Calculations of the Effects of Angular Momentum on the Early Evolution of Jupiter
Abstract
The planet Jupiter is assumed to have formed as a subcondensation in the solar nebula. The initial phase of its evolution is one of hydrostatic contraction with radiative energy transport. Calculations of evolutionary sequences through this phase are presented, including the effects of angular momentum. The calculations are carried out in two space dimensions under the assumptions of axial symmetry, constancy of angular velocity on cylindrical surfaces about the rotation axis, a pressuredensity relation given by the polytrope of index 3, conservation of angular momentum, and a homogeneous composition. The results show that under certain physically reasonable initial distributions of density and angular momentum the formation of a central planet and a rotating circumplanetary envelope is possible, while under assumptions a point of instability is reached that probably results in the breakup of the condensation by fission into two or more parts. The models are discussed with reference to the present angular momenta of Jupiter and its regular satellites.
 Publication:

Icarus
 Pub Date:
 July 1977
 DOI:
 10.1016/00191035(77)900288
 Bibcode:
 1977Icar...31..356B
 Keywords:

 Angular Momentum;
 Jupiter (Planet);
 Planetary Evolution;
 Planetology;
 Angular Velocity;
 Density Distribution;
 Energy Dissipation;
 Galilean Satellites;
 Momentum Transfer;
 Natural Satellites;
 Lunar and Planetary Exploration