Dynamical Origin of Extrasolar Planet Eccentricity Distribution

Abstract

We explore the possibility that the observed eccentricity distribution of extrasolar planets arose through planet-planet interactions, after the initial stage of planet formation was complete. Our results are based on ~3250 numerical integrations of ensembles of randomly constructed planetary systems, each lasting 100 Myr. We find that for a remarkably wide range of initial conditions the eccentricity distributions of dynamically active planetary systems relax towards a common final equilibrium distribution, well described by the fitting formula dn ~ e exp[-1/2 (e/0.3)^2] de. This distribution agrees well with the observed eccentricity distribution for e > 0.2, but predicts too few planets at lower eccentricities, even when we exclude planets subject to tidal circularization. These findings suggest that a period of large-scale dynamical instability has occurred in a significant fraction of newly formed planetary systems, lasting 1--2 orders of magnitude longer than the ~1 Myr interval in which gas-giant planets are assembled. This mechanism predicts no (or weak) correlations between semimajor axis, eccentricity, inclination, and mass in dynamically relaxed planetary systems. An additional observational consequence of dynamical relaxation is a significant population of planets (>10%) that are highly inclined (>25deg) with respect to the initial symmetry plane of the protoplanetary disk; this population may be detectable in transiting planets through the Rossiter-McLaughlin effect.

Accepted to ApJ, conclusions updated to reflect the current observational constraints

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• Direct Imaging of Irregular Satellite Disks in Scattered Light
• Dynamical orbital evolution scenarios of the wide-orbit eccentric planet HR 5183b
• Setting the Stage: The Early History of the Solar System
• Instability from high-order resonant chains in wide-separation massive planet systems
• 14 Her: a likely case of planet-planet scattering
• OGLE-2019-BLG-0468Lb,c: two microlensing giant planets around a G-type star
• Role of Dynamical Research in the Detection and Characterization of Exoplanets
• Longterm Stability of Planetary Systems formed from a Transitional Disk
• Inflated Eccentric Migration of evolving gas giants II: Numerical methodology and basic concepts
• The effect of late giant collisions on the atmospheres of protoplanets and the formation of cold sub-Saturns
• Effects of Magnetic Braking and Tidal Friction on Hot Jupiters