Calculations of the evolution of the giant planets

Details Calculations of the evolution of the giant planets Calculations of the evolution of the giant planets

Feb 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980icar...41..293b&link_type=abstract

Icarus, vol. 41, Feb. 1980, p. 293-308.

Astronomy and Astrophysics

Astronomy

35

Gas Giant Planets, Planetary Evolution, Protoplanets, Astronomical Models, Planetary Structure, Cores, Symmetry, Chemical Properties, Luminosity, Planetesimals, Structure, Rotation, Planets, Evolution, Equations Of State, Opacity, Nebulas, Solar System, Condensation, Composition, Mass, Density, Dynamics, Hydrostatics, Collapse, Dissociation, Data, Hydrogen, Equlibrium, Cooling, Contraction, Comparisons, Models, Temperatures, Jupiter, Saturn, Phases

Scientific paper

Evolutionary calculations are presented for spherically symmetric protoplanetary configurations with a homogeneous solar composition and with masses of 1000, 1500, 28,500 and 42,000 solar masses. Recent improvements in equation-of-state and opacity calculations are incorporated. Sequences start as subcondensations in the solar nebula with densities of 10 to the -10th to 10 to the -11th g/cu cm, evolve through a hydrostatic phase lasting 100 thousand to 10 million years, undergo dynamic collapse due to dissociation of molecular hydrogen, and regain hydrostatic equilibrium with densities of about 1 g/cu cm. The nature of the objects at the onset of the final phase of cooling and contraction is discussed and compared with previous calculations.

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