An empirically derived three-dimensional Laplace resonance in the Gliese 876 planetary system

Nelson, Benjamin E.; Robertson, Paul; Payne, Matthew J.; Pritchard, Seth; Deck, Katherine M.; Ford, Eric B.; Wright, Jason T.; Isaacson, Howard

doi:10.1093/mnras/stv2367

Cited by 82 publications

(49 citation statements)

References 91 publications

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“…Although the system also houses a much smaller inner planet, it is located very close to the star and with negligible gravitational interactions with the other members. The resonance offset for GJ876 is larger than observed in other cases with orbital period ratios of ∼ 2.02 and ∼ 2.04 (Nelson et al 2016). The GJ876 system has been shown to be significantly chaotic (Martí et al 2013), although stable for time spans comparable to the age of the system.…”

Section: Population Near the 2:1 And 3:2 Mmrsmentioning

confidence: 53%

Planetary migration and the origin of the 2:1 and 3:2 (near)-resonant population of close-in exoplanets

Ramos

Charalambous

Benítez-Llambay

et al. 2017

A&A

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We present an analytical and numerical study of the orbital migration and resonance capture of fictitious two-planet systems with masses in the super-Earth range undergoing Type-I migration. We find that, depending on the flare index and proximity to the central star, the average value of the period ratio, P 2 /P 1 , between both planets may show a significant deviation with respect to the nominal value. For planets trapped in the 2:1 commensurability, offsets may reach values on the order of 0.1 for orbital periods on the order of 1 day, while systems in the 3:2 mean-motion resonance (MMR) show much smaller offsets for all values of the semimajor axis. These properties are in good agreement with the observed distribution of near-resonant exoplanets, independent of their detection method. We show that 2:1-resonant systems far from the star, such as HD82943 and HR8799, are characterized by very small resonant offsets, while higher values are typical of systems discovered by Kepler with orbital periods approximately a few days. Conversely, planetary systems in the vicinity of the 3:2 MMR show little offset with no significant dependence on the orbital distance. In conclusion, our results indicate that the distribution of Kepler planetary systems around the 2:1 and 3:2 MMR are consistent with resonant configurations obtained as a consequence of a smooth migration in a laminar flared disk, and no external forces are required to induce the observed offset or its dependence with the commensurability or orbital distance from the star.

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Section: Population Near the 2:1 And 3:2 Mmrsmentioning

confidence: 53%

Planetary migration and the origin of the 2:1 and 3:2 (near)-resonant population of close-in exoplanets

Ramos

Charalambous

Benítez-Llambay

et al. 2017

A&A

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show abstract

“…We assess the evidence for both models by computing the fully marginalized likelihood (i.e., Bayesian evidence) of the population-level parameters using an importance sampling algorithm (Nelson et al 2016). For the RV+Kepler data, the Bayes factor p( d|M 2 )/p( d|M 1 ) is ≈0.1.…”

Section: Resultsmentioning

confidence: 99%

Evidence for Two Hot-Jupiter Formation Paths

Nelson¹,

Rasio²

2017

Self Cite

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Disk migration and high-eccentricity migration are two well-studied theories to explain the formation of hot Jupiters. The former predicts that these planets can migrate up until the planet-star Roche separation (a Roche ) and the latter predicts they will tidally circularize at a minimum distance of 2a Roche . Considering long-running radial velocity and transit surveys have identified a couple hundred hot Jupiters to date, we can revisit the classic question of hot Jupiter formation in a data-driven manner. We approach this problem using data from several exoplanet surveys (radial velocity, Kepler, HAT, and WASP) allowing for either a single population or a mixture of populations associated with these formation channels, and applying a hierarchical Bayesian mixture model of truncated power laws of the form x γ−1 to constrain the population-level parameters of interest (e.g., location of inner edges, γ, mixture fractions). Within the limitations of our chosen models, we find the current radial velocity and Kepler sample of hot Jupiters can be well explained with a single truncated power law distribution with a lower cutoff near 2a Roche , a result that still holds after a decade, and γ = −0.51± 0.19 0.20 . However, the HAT and WASP data show evidence for multiple populations (Bayes factor ≈ 10 21 ). We find that 15 ± 9 6 % reside in a component consistent with disk migration (γ = −0.04± 0.53 1.27 ) and 85 ± 6 9 % in one consistent with high-eccentricity migration (γ = −1.38± 0.32 0.47 ). We find no immediately strong connections with some observed host star properties and speculate on how future exoplanet surveys could improve upon hot Jupiter population inference.

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“…For example, Jupiter's Galilean moons are known to be locked into a so-called three-body Laplacian resonance (i.e., 4:2:1 MMR) in our solar system. On the other hand, other evidences are found in the exoplanetary systems, in which three planets of the GJ 876 system (Marcy et al 2001;Rivera et al 2010;Batygin et al 2015;Nelson et al 2016) and Kepler-79 (KOI-152) (Steffen et al 2010;Wang et al 2012) are reported to be close to 4:2:1 MMR. In this work, we have provided substantial evidences on this from the simulations.…”

Section: The Emergence Of 4:2:1 Mmrs Only With Terrestrial Planetsmentioning

confidence: 98%

Terrestrial planet formation under migration: systems near the 4:2:1 mean motion resonance

Sun¹,

Ji²,

Wang³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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In this work, we extensively investigate the formation of near 4:2:1 mean motion resonances (MMRs) configuration by performing two sets of N-body simulations. We model the eccentricity damping, gas drag, type I and type II planetary migration of planetesimals, planetary embryos and giant planets in the first sets. For the simulations of giant planets with type II migration, the massive terrestrial planets, with a mass up to several Earth masses, are likely produced in the systems. We further show that by shepherding and/or scattering mechanisms through Jovian planet's type II migration, the terrestrial planets and giant planets in the systems can be evolved into a near 4:2:1 MMRs. Moreover, the models are applicable to the formation of Kepler-238 and 302 systems. In the second set, we study the 4:2:1 MMRs formation in the terrestrial planetary systems, where the planets undergo type I migration and eccentricity damping. By considering type I migration, ∼ 17.1% of the simulations indicate that terrestrial planets are evolved into 4:2:1 MMRs. However, this probability should depend on the initial conditions of planets. Hence, we conclude that both type I and type II migration can play a crucial role in close-in terrestrial planet formation.

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An empirically derived three-dimensional Laplace resonance in the Gliese 876 planetary system

Cited by 82 publications

References 91 publications

Planetary migration and the origin of the 2:1 and 3:2 (near)-resonant population of close-in exoplanets

Planetary migration and the origin of the 2:1 and 3:2 (near)-resonant population of close-in exoplanets

Evidence for Two Hot-Jupiter Formation Paths

Terrestrial planet formation under migration: systems near the 4:2:1 mean motion resonance

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