The formation of iron, stone, and mixed planetesimals in the early solar system

Details The formation of iron, stone, and mixed planetesimals in the early solar system The formation of iron, stone, and mixed planetesimals in the early solar system

Jan 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978icar...33...74w&link_type=abstract

Icarus, vol. 33, Jan. 1978, p. 74-88. Research supported by the National Research Council of Canada and Science Research Counci

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Astronomical Models, Planetary Evolution, Solar System, Charged Particles, Interplanetary Dust, Iron, Particle Size Distribution, Planetology, Rocks, Solar Corona, Planetesimals, Particle Interactions, Origin, Dust, Accretion, Temperatures, Iron, Rocks, Solar System, Gases, Terrestrial Planets, Jovian Planets, Charged Particles

Scientific paper

The interactions of dust grains with each other in a finite-temperature solar nebula are examined, taking into account the important fact that such grains would carry net steady-state charges like those of grains in interstellar clouds. This charge is given by the well-known Spitzer relation. It provides a screening mechanism that operates during accretion and results in bodies of differing compositions depending on the local temperature in the nebula. In a typical nebula, it is found that planetesimals of 1 mm to 100 cm size form in a time of order one to ten million years. These planetesimals are of iron and stone and mixed composition in the inner solar system, but of mixed composition only in the outer solar system. The predictions of this type of charged-dust accretion can be compared to known data on meteorites and the composition of the planets.

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