TOI-216: Resonant Constraints on Planet Migration

@article{Nesvorn2022TOI216RC,
  title={TOI-216: Resonant Constraints on Planet Migration},
  author={David Nesvorn{\'y} and Ondřej Chrenko and Mario Flock},
  journal={The Astrophysical Journal},
  year={2022},
  volume={925}
}
TOI-216 is a pair of close-in planets with orbits deep in the 2:1 mean motion resonance. The inner Neptune-class planet (TOI-216b) is near 0.12 au (orbital period P b ≃ 17 days) and has a substantial orbital eccentricity (e b ≃ 0.16) and large libration amplitude (A ψ ≃ 60°) in the resonance. The outer planet (TOI-216c) is a gas giant on a nearly circular orbit. We carry out N-body simulations of planet migration in a protoplanetary gas disk to explain the orbital configuration of TOI-216… 
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References

SHOWING 1-10 OF 95 REFERENCES

TOI-216b and TOI-216 c: Two Warm, Large Exoplanets in or Slightly Wide of the 2:1 Orbital Resonance

Warm, large exoplanets with 10–100 day orbital periods pose a major challenge to our understanding of how planetary systems form and evolve. Although high eccentricity tidal migration has been

Stability of resonant configurations during the migration of planets and constraints on disk-planet interactions

We study the stability of mean-motion resonances (MMR) between two planets during their migration in a protoplanetary disk. We use an analytical model of resonances, and describe the effect of the

Radial Migration of Gap-opening Planets in Protoplanetary Disks. II. The Case of a Planet Pair

When two planets are born in a protoplanetary disk, they may enter into mean-motion resonance as a consequence of convergent planetary migration. The formation of mean-motion resonances is important

A Pair of Resonant Planets Orbiting GJ 876

Precise Doppler measurements during 6 yr from the Lick and Keck observatories reveal two planets orbiting GJ 876 (M4V). The orbital fit yields companion masses of M sin i = 0.56 and 1.89 MJ, orbital

A resonant pair of warm giant planets revealed by TESS

We present the discovery of a pair of transiting giant planets using four sectors of TESS photometry. TOI-216 is a 0.87 M⊙ dwarf orbited by two transiters with radii of 8.2 and 11.3 R⊕, and periods

OVERSTABLE LIBRATIONS CAN ACCOUNT FOR THE PAUCITY OF MEAN MOTION RESONANCES AMONG EXOPLANET PAIRS

We assess the multi-planet systems discovered by the Kepler satellite in terms of current ideas about orbital migration and eccentricity damping due to planet–disk interactions. Our primary focus is

Modeling Radial Velocity Data of Resonant Planets to Infer Migration Histories

A number of giant-planet pairs with period ratios ≲2 discovered by the radial velocity (RV) method may reside in mean motion resonances. Convergent orbital migration and resonant capture at the time

Radial Migration of Gap-opening Planets in Protoplanetary Disks. I. The Case of a Single Planet

A large planet orbiting a star in a protoplanetary disk opens a density gap along its orbit due to the strong disk–planet interaction and migrates with the gap in the disk. It is expected that in the

Formation of a planetary Laplace resonance through migration in an eccentric disk

Context. Orbital mean motion resonances in planetary systems originate from dissipative processes in disk-planet interactions that lead to orbital migration. In multi-planet systems that host giant

Toward a new paradigm for Type II migration

Context. Giant planets open gaps in their protoplanetary and subsequently suffer so-called type II migration. Schematically, planets are thought to be tightly locked within their surrounding disks,
...