Article ID | Journal | Published Year | Pages | File Type |
---|---|---|---|---|
1782656 | Planetary and Space Science | 2007 | 6 Pages |
Abstract
We study how the pattern of thermal convection and differential rotation in the interior of a giant gaseous planet is affected by the presence of a small solid core as a function of the planetary rotation rate. We show, using 2D anelastic, hydrodynamic simulations, that the presence of a small solid core results in significantly different flow structure relative to that of a fully convective interior only if there is little or no planetary rotation.
Related Topics
Physical Sciences and Engineering
Earth and Planetary Sciences
Geophysics
Authors
Martha Evonuk, Gary A. Glatzmaier,