  Miranda has a unusually high inclination ($I=4.338^\circ$), and its surface
reveals signs of past endogenic activity. Investigations of the dynamical
aspects of its orbital evolution suggest probable resonant processes, in
particular with Umbriel, as an explanation for the present high inclination of
Miranda. The tidal heating induced by gravitational interactions can lead to
the rise of eccentricities and, consequently, to the increased dissipation of
energy inside the satellite and higher internal temperatures. We study here the
possible increase in eccentricities caused by orbital resonances and the
resulting endogenic heating on Miranda taking into account its temperature
dependent rheology. The coupled orbital-thermal evolution model was run with
different rheological models and the thermal parameters starting form a cold
thermal state, in radiative equilibrium with the environment. For the nominal
parameters of the evolution scenarios studied, the resonances were not
sufficient to rise neither the eccentricities nor the internal temperatures
significantly. Lowest dissipation function $Q$ of around 100 and final
eccentricity of $e\approx0.02$ were obtained during the resonance 3:1 with
Umbriel.
