Photometric Properties for Selected Algol-Type Binaries. Viii. The Triple Systems Di Peg and Af Gem Revisited

Yang, Yuangen; Yang, Ying; Li, Shu-Zheng

doi:10.1088/0004-6256/147/6/145

Cited by 9 publications

(12 citation statements)

References 29 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…By using the formula of ∆P/P = 9∆Q/Ma 2 = 2πA/P mod , where M is the mass of the active component, and a is the separation between both components, respectively (Yang et al 2012), we can compute the values as follows: ∆Q 1 = 9.64 × 10 48 g cm 2 and ∆Q 2 = 1.14 × 10 49 g cm 2 , which is evidently smaller than the typical values of 10 51 10 52 g cm 2 for close binaries (Lanza & Rodonò 1999). Therefore, we can rule out Applegates mechanism for interpreting the cyclic variations for NSVS 01286630 (Yang et al 2014). Hence, NSVS 01286630 maybe a triple system.…”

Section: Discussionmentioning

confidence: 95%

NSVS 01286630: a detached binary with a close-in companion

Zhang

Qian

Liao

et al. 2018

Res. Astron. Astrophys.

View full text Add to dashboard Cite

New photometric observations of NSVS 01286630 were performed and two sets of four-color (B, V , R c , I c ) light curves (LCs) were obtained. Using the 2013 version of the Wilson-Devinney (W − D) code, we analyzed these data. The photometric solutions reveal that NSVS 01286630 is an active detached eclipsing binary (EB) with a high orbit inclination(nearly 90 • ). Remarkably, the temperature of the primary component (the hotter star) is higher than the secondary one, but, the value of mass ratio q( M2 M1 ) for NSVS 0128663 is more than 1, which can be explained that the surface of the secondary component of NSVS 01286630is covered with big cool-star-spots. Based on our new CCD mid-eclipse times and the data published until now, the variations of the mid-eclipse times were reanalyzed in detail using a weighted least-squares method. It is discovered that the (O − C) diagram of the system shows a cyclic oscillation with a period of 3.61 yr and an amplitude of 0.001 days. The cyclic variation may be caused by the light travel time effect (LTTE) due to the presence of a third companion, whose mass we calculated is M 3 sin(i 3 )=0.11 M ⊙ . The third body may affect the orbital evolution of the central binary system by transferring the angular momentum.

show abstract

Section: Discussionmentioning

confidence: 95%

NSVS 01286630: a detached binary with a close-in companion

Zhang

Qian

Liao

et al. 2018

Res. Astron. Astrophys.

View full text Add to dashboard Cite

show abstract

“…Additionally, as mentioned in the previous section, the residuals from the sine fit show another low-amplitude, short-period and eccentric cyclic modulation. This variation is also interpreted as the existence of a fourth body physically connected to the system by Yang et al (2014). From the O-C diagram, we calculated the period and amplitude of the secondary modulation as 27.40(24) yr and 0.0051(2) days.…”

Section: Resultsmentioning

confidence: 99%

“…Based on the results, he suggested the existence of a third light which provided 24% contribution to the total light of the system. More photometric studies were performed by Chou and Kitamura (1968), Binnendijk (1973), Chaubey (1982), Lu (1992), andYang et al (2014). Gaposchkin (1953) detected a variation in the orbital period of the star.…”

Section: Introductionmentioning

confidence: 95%

“…The masses of the inner and outer sub-stellar objects were given to be M in ∼ 0.095 M and M out ∼ 0.170 M . On the basis of these results, Yang et al (2014) suggested that the system has consisted of four objects.…”

Section: Introductionmentioning

confidence: 96%

“…Recently, Yang et al (2014) reproduced the photometric models by the help of new multi-color observations and previously published ones in literature. They determined the system parameters as i = 89…”

Section: Introductionmentioning

confidence: 97%

See 2 more Smart Citations

The Period Analysis of the Hierarchical System DI Peg

Özuyar¹,

Elmaslı²,

Çalışkan³

2018

IBVS

View full text Add to dashboard Cite

The existence of an additional body around a binary system can be detected by the help of the light-travel time effect. Due to the motions of binary and the companion stars around the common mass center of the ternary system, the light-time effect produces an irregularity on the eclipse timings. Monitoring the variations in these timings, sub-stellar or planet companions orbiting around the binary system can be identified. In this paper, additional bodies orbiting the Algol type binary DI Peg are examined by using the archival eclipse timings including our CCD data observed at the Ankara University Kreiken Observatory. More than five hundred minimum times equivalent to around nine decades are employed to identify the orbital behavior of the binary system. The best fit to the timings shows that the orbital period of DI Peg has variation due to an integration of two sinusoids with the periods of P3 = 49.50 ± 0.36 yr and P4 = 27.40 ± 0.24 yr. The orbital change is thought to be most likely due to the existence of two M-type red dwarf companions with the masses of M3 = 0.213 ± 0.021 M and M4 = 0.151 ± 0.008 M , assuming that the orbits of additional bodies are co-planar with the orbit of the binary system. Also, the residuals of two sinusoidal fits still seem to show another modulation with the period of roughly P = 19.5 yr. The origin of this modulation is not clear and more observational data are required to reveal if the periodicity is caused by another object gravitationally bounded to the system.

show abstract

Ww Geminorum: An Early B-Type Eclipsing Binary Evolving Into the Contact Phase

Yang

Dai

et al. 2014

View full text Add to dashboard Cite

Photometric Properties for Selected Algol-Type Binaries. Viii. The Triple Systems Di Peg and Af Gem Revisited

Cited by 9 publications

References 29 publications

NSVS 01286630: a detached binary with a close-in companion

NSVS 01286630: a detached binary with a close-in companion

The Period Analysis of the Hierarchical System DI Peg

Ww Geminorum: An Early B-Type Eclipsing Binary Evolving Into the Contact Phase

Contact Info

Product

Resources

About