Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985avest..18..322s&link_type=abstract
(Astronomicheskii Vestnik, vol. 18, Oct.-Dec. 1984, p. 322-341) Solar System Research (ISSN 0038-0946), vol. 18, no. 4, April 19
Astronomy and Astrophysics
Astronomy
Cosmology, Planetary Nebulae, Solar System, Asteroids, Comets, Earth (Planet), Gas Giant Planets, Natural Satellites
Scientific paper
The possibility of the formation of the sun and preplanetary nebula from a proto-solar nebula with an initial mass of about 1.05 solar mass and initial angular momentum of about 10 to the 52nd per sq cm/sec is discussed. Turbulence was generated during the collapse of the nebula, at the stage of gas accretion onto the nucleus and surrounding nascent disk, and the gas viscosity could have been sufficient for the expansion of the disk to the size of the planetary system. The formation of a dust layer in the disk, its disintegration into clumps, and their transformation into solid bodies are discussed. The evolution of the swarm of preplanetary bodies, the formation of the planetesimals (the number of which initially reached a hundred in the zone of the earth), and their accumulation into the planets are examined. It is shown that the formation of the small bodies of the solar system - the satellites, asteroids, and comets - was a natural side effect of the process of the accumulation of the planets. The initial temperature of the earth, the inhomogeneity of its interior, and the possibility of its differentiation at the final stage of accumulation are discussed.
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