Orbital period changes of the W UMa binary YY Eri

Yu, Ting; Hu, Ke; Yu, Yun-Xia; Fang, Xiang

doi:10.1088/1674-4527/18/9/106

Cited by 2 publications

(2 citation statements)

References 27 publications

(43 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…That means the period is increased continuously by approximately 4.57 × 10 -3 seconds/year. Corresponding to the period changing rate of 5.51× 10 -3 seconds/year calculated by Ting et al in 2018 [10]. The increase of the period showed that the distance between the stars was increased according to Thermal Relaxation Oscillation (TRO) theory.…”

Section: Resultsmentioning

confidence: 68%

See 1 more Smart Citation

A Period Change Study of the Contact Binary System YY Eri

Pancharoen

Maithong

2022

ASEAN Sci Tech Rept

View full text Add to dashboard Cite

The W UMa type of the eclipsing binary system YY Eri was observed by using a 0.7-meter telescope with a CCD photometric system in B, V, and R filters at the Regional Observatory for the Public, Chachoengsao, Thailand, on 5 December 2018, from 12:30 PM to 10:00 PM, UT. The obtained data were calculated using the photometry method to construct the light curve of each wavelength band and determine the minimum time. HJD 2458458.306 and HJD 2458458.144 are the minimum time of the primary and secondary eclipse, respectively. The data were used to plot the O-C curve. The upward parabolic curve means the period increases at the rate of 4.57× 10-3 seconds/year. The sinusoidal curve suggests that YY Eri might have a third body which is located at a distance of about 3.45 AU from the center of mass with an orbital period of 68.6 years.

show abstract

Section: Resultsmentioning

confidence: 68%

“…Solar mass in equation ( 4) comes from the study by Kim et al in 1998 [13]. If the orbital of the third body is the circle, the calculated mass of the third body is 0.34 Solar mass, corresponding to the studies of Ting et al in 2018 [10]. They calculated the range of third mass for the inclination of 30-90 degrees are 0.17 -0.36 Solar mass.…”

Section: Resultsmentioning

confidence: 97%

A Period Change Study of the Contact Binary System YY Eri

Pancharoen

Maithong

2022

ASEAN Sci Tech Rept

View full text Add to dashboard Cite

show abstract

The first photometric investigations of the G-type shallow contact binary IO Cnc

Liao

Xiao

et al. 2021

Res. Astron. Astrophys.

View full text Add to dashboard Cite

IO Cnc was classified to be a new G-type (G0) W UMa-type eclipsing binary system. Our first multicolor photometric solutions show that IO Cnc is a new W-subtype shallow contact binary with a fill-out factor of f = 16.1% and a low mass ratio of q = 3.12 (or 1/q = 0.32). During orbital period investigations, a cyclic variation and a downward parabolic variation with a rate of (−1.28 ± 0.43) × 10−7 d yr−1 was discovered in the observed–calculated (O − C) curve. The cyclic variation was analyzed by the light travel time effect (LTTE) via a potential red dwarf companion star, an orbital semi-major axis shorter than 4.88 ± 0.82 AU was obtained. Finally, we collect physical parameters of a sample of 50 G-type shallow contact binaries (f ≤ 20%), it is suggested that most of the G-type shallow contact binaries are undergoing a long-term and periodic orbital period changes, especially more systems show long-term decreases. The long-term orbital period decrease indicates that IO Cnc is in a mass transferring from the more massive component to the less massive one. With the long-term decrease of the orbital period, this shallow contact binary will evolve into a deeper contact one.

show abstract

Orbital period changes of the W UMa binary YY Eri

Cited by 2 publications

References 27 publications

A Period Change Study of the Contact Binary System YY Eri

A Period Change Study of the Contact Binary System YY Eri

The first photometric investigations of the G-type shallow contact binary IO Cnc

Contact Info

Product

Resources

About