Is the orbital distribution of multiplanet systems influenced by pure three-planet resonances?

Cerioni, M.; Beaugé, C.; Gallardo, Tabaré

doi:10.1093/mnras/stac876

Cited by 8 publications

(6 citation statements)

References 39 publications

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“…In such a model, some planet pairs are "near-resonant" only coincidentally (reaching that state after the dissipation of the protoplanetary disk) and not as the consequence of resonant capture or damping. The actual fraction of systems that never experienced a post-gas instability in the overall sample is unclear: Izidoro et al (2021) suggest that no more than 5% remain stable and resonant, but it remains to be seen whether those results are consistent with the overabundance of threebody libration seen in the Kepler sample (Goldberg & Batygin 2021;Cerioni et al 2022). While basic modeling of the peaks in the period ratio distribution has had some success (e.g., Choksi & Chiang 2020;Ghosh & Chatterjee 2023), the results of this work illuminate a novel and stringent constraint that must be accounted for in a complete model of planet formation.…”

Section: Discussionmentioning

confidence: 99%

Dynamics and Origins of the Near-resonant Kepler Planets

Goldberg

Batygin

2023

ApJ

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Short-period super-Earths and mini-Neptunes encircle more than ∼50% of Sun-like stars and are relatively amenable to direct observational characterization. Despite this, environments in which these planets accrete are difficult to probe directly. Nevertheless, pairs of planets that are close to orbital resonances provide a unique window into the inner regions of protoplanetary disks, as they preserve the conditions of their formation, as well as the early evolution of their orbital architectures. In this work, we present a novel approach toward quantifying transit timing variations within multiplanetary systems and examine the near-resonant dynamics of over 100 planet pairs detected by Kepler. Using an integrable model for first-order resonances, we find a clear transition from libration to circulation of the resonant angle at a period ratio of ≈0.6% wide of exact resonance. The orbital properties of these systems indicate that they systematically lie far away from the resonant forced equilibrium. Cumulatively, our modeling indicates that while orbital architectures shaped by strong disk damping or tidal dissipation are inconsistent with observations, a scenario where stochastic stirring by turbulent eddies augments the dissipative effects of protoplanetary disks reproduces several features of the data.

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Section: Discussionmentioning

confidence: 99%

Dynamics and Origins of the Near-resonant Kepler Planets

Goldberg

Batygin

2023

ApJ

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“…The offsets observed in several planetary systems with respect to 2P-MMRs (e.g., Kepler-80, TOI-178) appear consistent with such an evolutionary route (e.g., MacDonald et al 2016;Leleu et al 2021), perhaps indicating that the resonant structure of small-mass planetary systems could have a stronger correlation to 3P-MMRs than to two-planet commensurabilities (Cerioni et al 2022). However, in no case was a capture reported in a first-order three-planet resonance, nor was such a configuration suggested as an evolutionary route due to tidal effects.…”

Section: Tidal Evolution Of the Six-planet Chainmentioning

confidence: 71%

“…Direct tidal interactions between the other planets and the star proved negligible, and thus their tidal parameters could not be constrained. Surprisingly, even the current offset of the outer pair n f /n g ; 3.3 can be explained by tidal evolution alone, indicating that perhaps other seemingly nonresonant systems may be dynamically affected by two-planet or three-planet commensurabilities, even more so than previously thought (e.g., Cerioni et al 2022).…”

Section: Discussionmentioning

confidence: 83%

“…On one hand, it has recently been argued that, even when lacking in pairwise commensurabilities, their distribution of orbital periods shows a correlation with the web of three-planet mean-motion resonances (3P-MMRs) (Cerioni et al 2022), suggesting a more complex resonant evolution than previously thought. On the other hand, planetary systems showing a high number of MMRs among their constituents are predominantly low-mass (e.g., etc.…”

Section: Introductionmentioning

confidence: 97%

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A Six-planet Resonance Chain in K2-138?

