1:1 orbital resonance of circumbinary planets
arXiv:1908.10395 · doi:10.1051/0004-6361/201936478
Abstract
The recent detection of the third planet in Kepler-47 has shown that binary stars can host several planets in circumbinary orbits. To understand the evolution of such systems we have performed two-dimensional hydrodynamic simulations of the circumbinary disc with two embedded planets for several Kepler systems. In two cases, Kepler-47 and -413, the planets are captured in a 1:1 mean-motion resonance at the planet parking position near the inner edge of the disc. The orbits are fully aligned, have mean eccentricities of about 0.25 to 0.30, and the planets are entangled in a horseshoe type of motion. Subsequent n-body simulations without the disc show that the configurations are stable. Our results point to the existence of a new class of stable resonant orbits around binary stars. It remains to be seen if such orbits exist in reality.
arXiv comment5 pages, accepted by A&A Letters
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- Searching for Small Circumbinary Planets I. The STANLEY Automated Algorithm and No New Planets in Existing Systems
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- Using planet migration and dust drift to weigh protoplanetary discs
- Circumbinary planets: migration, trapping in mean-motion resonances, and ejection
- Stability of coorbital planets around binaries
- On the Detection of Habitable Trojan Planets in the Kepler Circumbinary Systems
- The morphology of CSCha circumbinary disk suggesting the existence of a Saturn-mass planet