Structure and evolution of isolated giant gaseous protoplanets

Details Structure and evolution of isolated giant gaseous protoplanets Structure and evolution of isolated giant gaseous protoplanets

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979icar...38..367d&link_type=abstract

Icarus, vol. 38, June 1979, p. 367-391.

Computer Science

48

Gas Giant Planets, Planetary Evolution, Planetary Structure, Angular Momentum, Gas Chromatography, Gas Mixtures, Granular Materials, Planetary Cores, Planetary Mass, Solar System, Planetesimals, Jovian Planets, Structure, Evolution, Origin, Convection, Jupiter, Mass, Grains, Core, Gases, Opacity, Saturn, Temperatures, Pressure, Interior, Metallic Core, Solar Nebula, Tidal Stress, Thermodynamics

Scientific paper

A model is developed describing the structure and evolution of isolated giant gaseous protoplanets in the mass range 0.3-4.5 Jovian masses. The central region of protoplanets of mass less than about 1 Jovian mass is, at some evolutionary epoch, thermodynamically favorable to the liquefaction of major interstellar grain components. All protoplanets studied are convective throughout most of their interior. In addition, it was found that the thermal contraction time depends sensitively on the surface opacity (at T less than 200 K).

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