Oligarchic growth of giant planets

  title={Oligarchic growth of giant planets},
  author={E. Thommes and M. Duncan and H. Levison},
Runaway growth ends when the largest protoplanets dominate the dynamics of the planetesimal disk; the subsequent self-limiting accretion mode is referred to as “oligarchic growth.” Here, we begin by expanding on the existing analytic model of the oligarchic growth regime. From this, we derive global estimates of the planet formation rate throughout a protoplanetary disk. We find that a relatively high-mass protoplanetary disk (∼10 × minimum-mass) is required to produce giant planet core-sized… Expand
Oligarchic and giant impact growth of terrestrial planets in the presence of gas giant planet migration
Giant planets found orbiting close to their central stars, the so-called hot Jupiters, are thought to have originally formed in the cooler outer regions of a protoplanetary disk and then to haveExpand
Oligarchic planetesimal accretion and giant planet formation II
Aims. In the context of the core instability model, we present calculations of in situ giant planet formation. The oligarchic growth regime of solid protoplanets is the model adopted for the growthExpand
Giant planet formation with pebble accretion
Abstract In the core accretion model for giant planet formation, a solid core forms by coagulation of dust grains in a protoplanetary disk and then accretes gas from the disk when the core reaches aExpand
Fast Accretion of Small Planetesimals by Protoplanetary Cores
We explore the dynamics of small planetesimals coexisting with massive protoplanetary cores in a gaseous nebula. Gas drag strongly affects the motion of small bodies, leading to the decay of theirExpand
Theory of planet formation
We review the current theoretical understanding how growth from micro-meter sized dust to massive giant planets occurs in disks around young stars. After introducing a number of observationalExpand
Exploring the conditions for forming cold gas giants through planetesimal accretion
The formation of cold gas giants similar to Jupiter and Saturn in orbit and mass is a great challenge for planetesimal-driven core accretion models because the core growth rates far from the star areExpand
Formation of Cores of Giant Planets and an Implication for "Planet Desert"
We discuss accretion of cores of giant planets from planetesimals, based on the results of N-body simulations. We derive the core isolation mass, which is a final core mass as a result ofExpand
Formation of planetary systems by pebble accretion and migration : Growth of gas giants
Giant planets migrate though the protoplanetary disc as they grow their solid core and attract their gaseous envelope. Previously, we have studied the growth and migration of an isolated planet in anExpand
Terrestrial Rock Gas Planet Mass Gas Giant Ice Giant Ices
The standard planetesimal model of terrestrial-planet formation is based on astronomical and cosmochemical observations, and the results of laboratory experiments and numerical simulations. In thisExpand
Growth after the streaming instability: from planetesimal accretion to pebble accretion.
Streaming instability is a key mechanism in planet formation, clustering pebbles into planetesimals. It is triggered at a particular disk location where the local volume density of solids exceedsExpand


Evolution of the Solar Nebula. IV. Giant Gaseous Protoplanet Formation
The discovery of the first extrasolar planets, with masses in the range of ~0.5 MJup (MJup = Jupiter mass) to ~3 MJup, demands a reevaluation of theoretical mechanisms for giant planet formation.Expand
Formation of Protoplanets from Planetesimals in the Solar Nebula
Planetary accretion from planetesimals to protoplanets is investigated using three-dimensional N-body simulations. The effect of gas drag due to solar nebula is included and realistic-sizedExpand
Timescales for planetary accretion and the structure of the protoplanetary disk
Abstract This paper outlines a unified scenario for Solar System formation consistent with astrophysical constraints. Jupiter's core could have grown by runaway accretion of planetesimals to a massExpand
Formation of the Giant Planets by Concurrent Accretion of Solids and Gas
New numerical simulations of the formation of the giant of the second phase. planets are presented, in which for the first time both the gas and The actual rates at which the giant planets accretedExpand
Accretion rates of protoplanets: II. Gaussian distributions of planetesimal velocities
Abstract We calculate the growth rate of a protoplanet embedded in a uniform surface density disk of planetesimals having a triaxial Gaussian velocity dispersion. The longitudes of the apses andExpand
Making the Terrestrial Planets: N-Body Integrations of Planetary Embryos in Three Dimensions
We simulate the late stages of terrestrial-planet formation using N-body integrations, in three dimensions, of disks of up to 56 initially isolated, nearly coplanar planetary embryos, plus JupiterExpand
Planet Migration and Gap Formation by Tidally Induced Shocks
Gap formation in a gas disk triggered by disk-planet tidal interaction is considered. Density waves launched by the planet are assumed to be damped as a result of their nonlinear evolution leading toExpand
Formation of Protoplanet Systems and Diversity of Planetary Systems
We investigate the formation of protoplanet systems from planetesimal disks by global (N = 5000 and 10,000 and 0.5 AU 2. The growth timescale increases with a but decreases with Σ1. Based on theExpand
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. Expand
Thermal Profiles in Protoplanetary Disks
  • A. Boss
  • Materials Science, Physics
  • 1995
Disk temperatures control the degree of condensation of iron, silicates, and ices, and hence determine the surface density and type of solids available for initiating planetesimal accumulation.Expand