The early evolution of Jupiter in the absence of solar tidal forces

Details The early evolution of Jupiter in the absence of solar tidal forces The early evolution of Jupiter in the absence of solar tidal forces

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982mnras.198..947s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 198, Mar. 1982, p. 947-959.

Astronomy and Astrophysics

Astronomy

8

Computerized Simulation, Jupiter (Planet), Planetary Evolution, Protoplanets, Astronomical Models, Energy Transfer, Hydrodynamic Equations, Radiative Transfer, Tides, Jupiter, Evolution, Tidal Effects, Opacity, Equations Of State, Pressure, Irradiation, Data, Heat, Thermal Effects, Shock, Equations Of Motion, Mathematical Models, Simulations, Computer Techniques, Hydrodynamics, Energy, Capture, Origin, Solar System, Surface, Solar Radiation, Collapse, Interior, Planetesimals, Condensation, Density

Scientific paper

The early evolution of a Jupiter-like protoplanet is simulated by constructing a physically detailed computer-based model which solves the equations of hydrodynamics and radiative energy transfer for the spherically symmetric case. The model is specifically developed to study the initial and boundary conditions relevant to the capture theory for the origin of the solar system. It is found that the absence of an external medium promotes the rapid expansion of surface material which is enhanced by solar irradiation. Only when the Jeans criterion is less than 0.8 does a spontaneous hydrodynamic collapse of the interior allow a substantial proportion of the protoplanet to condense to planetary densities.

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