Origin of the orbital architecture of the giant planets of the Solar System

  title={Origin of the orbital architecture of the giant planets of the Solar System},
  author={Kleomenis Tsiganis and Rodney Gomes and Alessandro Morbidelli and Harold F. Levison},
Planetary formation theories suggest that the giant planets formed on circular and coplanar orbits. The eccentricities of Jupiter, Saturn and Uranus, however, reach values of 6 per cent, 9 per cent and 8 per cent, respectively. In addition, the inclinations of the orbital planes of Saturn, Uranus and Neptune take maximum values of ∼2 degrees with respect to the mean orbital plane of Jupiter. Existing models for the excitation of the eccentricity of extrasolar giant planets have not been… 
Constructing the secular architecture of the solar system. I. The giant planets
Using numerical simulations, we show that smooth migration of the giant planets through a planetesimal disk leads to an orbital architecture that is inconsistent with the current one: the resulting
Origin of the obliquities of the giant planets in mutual interactions in the early Solar System
The present obliquities of the giant planets were probably achieved when Jupiter and Saturn crossed the 1:2 orbital resonance during a specific migration process, and the existence of the regular satellites does not represent a problem in this model because, although they formed soon after the planetary formation, they can follow the slow evolution of the equatorial plane it produces.
Young Solar System's Fifth Giant Planet?
Studies of solar system formation suggest that the solar system's giant planets formed and migrated in the protoplanetary disk to reach the resonant orbits with all planets inside ∼15 AU from the
The fragility of the terrestrial planets during a giant-planet instability
Many features of the outer solar system are replicated in numerical simulations if the giant planets undergo an orbital instability that ejects one or more ice giants. During this instability,
Dynamics of the Giant Planets of the Solar System in the Gaseous Protoplanetary Disk and Their Relationship to the Current Orbital Architecture
We study the orbital evolution of the four giant planets of our solar system in a gas disk. Our investigation extends the previous works by Masset & Snellgrove and Morbidelli & Crida, which focused
The eccentricity distribution of giant planets and their relation to super-Earths in the pebble accretion scenario
Observations of the population of cold Jupiter planets ($r>$1 AU) show that nearly all of these planets orbit their host star on eccentric orbits. For planets up to a few Jupiter masses, eccentric
Constraining the primordial orbits of the terrestrial planets
Evidence in the Solar System suggests that the giant planets underwent an epoch of radial migration that was very rapid, with an e-folding timescale shorter than 1~Myr. It is probable that the cause
Constructing the secular architecture of the solar system II: The terrestrial planets
We investigate the dynamical evolution of the terrestrial planets during the planetesimal-driven migration of the giant planets. A basic assumption of this work is that giant planet migration
Debris disks as signposts of terrestrial planet formation
There exists strong circumstantial evidence from their eccentric orbits that most of the known extra-solar planetary systems are the survivors of violent dynamical instabilities. Here we explore the


Orbital Evolution of Planets Embedded in a Planetesimal Disk
The existence of the Oort comet cloud, the Kuiper belt, and plausible inefficiencies in planetary core formation all suggest that there was once a residual planetesimal disk of mass ∼10–100 M⊕ in the
Nebular gas drag and planetary accretion. II. Planet on an eccentric orbit.
Abstract We study the trajectories of planetesimals whose orbits decay starward as a result of gas drag and are perturbed by the gravity of a massive planet on an eccentric orbit. Each planetesimal
The Primordial Excitation and Clearing of the Asteroid Belt
Abstract In this paper, we use N -body integrations to study the effect that planetary embryos spread between ∼0.5 and 4 AU would have on primordial asteroids. The most promising model for the
Nebular Gas Drag and Planetary Accretion
Abstract We have studied the orbital dynamics of planetesimals whose decay due to gas drag in the primordial solar nebula causes them to spiral sunward and approach a growing planet. The planet is
Excitation and Propagation of Eccentricity Disturbances in Planetary Systems
The high eccentricities of the known extrasolar planets remain largely unexplained. We explore the possibility that eccentricities are excited in the outer parts of an extended planetary disk by
Eccentricity Evolution for Planets in Gaseous Disks
At least several percent of solar-type stars possess giant planets. Surprisingly, most move on orbits of substantial eccentricity. We investigate the hypothesis that interactions between a giant
Origin of the cataclysmic Late Heavy Bombardment period of the terrestrial planets
This model not only naturally explains the Late Heavy Bombardment, but also reproduces the observational constraints of the outer Solar System.