  Paper on the creep tide theory and its applications to satellites and planets
with emphasis on a new set of differential equations allowing easier numerical
studies. The creep tide theory is a new paradigm that does not fix a priori the
tidal deformation of the body, but considers the deformation as a
low-Reynolds-number flow. The evolution under tidal forces is ruled by an
approximate solution of the Navier-Stokes equation depending on the body's
viscosity with no ad hoc assumptions on its shape and orientation. It
reproduces closely the results of Darwinian theories in the case of gaseous
planets and stars, but the results are completely different in the case of
stiff satellites and planets. It explains the tidal dissipations of Enceladus
and Mimas. The extension of the theory to nonhomogeneous icy satellites with a
subsurface ocean allows the amplitude of the forced oscillations around
synchronization (librations) to be better determined.
