Accumulation of the planets

Details Accumulation of the planets Accumulation of the planets

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987pggp.rept...92w&link_type=abstract

In NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1986 p 92-94 (SEE N87-23341 16-91)

Physics

Geophysics

Asteroids, Astronomical Models, Collisions, Gases, Kinetic Theory, Protoplanets, Gravitational Effects, Mass Distribution, Monte Carlo Method, Perturbation, Velocity

Scientific paper

In modeling the accumulation of planetesimals into planets, it is appropriate to distinguish between two stages: an early stage, during which approximately 10 km diameter planetesimals accumulate locally to form bodies approximate 10 to the 25th g in mass; and a later stage in which the approximately 10 to the 25th g planetesimals accumulate into the final planets. In the terrestrial planet region, an initial planetesimal swarm corresponding to the critical mass of dust layer gravitational instabilities is considered. In order to better understand the accumulation history of Mercury-sized bodies, 19 Monte-Carlo simulations of terrestrial planet growth were calculated. A Monte Carlo technique was used to investigate the orbital evolution of asteroidal collision debris produced interior to 2.6 AU. It was found that there are two regions primarily responsible for production of Earth-crossing meteoritic material and Apollo objects. The same techniques were extended to include the origin of Earth-approaching asteroidal bodies. It is found that these same two resonant mechanisms predict a steady-state number of Apollo-Amor about 1/2 that estimated based on astronomical observations.

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