Dust and the formation of planets with iron cores in the early solar system

Details Dust and the formation of planets with iron cores in the early solar system Dust and the formation of planets with iron cores in the early solar system

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978a%26a....69..125w&link_type=abstract

Astronomy and Astrophysics, vol. 69, no. 1, Sept. 1978, p. 125-128.

Astronomy and Astrophysics

Astrophysics

3

Cosmic Dust, Planetary Cores, Planetary Evolution, Solar System, Terrestrial Planets, Charged Particles, Interstellar Matter, Iron, Planetary Nebulae, Silicates, Solar Corona, Earth, Heat, Core, Iron, Interior, Review, Mantle, Clouds, Grain Size, Origin, Solar System, Accretion, Metallic Core, Silicates, Solar Nebula, Cosmic Dust, Temperatures

Scientific paper

A hypothesis is considered which can account for the formation of terrestrial-type planets that were already differentiated into a metallic core and a silicate mantle at formation. It is suggested that dust in the primeval solar nebula was charged in the same way that steady-state processes of electron capture charge the dust particles in interstellar clouds. Charged-dust accretion is shown to have acted as a screening mechanism which allowed metal grains to accrete easily onto each other but inhibited the accretion of silicate material until the temperature in the nebula dropped below 100 K. Calculations are discussed which indicate that: (1) meter-sized planetesimals of iron formed first and then accumulated by gravitational instability into bodies similar to earth's core; (2) these bodies were subsequently mantled by the silicate fraction a considerable time later (at least 10 million years); and (3) planets that were already segregated at the outset formed in the inner solar system.

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