Orateur
Description
Analytical models describing the rotation of celestial bodies with a viscous fluid core commonly assume a simple motion for the fluid - a solution originally derived by Hough and Poincaré for a perfect (inviscid) fluid. In these models, viscosity is subsequently introduced ad hoc through an empirical friction torque at the core-mantle interface.
We propose a new analytical model in which the fluid core motion is described more realistically through a solution of the linearized Navier-Stokes equations. Our methodology is inspired by the work of Ievleva, who studied the motion of a pendulum containing a spherical cavity filled with an incompressible viscous fluid. We will examine the effects (similarities and differences) of this change in model on the rotational dynamics of the planets.