Evidence for a planetary mass third body orbiting the binary star KIC 5095269

Getley, A. K.; Carter, B.; King, Rachel; O'Toole, S. J.

doi:10.1093/mnras/stx604

Cited by 44 publications

(20 citation statements)

References 26 publications

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“…the eclipse timing fit, the models reproducing the O-C effects and the stability of the system) all strongly point to the existence and viability of this as a planetary candidate. The third body in this system is in an orbit with an inclination of 105°and with a configuration similar to that of the planetary mass third body found orbiting KIC5095269 (Getley et al 2017). It is also further evidence that low mass objects can have a significant effect on the orbital properties of the host stars and also that, for at least some orbital configurations, eclipse timing variations are a valid way of detecting planetary mass bodies.…”

Section: Kic7821010supporting

confidence: 69%

“…The Kepler data were used to produce O -C diagrams for detached eclipsing binaries to study eclipse timing variations. We created a C++ program, called or , to determine the mid-eclipse times of as many primary and secondary eclipses in the Kepler detached binary systems as possible (see Getley et al 2017).…”

Section: Methodsmentioning

confidence: 99%

“…The high precision observations from Kepler enable eclipse time studies to be performed where variations in the eclipse times of binary stars can be used to detect third bodies (e.g. Getley et al 2017;Borkovits et al 2016). Binary stars that have orbits aligned with the Earth will eclipse each other and detached and isolated binary stars should have eclipses that occur at predictable intervals.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Stability of planetary, single M dwarf, and binary star companions to Kepler detached eclipsing binaries and a possible five-body system

Getley

Carter

King

et al. 2020

Monthly Notices of the Royal Astronomical Society

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In this study we identify 11 Kepler systems (KIC 5255552, 5653126, 5731312, 7670617, 7821010, 8023317, 10268809, 10296163, 11519226, 11558882 and 12356914) with a ”flip-flop” effect in the eclipse timing variations O-C diagrams of the systems, report on what these systems have in common and whether these systems are dynamically stable. These systems have previously reported high eccentric binary stars with highly eccentric third bodies/outer companions. We find that all of the additional bodies in the system are dynamically stable for the configurations previously reported and are therefore likely to exist as described. We also provide additional evidence of KIC5255552 being a quadruple star system comprised of an eclipsing binary pair and non-eclipsing binary pair with the possibility of a fifth body in the system. With the advent of the NASA TESS exoplanet survey, its precision photometric monitoring offers an opportunity to help confirm more local eclipsing binary star companions, including planets.

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Section: Kic7821010supporting

confidence: 69%

Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Stability of planetary, single M dwarf, and binary star companions to Kepler detached eclipsing binaries and a possible five-body system

Getley

Carter

King

et al. 2020

Monthly Notices of the Royal Astronomical Society

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show abstract

“…Kepler-34b with a mass of 0.22 M J orbits an eclipsing binary star system (Kepler-34) that has an orbital eccentricity of 0.52 (Welsh et al 2012;Kley & Haghighipour 2015). The moderately eccentric Email: chenc21@unlv.nevada.edu (e = 0.26) binary KIC 5095269 hosts a circumbinary planet KIC 5095269b (Getley et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Orbital dynamics of circumbinary planets

Chen

Franchini

Lubow

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We investigate the dynamics of a nonzero mass, circular orbit planet around an eccentric orbit binary for various values of the binary eccentricity, binary mass fraction, planet mass, and planet semi-major axis by means of numerical simulations. Previous studies investigated the secular dynamics mainly by approximate analytic methods. In the stationary inclination state, the planet and binary precess together with no change in relative tilt. For both prograde and retrograde planetary orbits, we explore the conditions for planetary orbital libration versus circulation and the conditions for stationary inclination. As was predicted by analytic models, for sufficiently high initial inclination, a prograde planet's orbit librates about the stationary tilted state. For a fixed binary eccentricity, the stationary angle is a monotonically decreasing function of the ratio of the planet-to-binary angular momentum j. The larger j, the stronger the evolutionary changes in the binary eccentricity and inclination. We also calculate the critical tilt angle that separates the circulating from the librating orbits for both prograde and retrograde planet orbits. The properties of the librating orbits and stationary angles are quite different for prograde versus retrograde orbits. The results of the numerical simulations are in very good quantitative agreement with the analytic models. Our results have implications for circumbinary planet formation and evolution.

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“…Another example is V893 Scorpi where observed variations of the eclipse period of 10.2 years are interpreted as a light travel time effect caused by the presence of a giant planet with 9.5 M J (Bruch 2014). Finally DP Leonis (Beuermann et al 2011), HW Vir (Lee et al 2009), NN Ser (Beuermann et al 2010), NY Virginis (Qian et al 2012a), RR Caeli (Qian et al 2012b) and KIC 5095269 (Getley et al 2017) are part of this small group of post-CE binaries suspected to possess planets.…”

Section: Introductionmentioning

confidence: 99%

Revisiting Fs Aurigae and Its Triple Cataclysmic Variable System Hypothesis

Chavez¹,

Avilés²,

Georgakarakos

et al. 2020

RMxAA

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A very long term variability (VLPP), with period of 875 days, was observed in the long-term light curve of FS Aurigae (FS Aur) in 2011. This periodicity was calculated over 6 cycles. We re-examined the periodicity with new observations over the past 5 yrs. A total of 18 years of observations confirm the hypothesis of a third body perturbing in a secular way the cataclysmic variable (CV). Improvements to the model such as eccentric and inclined orbits for the third body and a binary post-Newtonian correction are considered. We confirm the VLPP of FS Aur and find the new period of 857 ± 78 days. The secular perturbations are most efficient when the mass of the third body is M₃≈ 29MJ, much less than the 50MJ reported in 2011. We estimate the effect of the third body on the mass transfer rate and on the brightness of the system. We consider alternative scenarios for the VLPP. New data and analysis support the hypothesis that FS Aur is a CV in a triple system.

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Evidence for a planetary mass third body orbiting the binary star KIC 5095269

Cited by 44 publications

References 26 publications

Stability of planetary, single M dwarf, and binary star companions to Kepler detached eclipsing binaries and a possible five-body system

Stability of planetary, single M dwarf, and binary star companions to Kepler detached eclipsing binaries and a possible five-body system

Orbital dynamics of circumbinary planets

Revisiting Fs Aurigae and Its Triple Cataclysmic Variable System Hypothesis

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