1:1 orbital resonance of circumbinary planets

Penzlin, Anna B. T.; Ataiee, Sareh; Kley, W.

doi:10.1051/0004-6361/201936478

Cited by 13 publications

(12 citation statements)

References 19 publications

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“…Even though the gap in the middle panel is only partially opened it already leads to a reduction in orbital eccentricity of the cavity and planet. However, in both cases the planet is still too well embedded in the disc and influenced by its dynamics such that the orbit of the planet and the cavity are fully aligned and precess at the same rate, as also observed in Kley et al (2019); Penzlin et al (2019). For an even lower viscosity of α = 10 −4 (right panel) the planet opens a deeper gap that erases directly the disc driven planet dynamics and allows the planet to reach a stable orbit inside the cavity.…”

Section: The Influence Of Viscositymentioning

confidence: 68%

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Parking planets in circumbinary discs

Penzlin,

Kley,

Nelson

2020

Preprint

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The Kepler space mission discovered about a dozen planets orbiting around binary stars systems. Most of these circumbinary planets lie near their instability boundaries at about 3 to 5 binary separations. Past attempts to match these final locations through an inward migration process were only successful for the Kepler-16 system. Here, we study 10 circumbinary systems and try to match the final parking locations and orbital parameters of the planets with a disc driven migration scenario. We performed 2D locally isothermal hydrodynamical simulations of circumbinary discs with embedded planets and followed their migration evolution using different values for the disc viscosity and aspect ratio. We found that for the six systems with intermediate binary eccentricities (0.1 ≤ e bin ≤ 0.21) the final planetary orbits matched the observations closely for a single set of disc parameters, specifically a disc viscosity of α = 10 −4 , and an aspect ratio of H/r ∼ 0.04. For these systems the planet masses were large enough to open at least a partial gap in their discs as they approach the binary, forcing the discs to become circularized and allowing for further migration towards the binary, leading to good agreement with the observed planetary orbital parameters. For systems with very small or large binary eccentricities the match was not as good because the very eccentric discs and large inner cavities in these cases prevented close-in planet migration. In test simulations with higher than observed planet masses better agreement could be found for those systems. The good agreement for 6 out of the 10 modelled systems, where the relative difference between observed and simulated final planet orbit is ≤ 10%, strongly supports the idea that planet migration in the disc brought the planets to their present locations.

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Section: The Influence Of Viscositymentioning

confidence: 68%

“…Possibly, multiple planets are present in some of the systems that are even slightly inclined so that we see only one of the planets. In Penzlin et al (2019) we showed that a secondary planet does not change the orbit of the first one significantly, hence we did not include multi-planet simulations here.…”

Section: Discussion and Summarymentioning

confidence: 99%

Parking planets in circumbinary discs

Penzlin,

Kley,

Nelson

2020

Preprint

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“…The models by these authors also show that the formation of a stable co-orbital ring is possible for the Kepler-16 system. Similarly, Penzlin et al (2019) found that co-orbital planets can have stable configurations in the Kepler-47 system. Most recently, Leleu et al (2019) studied the dynamics of a pair of migrating co-orbital planets and showed that depending on the mass-ratio and eccentricities of the planets, and also depending on the type and strength of dissipative forces, the two planets may reside at stable Lagrangian points, may undergo horseshoe orbits, or may scatter out of the system.…”

Section: Introductionmentioning

confidence: 81%

On the Detection of Habitable Trojan Planets in the Kepler Circumbinary Systems

Sudol,

Haghighipour

2021

Preprint

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We present the results of a study of the prospect of detecting habitable Trojan planets in the Kepler Habitable Zone circumbinary planetary systems (Kepler-16, -47, -453, -1647(Kepler-16, -47, -453, - , -1661. We integrated the orbits of 10,000 separate N-body systems (N = 4, 6), each with a one Earth-mass body in a randomly selected orbit near the L 4 and L 5 Lagrangian points of the host HZ circumbinary planet. We find that stable Trojan planets are restricted to a narrow range of semimajor axes in all five systems and limited to small eccentricities in Kepler-16, -47, and -1661. To assess the prospect of the detection of these habitable Trojan planets, we calculated the amplitudes of the variations they cause in the transit timing of their host bodies. Results show that the mean amplitudes of the transit timing variations (TTVs) correlate with the mass of the transiting planet and range from 70 minutes for Kepler-16b to 390 minutes for Kepler-47c. Our analysis indicates that the TTVs of the circumbinary planets caused by these Trojan bodies fall within the detectable range of timing precision obtained from the Kepler telescope's long-cadence data. The latter points to Kepler data as a viable source to search for habitable Trojan planets.

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“…14 we can rule out exterior planets larger than 6R ⊕ , and for many of the systems this limit is significantly smaller. We also rule out the commensurate planets predicted by Penzlin et al (2019), unless they are significantly smaller than the detected planet at that period.…”

Section: Searching For Additional Planets In Known Systemsmentioning

confidence: 99%

“…Under certain conditions co-orbital circumbinary planets (i.e. a 1:1 resonance) are predicted by Penzlin et al (2019), to which the algorithm is also sensitive.…”

Section: Searching For Additional Planets In Known Systemsmentioning

confidence: 99%

Searching for Small Circumbinary Planets I. The STANLEY Automated Algorithm and No New Planets in Existing Systems

Martin,

Fabrycky

2021

Preprint

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No circumbinary planets have been discovered smaller than 3R ⊕ , yet planets of this small size comprise over 75% of the discoveries around single stars. The observations do not prove the nonexistence of small circumbinary planets, but rather they are much harder to find than around single stars, because their transit timing variations are much larger than the transit durations. We present Stanley: an automated algorithm to find small circumbinary planets. It employs custom methods to detrend eclipsing binary light curves and stack shallow transits of variable duration and interval using N-body integrations. Applied to the Kepler circumbinaries, we recover all known planets, including the three planets of Kepler-47, and constrain the absence of additional planets of similar or smaller size. We also show that we could have detected < 3R ⊕ planets in half of the known systems. Our work will ultimately be applied to a broad sample of eclipsing binaries to (hopefully) produce new discoveries, and derive a circumbinary size distribution which can be compared to that for single stars.

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1:1 orbital resonance of circumbinary planets

Cited by 13 publications

References 19 publications

Parking planets in circumbinary discs

Parking planets in circumbinary discs

On the Detection of Habitable Trojan Planets in the Kepler Circumbinary Systems

Searching for Small Circumbinary Planets I. The STANLEY Automated Algorithm and No New Planets in Existing Systems

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