This paper deals with a new formulation of the creep tide theory ( Ferraz-Mello , Cel .
Mech .
Dyn .
Astron . 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 } { 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 . 122 , 359 , 2015 ) are included at the end of the paper .