XZ And a semidetached asynchronous binary system

Manzoori, Davood

doi:10.1134/s1063773716050066

Cited by 4 publications

(9 citation statements)

References 22 publications

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“…which is about five times less than the ∆P/P = 1.45 × 10 −9 estimate of XZ And obtained by Manzoori (2016). The two and the three signal model results would have been nearly the same, but the one signal model M 1 and M 2 values would have given a completely wrong result (Table A16).…”

Section: Astrophysicsmentioning

confidence: 68%

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About ten stars orbit eclipsing binary XZ And

Jetsu

2020

Preprint

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A third body in an eclipsing binary system causes regular periodic changes in the observed (O) minus the computed (C) eclipse epochs. Fourth bodies have rarely been detected from the O-C data. We apply the new Discrete Chi-square Method (DCM) to the O-C data of the eclipsing binary XZ Andromedae. These data contain the periodic signatures of at least ten wide orbit stars (WOSs). Their orbital periods are between 1.6 and 91.7 years. Since no changes have been observed in the eclipses of XZ And during the past 127 years, the orbits of all these WOSs are most probably co-planar. We give detailed instructions of how the professional and the amateur astronomers can easily repeat all stages of our DCM analysis with an ordinary PC, as well as apply this method to the O-C data of other eclipsing binaries.

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Section: Astrophysicsmentioning

confidence: 68%

“…Borkovits et al, 2005). Such long-term changes have also been observed in XZ And (Chaplin, 2019;Demircan et al, 1995;Manzoori, 2016). When Hajdu et al (2019) studied O-C data of 80 000 EBs, they detected only four EB candidates that may have a fourth body.…”

Section: Introductionmentioning

confidence: 66%

About ten stars orbit eclipsing binary XZ And

Jetsu

2020

Preprint

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“…The only reason for such variations is the light-travel time effect induced by two companions in a possible mean-motion resonance. Manzoori (2016) carried out the photometric-spectroscopic analysis, and indicated that the orbital inclination of the eclipsing pair is 89.8 • , and the total masses of the eclipsing pair are m b = 3.12 M .…”

Section: Resultsmentioning

confidence: 99%

“…Selam and Demircan (1999) reported two periods of 36.79 and 126.35 yr for these two companions. Recently, Yang (2013) found only a quasi-cyclic period of 32.60 yr, while Manzoori (2016) obtained two periods, i.e., 23.3 and 34.8 yr.…”

Section: Introductionmentioning

confidence: 99%

A strange phenomenon in XZ Andromedae: two Keplerian periods with a 1:3 ratio

Yuan

Qian

2019

Res. Astron. Astrophys.

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Six mid-eclipse times of the eclipsing binary XZ And are obtained, which are analysed together with others collected from the literature. Two sets of cyclic variations with periods of 33.43 and 100.4 yr are found if a double-Keplerian model is used to fit the data. The 1:3 ratio of the periods suggests that both cyclic variations arise from dynamic motions of two companions rather than magnetic activity of the eclipsing pair. According to the double-Keplerian model, the companions have the masses of ∼ 1.32M and ∼ 1.33M ,respectively. Comparing the total masses of the eclipsing pair of 3.12M , it is obvious that XZ And is a general N-body system. The strong gravitational perturbation between two companions invalidates the double-Keplerian model. It is strange that two Keplerian periods with a 1:3 ratio are derived from the best fits with the inappropriate model. The illogical, but interesting phenomena also appear in other two Algol systems, suggesting that our discoveries deserve attention from astronomers.

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“…where m 1 and m 2 are the masses of EB (Wolf et al 1999;Zasche & Wolf 2007;Manzoori 2016;Esmer et al 2021).…”

Section: Third Body O-c Changesmentioning

confidence: 99%

Say Hello to Algol's New Companion Candidates

Jetsu

2021

ApJ

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Constant orbital period ephemerides of eclipsing binaries give the computed eclipse epochs (C). These ephemerides based on the old data can not accurately predict the observed future eclipse epochs (O). Predictability can be improved by removing linear or quadratic trends from the O-C data. Additional companions in an eclipsing binary system cause light-time travel effects that are observed as strictly periodic O-C changes. Recently, Hajdu et al. ( 2019) estimated that the probability for detecting the periods of two new companions from the O-C data is only 0.00005. We apply the new Discrete Chisquare Method (DCM) to 236 years of O-C data of the eclipsing binary Algol (β Persei). We detect the tentative signals of at least five companion candidates having periods between 1.863 and 219.0 years. The weakest one of these five signals does not reveal a "new" companion candidate, because its 680.4 ± 0.4 days signal period differs only 1.4σ from the well-known 679.85 ± 0.04 days orbital period of Algol C. We detect these same signals also from the first 226.2 years of data, and they give an excellent prediction for the last 9.2 years of our data. The orbital planes of Algol C and the new companion candidates are probably co-planar, because no changes have been observed in Algol's eclipses. The 2.867 days orbital period has been constant since it was determined by Goodricke (1783).

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XZ And a semidetached asynchronous binary system

Cited by 4 publications

References 22 publications

About ten stars orbit eclipsing binary XZ And

About ten stars orbit eclipsing binary XZ And

A strange phenomenon in XZ Andromedae: two Keplerian periods with a 1:3 ratio

Say Hello to Algol's New Companion Candidates

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