Structure and evolution of gaseous protoplanets

Details Structure and evolution of gaseous protoplanets Structure and evolution of gaseous protoplanets

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989qjras..30..169b&link_type=abstract

Royal Astronomical Society, Quarterly Journal (ISSN 0035-8738), vol. 30, June 1989, p. 169-179. Research supported by NASA.

Astronomy and Astrophysics

Astronomy

1

Gas Giant Planets, Planetary Evolution, Planetary Systems, Protoplanets, Computerized Simulation, Natural Satellites, Planetary Atmospheres, Planetary Composition, Stellar Evolution

Scientific paper

The evolutionary stages of a giant planet are reviewed, starting with the formation of the solar nebula and ending at the present time. The general mechanism for formation of a giant planet is assumed to involve the accumulation of solid material to form a core which grows to a critical mass, after which rapid accretion of the gaseous envelope occurs. The object then evolves at constant mass to its present state. Detailed numerical simulations of these evolutionary phases, under the assumption of spherical symmetry are reviewed, with particular attention to formation time scales, chemical composition, rotation, and satellite formation.

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