Multi-color light curves and orbital period research of eclipsing binary V1073 Cyg

Tian, Xiaomin; Zhu, L.-Y.; Qian, S.‐B.; Li, Linjia; Jiang, Lin-Qiao

doi:10.1088/1674-4527/18/2/20

Cited by 17 publications

(6 citation statements)

References 62 publications

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“…The downward parabolic curve in the O − C diagram shows an orbital period decrease at a rate of dP/dt = −14.19 × 10 −9 d yr −1 without a sinusoidal term and dP/dt = −9.61 × 10 −9 d yr −1 with a cyclical term. The type of variations, i.e., a long-term decrease combined with a cyclic change, is commonly found in W UMa-type stars, for example V417 Aql (Qian 2003), V1139 Cas (Li et al 2015b), MR Com (Qian et al 2013b), BX Peg (Li et al 2015a), V524 Mon (He et al 2012), and V1073 Cyg (Tian et al 2018). Some W-type contact binaries whose properties are similar to RW Dor are listed in table 8: most of them are shallow contact binaries with decreasing period.…”

Section: Discussionmentioning

confidence: 99%

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Sarotsakulchai

Qian

Soonthornthum

et al. 2019

Publications of the Astronomical Society of Japan

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New CCD photometric light curves of the short-period (P = 0.285 d) eclipsing binary RW Dor are presented. The observations were performed with the PROMPT-8 robotic telescope at CTIO in Chile between 2015 March and 2017 March. Other eclipse timings were obtained from the 2.15 m JS telescope at CASLEO, San Juan, Argentina in 2011 December. Based on a light curve analysis, it is found that RW Dor is a W-type shallow contact binary with a fill-out factor f ∼ 11% and a high mass ratio q ∼ 1.587 (1/q = 0.63), where the hotter component is the less massive one (M 1 ∼ 0.52 M and M 2 ∼ 0.82 M ). For orbital-period investigation, 15 new eclipse times and those previously published were compiled. O − C analysis with very weak evidence suggests that a long-term decrease in period with a rate of dP/dt = −9.61 × 10 −9 d yr −1 is superimposed on a cyclic variation (A 3 = 0.0054 d and P 3 = 49.9 yr). The long-term decrease can be interpreted as mass transfer from the more massive component to the less massive one, or combined with angular momentum loss via magnetic braking. In addition, the marginal contact phase, high mass ratio (1/q > 0.4), and long-term decrease in period all suggest that RW Dor is a newly formed contact binary via Case A mass transfer, and it will evolve into a deeper normal contact binary. If the cyclic change is correct, the light travel-time effect via the presence of a cool third body will be a more plausible explanation for this.

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Section: Discussionmentioning

confidence: 99%

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Sarotsakulchai

Qian

Soonthornthum

et al. 2019

Publications of the Astronomical Society of Japan

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“…The light curves show β Lyrae characteristics. The atmospheric parameters of the primary star are estimated through the low resolution spectral fit as follows: T eff = TYC 6408-989-1 is one of the three well known Am type marginal contact binaries, the others are V1073 Cyg (Tian et al 2018) and V2782 Ori (Tian et al 2019). The orbital inclination of this target is i = 69.31(26) • .…”

Section: Discussionmentioning

confidence: 99%

Investigation of the shortest period Am type eclipsing binary TYC 6408–989–1

Tian

2021

Res. Astron. Astrophys.

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The first BV bands photometric observations and the low-resolution spectrum of the shortest period Am type eclipsing binary TYC 6408–989–1 have been obtained. The stellar atmospheric parameters of the primary star were obtained through the spectral fitting as follows: T eff = 6990 ± 117 K, log g = 4.25 ± 0.26 cm s−2, [Fe/H] = −0.45 ± 0.03 dex. The original spectra obtained by European Southern Observatory (ESO) were processed with an IRAF package by us. Based on the ESO blue-violet spectra, TYC 6408–989–1 was concluded as a marginal Am (Am:) star with a spectral type of kA3hF1mA5 IV-V identified through the MKCLASS program. The observed light curves were analyzed through the Wilson-Devinney code. The final photometric solutions show that TYC 6408–989–1 is a marginal contact binary with a low mass ratio (q = 0.27). The temperature of the secondary component derived through the light curve analysis is significantly higher than main sequence stars. In addition, TYC 6408–989–1 is a poor thermal contact binary. The temperature differences between the two components is about 1800 K. TYC 6408–989–1 should be located in the oscillation stage predicted by the thermal relaxation oscillations theory (TRO) and will evolve into the shallow contact stage eventually. The very short period (less than one day), marginal Am peculiarity and quite large rotational velocity (v sin i ≃ 160 km s−1) make TYC 6408–989–1 become a challenge to the cut-off of rotation velocities and periods of Am stars. We have collected the well known eclipsing Am binaries with absolute parameters from the literature.

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“…Our results show that V2787 Ori is a shallow-contact binary, and the fill-out factor is ´- ) . Among the eclipsing Am binaries, only three contact binaries were found: V1073 Cyg (Tian et al 2018), V2787 Ori and TYC 6408-989-1 (X. M. Tian, 2019, in preparation). The orbital period of V2787 Ori is longer than those of typical EW-type contact binary stars (Qian et al 2017;Qian et al 2018).…”

Section: Discussionmentioning

confidence: 99%

Am-Type Eclipsing Binary V2787 Ori: An Evolved Shallow-contact Binary with an Extremely Low Mass Ratio

Tian

Zhu

Wang

2019

PASP

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The first complete multicolor CCD light curves and low-resolution spectra of the short-period Am-type eclipsing binary V2787 Ori are presented. The atmospheric parameters of the primary component, including the effective temperature (T), the gravitational acceleration (log g), and the metallicity [Fe/H], are determined as T eff =6993±82 K, g log 4.10 0.22 cm s 2 =  , and dex Fe H 0.40 0.18 = - [ ], respectively. The Wilson-Devinney (W-D) code was used to analyze those BVR I c c light curves, and the photometric solutions of this eclipsing binary were derived for the first time. It was discovered that V2787 Ori is a shallow-contact, totaleclipsing binary with a factor of f=0.181(±0.077) and an extremely low mass ratio of q=0.120(±0.002). The primary contributes about 95% luminosity to the total system, and the temperature difference between the two components exceeds 1600 K. This target may be the smallest mass ratio B-subtype system, but it definitely is among the smallest mass ratio B-subtype systems. The temperature of the secondary is determined as 5413 K, while its mass is estimated as M M 0.17 0.01 2 =   ( ) . These properties indicate that the binary may undergo a special evolution where the secondary may be the original more massive component and has transferred most of its mass to its companion. We combined our newly determined eclipse times with those collected from the previous literature, and found that the O − C curve of the binary system shows a cyclic variation with an amplitude of 0.0054 days and a period of 17.3 years, which is explained as the result of the light-time effect, due to a third body orbiting around the central binary. The minimal mass of the third body is 0.208 M e , and the corresponding orbital radius is about 7.24 au. The shallow-contact configuration, the extremely low mass ratio, the evolved components, and the presence of a tertiary component, all make the B-subtype Am-type contact binary a significant target for further investigations.

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Multi-color light curves and orbital period research of eclipsing binary V1073 Cyg

Cited by 17 publications

References 62 publications

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

RW Doradus: A solar-type shallow contact binary with a new orbital period investigation

Investigation of the shortest period Am type eclipsing binary TYC 6408–989–1

Am-Type Eclipsing Binary V2787 Ori: An Evolved Shallow-contact Binary with an Extremely Low Mass Ratio

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