Hydrodynamics of giant planet formation. II - Model equations and critical mass. III - Jupiter's nucleated instability

Details Hydrodynamics of giant planet formation. II - Model equations and critical mass. III - Jupiter's nucleated instability Hydrodynamics of giant planet formation. II - Model equations and critical mass. III - Jupiter's nucleated instability

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991icar...91...39w&link_type=abstract

Icarus (ISSN 0019-1035), vol. 91, May 1991, p. 39-64.

Statistics

Computation

35

Astronomical Models, Gas Giant Planets, Magnetohydrodynamics, Planetary Evolution, Planetary Mass, Protoplanets, Chemical Composition, Solar System Evolution, Stellar Composition, Stellar Envelopes

Scientific paper

A spherically symmetric protoplanetary model with a growing rigid core and a gaseous envelope of solar composition is used to investigate the character and evolution of the nucleated instability; the model equations formulated are used to follow the static evolution of a protogiant planet in the 'Kyoto' solar nebula, lying at Jupiter's solar distance, to its critical core mass. Convective energy transfer has been formulated for inclusion in implicit radiation hydrodynamical computations. It is established that collapse need not occur at the critical mass, which in agreement with earlier investigations is found to be of the order of 13.1 earth masses. This model is then used as an initial condition for a radiation hydrodynamical calculation of the nucleated instability. It is found that nonlinear hydrodynamic waves are excited by a kappa mechanism, and that an outflow is driven.

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