Numerical models of giant planet formation with rotation

Details Numerical models of giant planet formation with rotation Numerical models of giant planet formation with rotation

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991icar...92..234k&link_type=abstract

Icarus (ISSN 0019-1035), vol. 92, Aug. 1991, p. 234-251. Research supported by NASA.

Astronomy and Astrophysics

Astronomy

21

Astronomical Models, Gas Giant Planets, Planetary Evolution, Planetary Rotation, Angular Momentum, Boundary Conditions, Centrifugal Force, Momentum Transfer, Protoplanets, Saturn (Planet)

Scientific paper

A 1D quasi-spherical approximation is presently used under the assumption of hydrostatic equilibrium to model giant-planet formation processes that encompass the accretion and transport of angular momentum for both radiative and convective zones. These calculations have been conducted up to masses comparable to those of Saturn. Angular momentum transport is strong, leading to strong concentration of angular momentum in the outer convective zones which develop envelope masses greater than 30 earth masses. When the models are allowed to contract near the calculation's end, the ratio of centrifugal force to gravity at the outer radius rises sufficiently to validate the quasi-spherical approximation.

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