Planetary migration in a planetesimal disk: why did Neptune stop at 30 AU?

  title={Planetary migration in a planetesimal disk: why did Neptune stop at 30 AU?},
  author={Rodney Gomes and Alessandro Morbidelli and Harold F. Levison},

Migration of the outermost objects in planetary systems

The outermost bodies of planetary systems embedded in a planetesimal disk migrate much faster than the other planets. The outward migration of such bodies is self-sustained by supplying fresh

Resonant Structures in Planetesimal Disks due to Planetary Migration

Context. The observed clumpy structures in debris disks are commonly interpreted as particles trapped in mean-motion resonances with an unseen exo-planet. Populating the resonances requires a

Constraining the Giant Planets’ Initial Configuration from Their Evolution: Implications for the Timing of the Planetary Instability

Recent works on planetary migration show that the orbital structure of the Kuiper Belt can be very well reproduced if, before the onset of planetary instability, Neptune underwent a long-range

Debris disks as signposts of terrestrial planet formation - II. Dependence of exoplanet architectures on giant planet and disk properties

We present models for the formation of terrestrial planets, and the collisional evolution of debris disks, in planetary systems that contain multiple marginally unstable gas giants. We previousl y

Evidence for very early migration of the Solar System planets from the Patroclus–Menoetius binary Jupiter Trojan

The orbital distribution of trans-Neptunian objects provides strong evidence for the radial migration of Neptune1,2. The outer planets’ orbits are thought to have become unstable during the early


A residual planetesimal disk of mass 10-100 M⊕ remained in the outer solar system following the birth of the giant planets, as implied by the existence of the Oort cloud, coagulation requirements for


We revisit the issue of the cause of the dynamical instability during the so-called Nice model, which describes the early dynamical evolution of the giant planets. In particular, we address the

The Kuiper Belt and the Solar System's Comet Disk

A growing body of evidence indicates that the sculpting of the Kuiper belt region may have involved large-scale planetary migration, the presence of other rogue planetary objects in the disk, and/or the close passage of other stars in the Sun's birth cluster.

Mass Distribution and Planet Formation in the Solar Nebula

The surface density profile Σ(r) of the solar nebula protoplanetary disk is a fundamental input to all models of disk processes and evolution. Traditionally it is estimated by spreading out the

Vega's hot dust from icy planetesimals scattered inwards by an outward-migrating planetary system

Vega has been shown to host multiple dust populations, including both hot exo-zodiacal dust at sub-AU radii and a cold debris disk extending beyond 100 AU. We use dynamical simulations to show how



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

Oligarchic growth of giant planets

The effects of a stellar encounter on a planetesimal disk

Abstract We investigate the effects of a passing stellar encounter on a planetesimal disk through analytical calculations and numerical simulations, and derive the boundary radius ( a planet )

Collisional Erosion in the Primordial Edgeworth-Kuiper Belt and the Generation of the 30-50 AU Kuiper Gap

One of the oustanding questions about the architecture of the outer solar system is how the trans-Neptunian disk of comets and small planet-scale objects known as the solar system's Edgeworth-Kuiper

Evidence for Early Stellar Encounters in the Orbital Distribution of Edgeworth-Kuiper Belt Objects

We show that early stellar encounters can explain the high eccentricities and inclinations observed in the outer part (>42 AU) of the Edgeworth-Kuiper Belt (EKB). We consider the proto-Sun as a

The origin of Pluto's orbit: implications for the

The origin of the highly eccentric, inclined, and resonance-locked orbit of Pluto has long been a puzzle. A possible explanation has been proposed recently which suggests that these extraordinary

Signatures of the Giant Planets Imprinted on the Edgeworth-Kuiper Belt Dust Disk

One method to detect extrasolar planetary systems is to deduce the perturbations of planets on the observed circumstellar dust disks. Our solar system, with its known configuration of planets,

Planetary Embryos Never Formed in the Kuiper Belt

Abstract We study the orbital evolutions of various systems of planetary embryos in the transneptunian region, undergoing mutual scattering and perturbations from the giant planets. We show that

Signatures of Exosolar Planets in Dust Debris Disks

We apply our recently elaborated, powerful numerical approach to the high-resolution modeling of the structure and emission of circumstellar dust disks, incorporating all relevant physical processes.

The formation of Uranus and Neptune in the Jupiter–Saturn region of the Solar System

The results of model calculations are reported that demonstrate that solid cores of the gas-giant planets Jupiter and Saturn will have been gravitationally scattered outwards as Jupiter, and perhaps Saturn, accreted nebular gas.