Calculations of the Early Evolution of Jupiter
Abstract
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 1.5 × 10 -11 g cm -3 and a temperature of 43 K; the calculations are carried to an equilibrium state where the central density reaches 0.5 g cm -3 and the central temperature reaches 2.5 × 10 4 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 quasistatic contraction.
- Publication:
-
Icarus
- Pub Date:
- November 1974
- DOI:
- Bibcode:
- 1974Icar...23..319B
- Keywords:
-
- Hydrodynamics;
- Jupiter (Planet);
- Planetary Evolution;
- Computer Programs;
- Condensing;
- Gravitational Collapse;
- Hydrogen;
- Planetary Temperature;
- Radiative Heat Transfer;
- Solar System