Physics – Geophysics
Scientific paper
Jun 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pggp.rept..443l&link_type=abstract
In NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990 p 443 (SEE N92-10728 01-91)
Physics
Geophysics
Astronomical Models, Collision Parameters, Collisions, Planetary Cores, Planetary Evolution, Planetary Nebulae, Protoplanets, Terrestrial Planets, Eccentric Orbits, Gas Dynamics, Gas Giant Planets, Gravitational Effects, Orbit Perturbation, Size Distribution, Velocity Distribution
Scientific paper
The formation of terrestrial planets and the cores of Jovian planets is reviewed in the framework of the planetesimal hypothesis, wherein planets are assumed to grow via the pairwise accumulation of small solid bodies. The rate of (proto)planetary growth is determined by the size and mass of the protoplanet, the surface density of planetesimals, and the distribution of planetesimal velocities relative to the protoplanet. Planetesimal velocities are modified by mutual gravitational interactions and collisions, which convert energy present in the ordered relative motions of orbiting particles (Keplerian shear) into random motions and tend to reduce the velocities of the largest bodies in the swarm relative to those of smaller bodies, as well as by gas drag, which damps eccentricities and inclinations.
Lissauer Jack . J.
Stewart Glen Robert
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