Physics
Scientific paper
Apr 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978icar...34..173f&link_type=abstract
Icarus, vol. 34, Apr. 1978, p. 173-181. Translation.
Physics
17
Gas Giant Planets, Mass Transfer, Planetary Evolution, Comets, Mass Distribution, Particle Collisions, Particle Energy, Planets, Accretion, Solar System, Planetesimals, Ejecta, Particles, Energy, Comets, Origin, Particle Interactions, Orbits, Three Body System
Scientific paper
The changes in the heliocentric energies of particles due to close encounters with the outer planets are analyzed. Two stages in the evolution of the planets are proposed. The first phase was characterized by the rapid growth of the protoplanets. During this stage the collisions prevailed over the ejection of particles in close encounters. The second phase was characterized by the 'spreading' of the residual solid matter toward the inner and outer regions of the solar system. For the outer planets the probabilities that a particle is ejected out of the solar system or achieves a near-parabolic orbit, after a close encounter, are calculated. The particles in near-parabolic orbits might have originated the cometary cloud that presumably surrounds the solar system. It is found that the ratio between these particles and the total number of ejected particles increases with the planet-sun distance. It is suggested that Neptune, and perhaps Uranus, could have supplied an important fraction of the total mass of the cometary cloud.
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