Rapid growth of gas-giant cores by pebble accretion

@article{Lambrechts2012RapidGO,
  title={Rapid growth of gas-giant cores by pebble accretion},
  author={Michiel Lambrechts and Anders Johansen},
  journal={Astronomy and Astrophysics},
  year={2012},
  volume={544}
}
The observed lifetimes of gaseous protoplanetary discs place strong constraints on gas and ice giant formation in the core accretion scenario. The approximately 10-Earth-mass solid core responsible for the attraction of the gaseous envelope has to form before gas dissipation in the protoplanetary disc is completed within 1–10 million years. Building up the core by collisions between km-sized planetesimals fails to meet this timescale constraint, especially at wide stellar separations… Expand
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References

SHOWING 1-10 OF 75 REFERENCES
Constraint on the Giant Planet Production by Core Accretion
The issue of giant planet formation by core accretion (CA) far from the central star is rather controversial because the growth of a massive solid core necessary for triggering the gas runaway canExpand
Rapid planetesimal formation in turbulent circumstellar disks
TLDR
It is reported that boulders can undergo efficient gravitational collapse in locally overdense regions in the midplane of the disk, and it is found that gravitationally bound clusters form with masses comparable to dwarf planets and containing a distribution of boulder sizes. Expand
Atmospheres of Protoplanetary Cores: Critical Mass for Nucleated Instability
We systematically study quasi-static atmospheres of accreting protoplanetary cores for different opacity behaviors and realistic planetesimal accretion rates in various parts of the protoplanetaryExpand
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
Dust accretion onto high-mass planets
Aims. We study the accretion of dust particles of various sizes onto embedded massive gas giant planets, where we take into account the structure of the gas disk due to the presence of the planet.Expand
Protostellar Disks: Formation, Fragmentation, and the Brown Dwarf Desert
We argue that gravitational instability of typical protostellar disks is not a viable mechanism for the fragmentation into multiple systems (binary stars, brown dwarf companions, or gas giantExpand
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
Gas giant formation with small cores triggered by envelope pollution by icy planetesimals
We have investigated how envelope pollution by icy planetesimals affects the critical core mass for gas giant formation and the gas accretion time-scales. In the core-accretion model, runaway gasExpand
Can Giant Planets Form by Direct Gravitational Instability
Gravitational instability has been invoked as a possible mechanism of the giant planet production in protoplanetary disks. Here we critically revise its viability by noting that to form planetsExpand
THE FORMATION MECHANISM OF GAS GIANTS ON WIDE ORBITS
The recent discoveries of massive planets on ultra-wide orbits of HR 8799 and Fomalhaut present a new challenge for planet formation theorists. Our goal is to figure out which of three giant planetExpand
...
1
2
3
4
5
...