confidence: 99%

“…During recent decades, the W-D code has undergone many changes (Wilson & Devinney 1971;Wilson 1990, We applied effective temperature of the primary, T 1 = 17 900 K, which is the same as what Leung et al (1984) determined. There was no mass ratio from spectral observation before, so we used the q-search method to find an initial mass ratio.…”

Section: Photometric Solutionsmentioning

confidence: 99%

“…Then, Sistero et al (1983) obtained more reliable light curves without large scatter. Leung et al (1984) analyzed the light curves and found that the degree of overcontact in this system is 48% and the mass ratio is 0.84. They also estimated the absolute parameters of the binary system by considering its membership in the young Galactic cluster IC 2944.…”

Section: Introductionmentioning

confidence: 98%

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New CCD photometric investigation of the early-type overcontact binary BH Cen in the young star-forming Galactic cluster IC 2944

Zhao

Qian

Zejda

et al. 2018

Res. Astron. Astrophys.

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BH Cen is a short-period early-type binary with a period of 0.792 d in the extremely young star-forming cluster IC 2944. New multi-color CCD photometric light curves in U , B, V , R and I bands are presented and are analyzed by using the Wilson-Devinney code. It is detected that BH Cen is a high-mass-ratio overcontact binary with a fill-out factor of 46.4% and a mass ratio of 0.89. The derived orbital inclination i is 88.9 degrees, indicating that it is a totally eclipsing binary and the photometric parameters can be determined reliably. By adding new eclipse times, the orbital period changes in the binary are analyzed. It is confirmed that the period of BH Cen shows a long-term increase while it undergoes a cyclic oscillation with an amplitude of A 3 = 0.024 d and a period of P 3 = 50.3 yr. The high mass ratio, overcontact configuration and long-term continuous increase in the orbital period all suggest that BH Cen is in the evolutionary state after the shortest-period stage of Case A mass transfer. The continuous increase in period can be explained by mass transfer from the secondary component to the primary one at a rate of Ṁ2 = 2.8×10 −6 M ⊙ per year. The cyclic change can be plausibly explained by the presence of a third body because both components in the BH Cen system are early-type stars. Its mass is determined to be no less than 2.2 M ⊙ at an orbital separation of about 32.5 AU. Since no third light was found during the photometric solution, it is possible that the third body may be a candidate for a compact object.

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Section: Discussionmentioning

confidence: 97%

Section: New Observations and Period Analysis Of Bh Cenmentioning

confidence: 99%

Section: Photometric Solutionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

See 2 more Smart Citations

New CCD photometric investigation of the early-type overcontact binary BH Cen in the young star-forming Galactic cluster IC 2944

Zhao

Qian

Zejda

et al. 2018

Res. Astron. Astrophys.

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“…They are uncommon objects, in contrast to the very abundant W UMas, and easily distinguished from them in several ways, including their early spectral types. Examples of these high temperature OC binaries are BH Centauri (see e.g., [16]), RZ Pyxidis (e.g., [17]), and V701 Scorpii (e.g., [18]). sources, although stars of measured apparent brightness are used in practice.…”

Section: Distancesmentioning

confidence: 99%

Close Binary Perspectives

Wilson

2020

Galaxies

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Development of analytic binary star models is discussed in historical and on-going perspective, beginning with an overview of paradigm shifts, the merits of direct (rectification-free) models, and fundamental four-type binary system morphology. Attention is called to the likelihood that many or even most cataclysmic variables may be of the double contact morphological type. Eclipsing binary distance estimates differ from those of standard candles in being individually measurable—without reliance on (usually nearby) objects that are assumed similar. Recent progress on circumstellar accretion disk models is briefly summarized, with emphasis on the separate roles of fluid dynamic, structural, and analytic models. Time-related parameters (ephemeris, apsidal motion, and light travel time) now can be found with a unified algorithm that processes light curves, velocity curves, and pre-existing eclipse timings together, without need to compute any new timings. Changes in data publication practices are recommended and logical errors and inconsistencies in terminology are noted. Parameter estimation strategies are discussed.

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Case a evolution of massive close binary systems

Nakamura

1987

Astrophys Space Sci

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Revised UBV photometric solution of the early-type contact system BH Centauri

Cited by 13 publications

References 0 publications

New CCD photometric investigation of the early-type overcontact binary BH Cen in the young star-forming Galactic cluster IC 2944

New CCD photometric investigation of the early-type overcontact binary BH Cen in the young star-forming Galactic cluster IC 2944

Close Binary Perspectives

Case a evolution of massive close binary systems

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