Pumping of a planetesimal disc by a rapidly migrating planet

@article{Edgar2004PumpingOA,
  title={Pumping of a planetesimal disc by a rapidly migrating planet},
  author={Richard G. Edgar and Pawel Artymowicz},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2004},
  volume={354},
  pages={769-772}
}
  • R. Edgar, P. Artymowicz
  • Published 1 September 2004
  • Physics
  • Monthly Notices of the Royal Astronomical Society
We examine the effect of a rapidly migrating protoplanet on a ring of planetesimals. The eccentricities of the planetesimals are usually increased bye ∈ (0.01, 0.1), with the exact increase being proportional to the mass of the protoplanet, and inversely proportional to its migration rate. The eccentricity distribution is also substantially changed from a Rayleigh distribution. We discuss the possible implications for further planet formation, and suggest that the rapid passage of a protoplanet… Expand
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References

SHOWING 1-10 OF 16 REFERENCES
A Reduced Efficiency of Terrestrial Planet Formation following Giant Planet Migration
Substantial orbital migration of massive planets may occur in most extrasolar planetary systems. Since migration is likely to occur after a significant fraction of the dust has been locked up into… Expand
Disk tides and accretion runaway
It is suggested that tidal interaction of an accreting planetary embryo with the gaseous preplanetary disk may provide a mechanism to breach the so-called runaway limit during the formation of the… Expand
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 )… Expand
Growth of a Migrating Protoplanet
Abstract In the solar nebula, protoplanets may rapidly migrate to the Sun due to the tidal interaction with the nebula disk (e.g., Ward 1986, Icarus67, 164–180). We investigated the growth rate of a… Expand
Accretional Evolution of a Planetesimal Swarm
We use our multi-zone simulation code (D. Spaute, S. Weidenschilling, D. R. Davis, and F. Marzari,Icarus92,147–164, 1991) to model numerically the accretion of a swarm of planetesimals in the region… Expand
Runaway Migration and the Formation of Hot Jupiters
We evaluate the coorbital corotation torque on a migrating protoplanet. The coorbital torque is assumed to come from orbit crossing fluid elements that exchange angular momentum with the planet when… Expand
Formation of planetary embryos: effects of fragmentation, low relative velocity, and independent variation of eccentricity and inclination.
TLDR
An earlier investigation of the formation of approximately 10(26) g planetary embryos from much smaller planetesimals has been extended to include the effects of collisional fragmentation, the low relative velocity regime in which the effects due to solar gravity are important, and independent perturbations of eccentricity and inclination. Expand
Velocity Evolution of Planetesimals: Unified Analytical Formulas and Comparisons with N-Body Simulations
Abstract Analytical formulas are derived for the rates of evolution of the mean square orbital eccentricities and inclinations of a general population of planetesimals. For planetesimals on crossing… Expand
Protostars and Planets VI
Various papers on the formation of stars and planets are presented. The general topics addressed include: molecular clouds and star formation, young stellar objects and circumstellar disks, chemistry… Expand
Disk-Satellite Interaction via Density Waves and the Eccentricity Evolution of Bodies Embedded in Disks
Using a generalized torque formula for Lindblad resonances in non-self-gravitating gaseous disks we study the interaction of disks with small, embedded bodies (not able to open a gap). For satellites… Expand
...
1
2
...