The formation of planets and satellites from self-similar disks

Details The formation of planets and satellites from self-similar disks The formation of planets and satellites from self-similar disks

Jul 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979a%26a....76..200w&link_type=abstract

Astronomy and Astrophysics, vol. 76, no. 2, July 1979, p. 200-207. Research supported by the Royal Society of London.

Astronomy and Astrophysics

Astrophysics

5

Astronomical Models, Natural Satellites, Planetary Evolution, Protoplanets, Solar System, Gas Giant Planets, Mass Distribution, Nebulae, Protostars, Terrestrial Planets

Scientific paper

Self-similar flow regimes tend to be set up in large-scale fluid systems remote from boundaries. The hypothesis is examined that the terrestrial planets and the satellite systems of the solar system formed from self-similar disks that were dominated by the gravitational attraction of their primary bodies. The surface density in such a self-similar disk model varies directly as the inverse square of R, and the azimuthal velocity is Keplerian, varying directly as the inverse square root of R, where R is the distance from the primary. The masses of bodies forming out of the disk are derived and compared with observations for the terrestrial planets and the satellite systems of Jupiter, Saturn, and Uranus. The fit is good, suggesting that these systems formed from self-similar disks. If this conclusion is tentatively accepted, it removes the arbitrariness from solar-nebula disk models, since self-similar disks have no free dimensional parameters.

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