Giant Planet Cores: Solid vs. Stable

Details Giant Planet Cores: Solid vs. Stable Giant Planet Cores: Solid vs. Stable

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufm.p51b1425e&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #P51B-1425

Physics

5700 Planetology: Fluid Planets, 5724 Interiors (8147)

Scientific paper

Planets with stable (non-convecting) fluid cores are usually modeled using a solid impermeable core. An alternative is to model the central region as a stable fluid with a subadiabatic entropy gradient. The energy in this region is transported via radiation rather than convection. This is a more realistic representation for a giant gaseous planet as it allows for some convective penetration into the stable region and eliminates the artificial rigid boundary condition at the interface. We use a 2D finite volume hydrodynamic code to compare the fluid behavior in two density stratified cases, one with a solid core and one with a stable subadiabatic fluid core. Our goal is to identify the differences between the convective patterns in these two cases and the resulting kinetic energy distribution and entropy profiles. Using these results, and subsequent 3D simulations, it may be possible to determine the core structure in giant planets based on surface observations such as the zonal wind patterns and strengths.

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