Final Stages of Planet Formation

@article{Goldreich2004FinalSO,
  title={Final Stages of Planet Formation},
  author={Peter Goldreich and Yoram Lithwick and Re’em Sari},
  journal={The Astrophysical Journal},
  year={2004},
  volume={614},
  pages={497-507}
}
We address three questions regarding solar system planets: What determined their number? Why are their orbits nearly circular and coplanar? How long did they take to form? Runaway accretion in a disk of small bodies resulted in a tiny fraction of the bodies growing much larger than all the others. These big bodies dominated the viscous stirring of all bodies. Dynamical friction by small bodies cooled the random velocities of the big ones. Random velocities of small bodies were cooled by… Expand
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References

SHOWING 1-10 OF 49 REFERENCES
Planet formation by coagulation: A focus on Uranus and Neptune
Planets form in the circumstellar disks of young stars. We review the basic physical processes by which solid bodies accrete each other and alter each others' random velocities, and we provideExpand
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
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
Making More Terrestrial Planets
The results of 16 new 3D N-body simulations of the final stage of the formation of the terrestrial planets are presented. These Nbody integrations begin with 150‐160 lunar-to-Mars size planetaryExpand
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
The Growth of Planetary Embryos: Orderly, Runaway, or Oligarchic?
We consider the growth of a protoplanetary embryo embedded in a planetesimal disk. We take into account the dynamical evolution of the disk caused by (1) planetesimal-planetesimal interactions, whichExpand
PLANETESIMAL FORMATION BY GRAVITATIONAL INSTABILITY
We investigate the formation of planetesimals via the gravitational instability of solids that have settled to the midplane of a circumstellar disk. Vertical shear between the gas and a subdisk ofExpand
Rapid collisional evolution of comets during the formation of the Oort cloud
TLDR
It appears that collisions will prevent most comets escaping from most locations in the region of the giant planets until the disk mass there declines sufficiently that the dynamical ejection timescale is shorter than the collisional lifetime. Expand
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
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
...
1
2
3
4
5
...