  This paper deals with a new formulation of the creep tide theory
(Ferraz-Mello, Cel. Mech. Dyn. Astron. {\bf 116}, 109, 2013 $-$ Paper I) and
with the tidal dissipation predicted by the theory in the case of stiff bodies
whose rotation is not synchronous but is oscillating around the synchronous
state with a period equal to the orbital period. We show that the tidally
forced libration influences the amount of energy dissipated in the body and the
average perturbation of the orbital elements. This influence depends on the
libration amplitude and is generally neglected in the study of planetary
satellites. However, they may be responsible for a 27 percent increase in the
dissipation of Enceladus. The relaxation factor necessary to explain the
observed dissipation of Enceladus ($\gamma=1.2-3.8\times 10^{-7}\ {\rm
s}^{-1}$) has the expected order of magnitude for planetary satellites and
corresponds to the viscosity $0.6-1.9 \times 10^{14}$ Pa s, which is in
reasonable agreement with the value recently estimated by Efroimsky (2018)
($0.24 \times 10^{14}$ Pa s) and with the value adopted by Roberts and Nimmo
(2008) for the viscosity of the ice shell ($10^{13}-10^{14}$ Pa s). For
comparison purposes, the results are extended also to the case of Mimas and are
consistent with the negligible dissipation and the absence of observed tectonic
activity. The corrections of some mistakes and typos of paper II (Ferraz-Mello,
Cel. Mech. Dyn. Astron. {\bf 122}, 359, 2015) are included at the end of the
paper.
