Resonance in the K2-19 system is at odds with its high reported eccentricities

Abstract

K2-19 hosts a planetary system composed of two outer planets, b and c, with size of $7.0\pm 0.2R_{\oplus }$ and $4.1\pm 0.2R_{\oplus }$ , and an inner planet, d, with a radius of $1.11\pm 0.05R_{\oplus }$. A recent analysis of Transit-Timing Variations (TTVs) suggested b and c are close to but not in 3:2 mean motion resonance (MMR) because the classical resonant angles circulate. Such an architecture challenges our understanding of planet formation. Indeed, planet migration through the protoplanetary disk should lead to a capture into the MMR. Here, we show that the planets are in fact, locked into the 3:2 resonance despite circulation of the conventional resonant angles and aligned periapses. However, we show that such an orbital configuration cannot be maintained for more than a few hundred million years due to the tidal dissipation experienced by planet d. The tidal dissipation remains efficient because of a secular forcing of the innermost planet eccentricity by planets b and c. While the observations strongly rule out an orbital solution where the three planets are on close to circular orbits, it remains possible that a fourth planet is affecting the TTVs such that the four planet system is consistent with the tidal constraints.

arXiv commentAccepted in MNRAS, replaced with published version

References in corpus (49)

• The K2 Mission: Characterization and Early results
• REBOUND: An open-source multi-purpose N-body code for collisional dynamics
• The Occurrence and Architecture of Exoplanetary Systems
• On detecting terrestrial planets with timing of giant planet transits
• DHP Framework: Digital Health Passports Using Blockchain -- Use case on international tourism during the COVID-19 pandemic
• EXOFAST: A fast exoplanetary fitting suite in IDL
• Architecture of Kepler's Multi-transiting Systems: II. New investigations with twice as many candidates
• Tidal dissipation in stars and giant planets
• Breaking the Chains: Hot Super-Earth systems from migration and disruption of compact resonant chains
• Extracting Planet Mass and Eccentricity From TTV data
• The California-Kepler Survey V. Peas in a Pod: Planets in a Kepler Multi-planet System are Similar in Size and Regularly Spaced
• Stellar Spin-Orbit Misalignment in a Multiplanet System
• Formation of planetary systems by pebble accretion and migration: How the radial pebble flux determines a terrestrial-planet or super-Earth growth mode
• Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc
• First order resonance overlap and the stability of close two planet systems
• Long-term tidal evolution of short-period planets with companions
• Formation of planetary systems by pebble accretion and migration: Growth of gas giants
• The Planet Nine Hypothesis
• KOI-142, the King of Transit Variations, is a Pair of Planets near the 2:1 Resonance
• Evolution of Giant Planets in Eccentric Disks
• How eccentric orbital solutions can hide planetary systems in 2:1 resonant orbits
• AMD-stability and the classification of planetary systems
• Investigations of approximate expressions for the transit duration
• Eleven Multi-planet Systems from K2 Campaigns 1 & 2 and the Masses of Two Hot Super-Earths
• Analytical Treatment of Planetary Resonances
• Obliquity-Driven Sculpting of Exoplanetary Systems
• Deformation and tidal evolution of close-in planets and satellites using a Maxwell viscoelastic rheology
• New families of symplectic splitting methods for numerical integration in dynamical astronomy
• Global m=1 modes and migration of protoplanetary cores in eccentric protoplanetary discs
• Growth of eccentric modes in disc-planet interactions
• Low-Eccentricity Migration of Ultra-Short Period Planets in Multi-Planet Systems
• A general model of resonance capture in planetary systems: First and second order resonances
• The TRAPPIST-1 system: Orbital evolution, tidal dissipation, formation and habitability
• Numerical and Analytical Modelling of Transit Time Variations
• Tidal dissipation in multi-planet systems and constraints to orbit-fitting
• Dissipation in planar resonant planetary systems
• Tidal dissipation in a homogeneous spherical body. I. Methods
• Bias and robustness of eccentricity estimates from radial velocity data
• The Orbit and Mass of the Third Planet in the Kepler-56 System
• AMD-stability in presence of first order Mean Motion Resonances
• Tidal dissipation in a homogeneous spherical body. II. Three examples: Mercury, Io, and Kepler-10 b
• One of the closest exoplanet pairs to the 3:2 Mean Motion Resonance: K2-19b \& c
• High order symplectic integrators for planetary dynamics and their implementation in REBOUND
• Resonance breaking due to dissipation in planar planetary systems
• An Integrable Model for the Dynamics of Planetary Mean Motion Resonances
• Formation of planetary systems by pebble accretion and migration: Hot super-Earth systems from breaking compact resonant chains
• The role of dissipative evolution for three-planet, near-resonant extrasolar systems
• K2-19b and c are in a 3:2 Commensurability but out of Resonance: A Challenge to Planet Assembly by Convergent Migration
• Characterization of the K2-19 Multiple-Transiting Planetary System via High-Dispersion Spectroscopy, AO Imaging, and Transit Timing Variations

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• Photodynamical analysis of the nearly resonant planetary system WASP-148: Accurate transit-timing variations and mutual orbital inclination
• Apsidal Alignment and Anti-Alignment of Planets in Mean-Motion Resonance: Disk-Driven Migration and Eccentricity Driving
• Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain
• Tides Tighten the Hycean Habitable Zone
• Not all roads lead to merger: AGN disc properties influence the interactions of highly unequal mass black holes
• Higher-Order Mean-Motion Resonances Can Form in Type-I Disk Migration
• Dynamical analysis of the 5:1 mean-motion resonance of the HD 202206 system
• Influence of Modeling Assumptions on the Inferred Dynamical State of Resonant Systems: A Case Study of the HD 45364 System