Abstract
<jats:p>Intrinsic attenuation in planetary ices remains poorly constrained at seismic frequencies and low temperatures, limiting quantitative predictions of wave propagation in icy moons. Existing models typically rely on constant-Q, or power-law formulations that lack microphysical grounding and fail to capture the strong temperature sensitivity of ice Ih. Here, we develop a physics-based attenuation model that combines dislocation relaxation, grain-boundary sliding, and proton reorientation mechanisms within a unified Cole-Maxwell-SAS framework, ensuring a consistent transition between seismic and tidal frequency regimes. The model is calibrated against laboratory and semi-empirical constraints over 94–273 K and pressures up to 100 MPa. The results predict order-of-magnitude variations in intrinsic shear attenuation across icy-shell thermal profiles, and provide a quantitative framework for assessing wave dispersion, energy loss, and seismic detectability in the shells of Titan-like satellites.</jats:p>