Evolution of planetesimals. I - Dynamics: Relaxation in a thin disk. II - Numerical simulations

Details Evolution of planetesimals. I - Dynamics: Relaxation in a thin disk. II - Numerical simulations Evolution of planetesimals. I - Dynamics: Relaxation in a thin disk. II - Numerical simulations

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...403..336p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 403, no. 1, p. 336-376.

Statistics

Computation

24

Computational Astrophysics, Planetary Evolution, Protoplanets, Solar System Evolution, Fokker-Planck Equation, Gravitational Effects, Orbital Elements, Planetary Orbits, Planets, Planetesimals, Solar System, Dynamics, Energy, Scattering, Collisions, Equilibrium, Planetary Systems, Orbital Elements, Origin, Model, Diffusion, Parameters, Gravity Effects, Disks, Calculations, Analysis, Orbits, Motion, Celestial Mechanics, Velocity, Damping, Relaxation, Friction, Mass, Accretion, Theoretical Studies, Coagulatio

Scientific paper

The study examines the effects of density inhomogeneity and differential rotation as well as inelastic collisions on the dynamical evolution of planetesimals. Consideration is given to a three-step analysis: the dynamical evolution of the planetesimals, collisions and mass accumulation, and interaction with gas. It is shown that the velocity dispersion of a cold system of planetesimals increases rapidly due to elastic gravitational scattering. When the dispersion in the epicycle amplitude becomes comparable to the planetesimals' Roche radius, energy is transferred from the systematic Keplerian shear to the dispersive motion. With a numerical N-body scheme, gravitational scattering and physical collisions among a system of planetesimals is simulated. It is shown that dynamical equilibrium is attained with a velocity dispersion comparable to the surface escape velocity of those planetesimals which contribute most of the system mass.

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