Computer Science
Scientific paper
Nov 1974
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974icar...23..319b&link_type=abstract
Icarus, vol. 23, Nov. 1974, p. 319-325.
Computer Science
23
Hydrodynamics, Jupiter (Planet), Planetary Evolution, Computer Programs, Condensing, Gravitational Collapse, Hydrogen, Planetary Temperature, Radiative Heat Transfer, Solar System
Scientific paper
The evolution of the protoplanet Jupiter is followed, using a hydrodynamic computer code with radiative energy transport. Jupiter is assumed to have formed as a subcondensation in the primitive solar nebula at a density just high enough for gravitational collapse to occur. The initial state has a density of 0.0015 nanograms per cu cm and a temperature of 43 K; the calculations are carried to an equilibrium state where the central density reaches 0.5 g per cu cm and the central temperature reaches 25,000 K. During the early part of the evolution the object contracts in quasi-hydrostatic equilibrium; later on hydrodynamic collapse occurs, induced by the dissociation of hydrogen molecules. After dissociation is complete, the planet regains hydrostatic equilibrium with a radius of a few times the present value. Further evolution beyond this point is not treated here; however the results are consistent with the existence of a high-luminosity phase shortly after the planet settles into its final quasi-static contraction.-
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