Origin of the solar system. I - Gravitational contraction of the turbulent protosun and the shedding of a concentric system of gaseous Laplacian rings

Details Origin of the solar system. I - Gravitational contraction of the turbulent protosun and the shedding of a concentric system of gaseous Laplacian rings Origin of the solar system. I - Gravitational contraction of the turbulent protosun and the shedding of a concentric system of gaseous Laplacian rings

Nov 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978m%26p....19..341p&link_type=abstract

Moon and the Planets, vol. 19, Nov. 1978, p. 341-398.

Computer Science

24

Convective Flow, Gravitational Collapse, Planetary Evolution, Solar System, Supersonic Heat Transfer, Turbulence Effects, Ammonia, Angular Momentum, Chemical Composition, Condensation, Hydrogen Clouds, Hydrostatics, Ice Nuclei, Interstellar Matter, Methane, Nonuniformity, Protostars, Stellar Evolution, Stellar Mass Accretion, Stellar Mass Ejection

Scientific paper

A theory for the origin of the solar system is presented. The theory, based on concepts of supersonic convection, indicates the possibility that the original Laplacian hypothesis may be valid. According to the suggested theory, the first stage of the sun's formation consisted of the condensation of CNO ices and later H2 including He as impurity atoms at interstellar densities to form a cloud of solid grains. Attention is directed to the time at which the central opacity rises sufficiently to halt the free collapse at a certain central density, and it is shown that there is insufficient gravitational energy for the vaporized cloud to acquire a complete hydrostatic equilibrium at that time. Instead, it is suggested, the inner 3-4% of the cloud mass collapses freely all the way to stellar size to release sufficient energy to stabilize the rest of the infalling cloud. The early solar nebula would then consist of a small dense quasi-stellar core surrounded by a vast tenuous but opaque turbulent convective envelope.

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