Cerioni,

Beaugé

2023

ApJ

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The K2-138 system hosts six planets and presents an interesting case study due to its distinctive dynamical structure. Its five inner planets are near a chain of 3/2 two-body mean-motion resonances, while the outermost body (planet g) is significantly detached, having a mean-motion ratio of n f/n g ∼ 3.3 with its closest neighbor. We show that the orbit of m g is actually consistent with the first-order three-planet resonance (3P-MMR) characterized by the relation 2n e − 4n f + 3n g = 0 and is the first time a pure first-order 3P-MMR has been found in a multiplanet system and tied to its current dynamical structure. Adequate values for the masses allow one to trace the dynamical history of the system from an initial capture in a six-planet chain (with n f/n g in a 3/1 resonance) up to its current configuration due to tidal interactions over the age of the star. The increase in resonance offset with semimajor axis, as well as its large value for n f/n g, can be explained by the slopes of the pure three-planet resonances in the mean-motion ratio plane. The triplets slide outward over these curves when the innermost pair is pulled apart by tidal effects, in a pantograph-like manner. The capture into the 3P-MMR is found to be surprisingly robust given similar masses for m g and m f, and it is possible that the same effect may also be found in other compact planetary systems.

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“…Recently, Cerioni et al (2022) analyzed from a statistical point of view the correlation between the observed distribution of compact low-mass multi-planet systems and the 2-and 3planet resonant structures and showed evidence in favor of a correlation with 3-planet resonances, which could be statistically explained by tides. Note also that the survival of Laplace-like resonances with tidal effects was newly investigated by Celletti et al (2021) for the satellite case (where the tides act in a different manner since the planets orbit a usually slow-rotating central star while the satellites orbit a fast-rotating central planet).…”

Section: Introductionmentioning

confidence: 99%

Tidal interactions shape period ratios in planetary systems with three-body resonant chains

Charalambous,

Teyssandier,

Libert

2023

A&A

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Aims. These last years several STIPs (Systems with Tightly packed Inner Planets) in the super-Earth mass regime have been discovered harboring chains of resonances. It is generally believed that planet pairs get trapped in MMR (mean-motion resonance) during the migration phase in the protoplanetary disk, while the tides raised by the host star provide a source of dissipation on very long timescales. In this work, we aim to study the departure from exact commensurabilities observed among the STIPs which harbor 3-planet resonances and analyze how tides play an important role in shaping the resonance offsets for the STIPs. Methods. We analyzed the resonance offsets between adjacent pairs for five multi-planetary systems, namely Kepler-80, Kepler-223, K2-138, TOI-178, and TRAPPIST-1, highlighting the existence of different trends in the offsets. On the one hand, we derived analytical estimates for the offsets, which confirm that the departure of the planetary pairs from the nominal MMRs are due to the 3-planet resonant dynamics. On the other hand, we performed N-body simulations including both orbital migration and tidal dissipation from the host star with simple prescriptions in order to test the effectiveness of this mechanism at shaping the observed trend in the offsets, focusing our study on the preservation of the resonant patterns in the different systems with the same general setup. Results. We found that the trends in the offsets of the five detected systems can be produced by tidal damping effects, regardless of the considered value for the tidal factor. It is a robust mechanism that relaxes the system towards equilibrium while efficiently moving it along 3-planet resonances, which induces the observed resonance offset for each planet pair. In addition, we showed that for Kepler-80, K2-138, and TOI-178, the amplitudes of the resonant offsets can also be reproduced with an appropriate tidal factor, for the estimated age of the systems.

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Is the orbital distribution of multiplanet systems influenced by pure three-planet resonances?

Cited by 8 publications

References 39 publications

Dynamics and Origins of the Near-resonant Kepler Planets

Dynamics and Origins of the Near-resonant Kepler Planets

A Six-planet Resonance Chain in K2-138?

Tidal interactions shape period ratios in planetary systems with three-body resonant chains

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