Cyclic period changes and the light-time effect in eclipsing binaries: A low-mass companion around the system VV Ursae Majoris

Tanriver, Mehmet

doi:10.1016/j.newast.2014.09.008

Cited by 4 publications

(1 citation statement)

References 15 publications

(6 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…where i is the inclination of the orbital plane of the third body, m 1 is the mass of primary [m ⊙ ], q = m 2 /m 1 is the dimensionless mass ratio of secondary and primary, m 3 is the mass of the third body [m ⊙ ], a = A/2 is half of the peak the peak amplitude of O-C modulation caused by the third body [d], and p 3 is the period of the modulations caused by the third body [y] (Borkovits and Hegedues, 1996;Tanrıver, 2015;Yang et al, 2016). We use the masses m 1 = 3.2m ⊙ and m 2 = 1.3m ⊙ (Demircan et al, 1995, A4 IV + G5 IV).…”

Section: Astrophysicsmentioning

confidence: 99%

About ten stars orbit eclipsing binary XZ And

Jetsu

2020

Preprint

View full text Add to dashboard Cite

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.

show abstract

Section: Astrophysicsmentioning

confidence: 99%

About ten stars orbit eclipsing binary XZ And

Jetsu

2020

Preprint

View full text Add to dashboard Cite

show abstract

Photometric Studies of Two Neglected Eclipsing Binaries AX Cassiopeia and V1107 Cassiopeia with Possibly Additional Companions

Yang

et al. 2016

PASP

View full text Add to dashboard Cite

New photometry for two eclipsing binaries, AX Cas and V1107 Cas, was carried out during the 2014-2015 observing season. With an updated version of the W-D program, photometric solutions were simultaneously derived from BV light curves. Results indicate that AX Cas is a semi-detached binary with a mass ratio of q 0.400 0.003for V1107 Cas, respectively. From 26 EB/EW binaries with only cyclic variations, we derived the relation between periods and total masses, indicating that mass loss from the system occurs from the semi-detached configuration to the contact case. The cyclic oscillations for 22 sample stars (including AX Cas and V1107 Cas) may be attributed to third bodies. Additional companions could remove angular momentum from the central systems, which may play a key role in the evolutionary process.

show abstract

Evolutionary inference and statistical constraints on Algols including SD2-type near contact binaries

Wang

Zhu

Yue

2022

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Algol-type binaries (Algols) have aroused extensive interests due to the idiosyncratic evolutionary stages of both components. To better understand the evolutionary properties of such characteristic population, we collected mostly double-lined samples and performed systematic work concentrated on their physical constraints. It is found that orbital period cut-off for the OB and AF type Algols are P(OB) >0.482 d, P(AF) >0.358 d; constraints on mean density and surface gravity of the secondary components are $\overline{\rho }_2$(OB) < 0.144 ρ⊙, $\overline{\rho }_2$(AF) < 0.26 ρ⊙, log g2(OB) < 4.719 cgs and log g2(AF) < 4.517 cgs. Limitations of a(OB) >3.48 R⊙ and a(AF) >2.29 R⊙ have been deduced from the a - P relation. Moreover, statistical analysis of secular period changes reveal that Algols with higher f1 and relevant shorter period generally show weak period change. It hints that there is some connections between f1 and orbital evolution. Systems with lower f1 have the chance to evolve from classic Algols to SD2-type near contact binaries; systems with higher f1 obey the evolutionary channel from SD2-type near contact binaries to contact binaries. However, it seems that SD2-type near contact binaries could not evolve toward classic Algols. As a natural lab Algols are producing peculiar stellar experimental samples via complicated astrophysical processes, which will enhance our understanding on the physical properties and evolution of such binary populations.

show abstract

Cyclic period changes and the light-time effect in eclipsing binaries: A low-mass companion around the system VV Ursae Majoris

Cited by 4 publications

References 15 publications

About ten stars orbit eclipsing binary XZ And

About ten stars orbit eclipsing binary XZ And

Photometric Studies of Two Neglected Eclipsing Binaries AX Cassiopeia and V1107 Cassiopeia with Possibly Additional Companions

Evolutionary inference and statistical constraints on Algols including SD2-type near contact binaries

Contact Info

Product

Resources

About