Timescales for planetary accretion and the structure of the protoplanetary disk

  title={Timescales for planetary accretion and the structure of the protoplanetary disk},
  author={Jack J. Lissauer},
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 mass sufficient to initiate rapid accretion of gas in times of order of 5 x 105−106 years, provided the surface density of solids in its accretion zone was at least 5–10 times greater than that required by minimum mass models of the protoplanetary disk. After Jupiter had accreted large amounts of nebular… Expand
The formation of Uranus and Neptune in the Jupiter ± Saturn region of the Solar System
the unreplenished inner disk to drain viscously onto the star in a short timescale. Studies of the ultraviolet and Ha ¯ux arising from the accretion process, and near-infrared ¯ux from the innerExpand
Modes of Gaseous Planet Formation
The discovery of gas giant planets around nearby stars has launched a new era in our understanding of the formation and evolution of planetary systems. However, none of the over four dozen companionsExpand
Possible Rapid Gas Giant Planet Formation in the Solar Nebula and Other Protoplanetary Disks.
  • Boss
  • Physics, Medicine
  • The Astrophysical journal
  • 2000
New three-dimensional, "locally isothermal," hydrodynamical models without velocity damping show that a disk instability can form Jupiter-mass clumps, implying that disk instability could obviate the core accretion mechanism in the solar nebula and elsewhere. Expand
Planetesimal Accretion onto Growing Proto-Gas Giant Planets
The solar and extrasolar gas giants appear to have diverse internal structure and metallicities. We examine a potential cause for these dispersions in the context of the conventional sequentialExpand
Formation of gas giant planets: core accretion models with fragmentation and planetary envelope
Abstract We have calculated formation of gas giant planets based on the standard core accretion model including effects of fragmentation and planetary envelope. The accretion process is found toExpand
Tidal Barrier and the Asymptotic Mass of Proto-Gas Giant Planets
According to the conventional sequential accretion scenario, observed extrasolar planets acquired their current masses via efficient gas accretion onto super-Earth cores with accretion timescalesExpand
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
Protoplanetary accretion disc models: The effects of several meteoritic, astronomical, and physical constraints
Abstract The concept of a protosolar viscous accretion disc is reviewed and a simple accretion disc model is laid out in such a way that the parameters controlling the properties and evolution of theExpand
Protoplanetary Formation. I. Neptune
Neptune has a gaseous envelope with mass larger than that of the Earth. We examine the possibility that proto-Neptune formed through an initial buildup of a core prior to the accretion of a gaseousExpand
Early accretional history of the Earth and the Moon-forming event
Abstract The accretion of the Earth is considered in the broader perspective of the formation of the solar system. Formation of planets from dust, or from a giant gaseous protoplanet predict uniformExpand


From icy planetesimals to outer planets and comets
Abstract Numerical simulations of planet growth in the outer solar system shows thatgrwoth of Uranus and Neptune occurs in reasonably short time, well below the actual age of the system, without theExpand
Mass loss from the region of Mars and the asteroid belt
Abstract Models of the solar nebula suggest that the mass of solid matter which condensed in the region of Mars and the asteroids was much greater than the amount now present. Bombardment by aExpand
The formation of planetesimals.
Four stages in the accretion of planetesimals are described. The initial stage is the condensation of dust particles from the gaseous solar nebula as it cools. These dust particles settle into a thinExpand
Calculations of the accretion and evolution of giant planets: The effects of solid cores
The evolution of the giant planets is calculated under the general hypothesis that the solid cores formed first, by accretion of small particles, and that these cores later gravitationally attractedExpand
Dynamical evolution of a cometary swarm in the outer planetary region
  • J. A. Fernández, W. Ip
  • Physics
  • 1981
The dynamical evolution of bodies under the gravitational influence of the accreting proto-Uranus and proto-Neptune is investigated. The main aim of this study is to analyze the interrelationsExpand
On the origin and initial temperature of Jupiter and Saturn
A two-stage growth of the giant planets, Jupiter and Saturn, is considered, which is different from the model of contraction of large gaseous protoplanets. In the first stage, within a time of ∼3 ×Expand
Orbital resonances in the solar nebula - Implications for planetary accretion
Abstract The influence of gas drag and gravitational perturbations by a planetary embryo on the orbit of a planetesimal in the solar nebula was examined. Non-Keplerian rotation of the gas causesExpand
Planetesimals to planets: Numerical simulation of collisional evolution
A simulation of collisional and gravitational interaction in the early solar system generates planets ∼500 km in diameter from an initial swarm of kilometer-sized planetesimals, such as might haveExpand
Some dynamical aspects of the accretion of Uranus and Neptune: The exchange of orbital angular momentum with planetesimals
Abstract The final stage of the accretion of Uranus and Neptune is numerically investigated. The four Jovian planets are considered with Jupiter and Saturn assumed to have reached their presentExpand
Protostellar angular momentum transport by spiral density waves
Abstract The gravitational collapse of molecular clouds or cloud cores is expected to lead to the formation of stars that begin their lives in a state of rapid rotation. It is known that, in at leastExpand