Resonances of Multiple Exoplanets and Implications for Their Formation

Abstract

Among $\sim 160$ of the multiple exoplanetary systems confirmed, about $30\%$ of them have neighboring pairs with a period ratio $\le 2$. A significant fraction of these pairs are around mean motion resonance (MMR), more interestingly, peak around 2:1 and 3:2, with a clear absence of more closely packed MMRs with period ratios less than 4:3, regardless of planet masses. Here we report numerical simulations demonstrating that such MMR behavior places important constraints on the disk evolution stage out of which the observed planets formed. Multiple massive planets (with mass $\ge 0.8$ $M_{\mathrm{Jup}}$) tend to end up with a 2:1 MMR mostly independent of the disk masses but low-mass planets (with mass $\le 30$ $M_{\oplus }$) can have MMRs larger than 4:3 only when the disk mass is quite small, suggesting that the observed dynamical architecture of most low-mass-planet pairs was established late in the disk evolution stage, just before it was dispersed completely.

arXiv comment5 pages, 5 figures, accepted for publication in ApJ Letters

References in corpus (23)

• Planetary Candidates Observed by Kepler, III: Analysis of the First 16 Months of Data
• Architecture and Dynamics of Kepler's Candidate Multiple Transiting Planet Systems
• A Closely-Packed System of Low-Mass, Low-Density Planets Transiting Kepler-11
• A torque formula for non-isothermal Type I planetary migration - II. Effects of diffusion
• A torque formula for non-isothermal Type I planetary migration - I. Unsaturated horseshoe drag
• A comparative study of disc-planet interaction
• Accretion in the Rho-Oph pre-main sequence stars
• Almost All of Kepler's Multiple Planet Candidates are Planets
• Toward a Deterministic Model of Planetary Formation VII: Eccentricity Distribution of Gas Giants
• Overstable Librations can account for the Paucity of Mean Motion Resonances among Exoplanet Pairs
• Post-Oligarchic Evolution of Protoplanetary Embryos and the Stability of Planetary Systems
• Evolution of Planetary Systems in Resonance
• Type I Planet Migration in Nearly Laminar Disks
• On the migration of a system of protoplanets
• Assembling the Building Blocks of Giant Planets around Intermediate Mass Stars
• Condition for Capture into First-order Mean Motion Resonances and Application to Constraints on Origin of Resonant Systems
• The Importance of Disk Structure in Stalling Type I Migration
• Are the Kepler Near-Resonance Planet Pairs due to Tidal Dissipation?
• On the 2:1 Orbital Resonance in the HD 82943 Planetary System
• Eccentricity Trap: Trapping of Resonantly Interacting Planets near the Disk Inner Edge
• A Population of Very-Hot Super-Earths in Multiple-Planet Systems Should be Uncovered by Kepler
• The GJ 876 Planetary System -- A Progress Report
• Characterizing the Orbital and Dynamical State of the HD 82943 Planetary System With Keck Radial Velocity Data

Cited by in corpus (11)

• First Results from High Angular Resolution ALMA Observations Toward the HL Tau Region
• Modeling Dust Emission of HL Tau Disk Based on Planet-Disk Interactions
• First versus second generation planet formation in post common envelope binary (PCEB) planetary systems
• Terrestrial Planet Formation in the Presence of Migrating Super-earths
• One of the closest exoplanet pairs to the 3:2 Mean Motion Resonance: K2-19b \& c
• Migration and Growth of Protoplanetary Embryos I: Convergence of Embryos in Protoplanetary Disks
• Migration of Planets Into and Out of Mean Motion Resonances in Protoplanetary Disks: Analytical Theory of Second-Order Resonances
• Migration and Growth of Protoplanetary Embryos II: Emergence of Proto-Gas-Giants Cores versus Super Earths' Progenitor
• Migration of Planets Into and Out of Mean Motion Resonances in Protoplanetary Discs: Overstability of Capture and Nonlinear Eccentricity Damping
• Terrestrial Planets Formation under Migration: the Systems near 4:2:1 Mean Motion Resonance
• The scattering outcomes of Kepler circumbinary planets: planet mass ratio