  In Noyelles et al. (2008, Astron. Astrophys., 478, 959-970), a resonance
involving the wobble of Titan is hinted. This paper studies this scenario and
its consequences. The first step is to build an accurate analytical model that
would help to find the likely resonances in the rotation of every synchronous
body. In this model, I take the orbital eccentricity of the body into account,
as well as its variable inclination with respect to Saturn's equator. Then an
analytical study using the second fundamental model of the resonance is
performed to study the resonance of interest. Finally, I study the dissipative
consequences of this resonance. I find that this resonance may have increased
the wobble of Titan by several degrees. For instance, if Titan's polar momentum
C is equal to 0.355MR_T^2 (M and R_T being respectively Titan's mass and
radius), the wobble might be forced to 41 degrees. Thanks to an original
formula, I find that the dissipation associated with the forced wobble might
not be negligible compared to the contribution of the eccentricity. I also
suspect that, due to the forced wobble, Titan's period of rotation may be
somewhat underestimated by observers. Finally, I use the analytical model
presented in this paper to compute the periods of the free librations of the
four Galilean satellites as well as the Saturnian satellite Rhea. For Io and
Europa, the results are consistent with previous studies. For the other
satellites, the periods of the free librations are respectively 186.37 d, 23.38
y and 30.08 y for Ganymede, 2.44 y, 209.32 y and 356.54 y for Callisto, and
51.84 d, 2.60 y and 3.59 y for Rhea.
