The thermal emission of Saturn’s icy moons

Context. The effects of space weathering and other alteration processes on the upper surface Saturn’s icy moons are yet to be explored. Aims. We present a thermophysical model parametrised by way regolith properties such as porosity, grain size, composition, well local topography. modelled temperature apparent emissivity intended compared measurements taken Cassini’s Composite Infrared Spectrometer (CIRS), using its focal plane FP1. study how they impacted topographic properties. Methods. As an example, we coupled topography Dione moon with our model. Simulations provide thermal history elements shape included in FP1 footprints at viewing geometries along one CIRS observation. heat transfer may occur through conduction or radiation. Its bolometric albedo, A , hemispherical emissivity, ε h expressed function Results. roughly reproduces observed variations temperature, T F chosen while assuming uniform dispersion temperatures within due difference time explains most directionality (Em), emission angles Em ≥ 30°. Adding 8-km scale amplifies this effect few percent. Refining 1 km increases it again single percent but high computational cost. This particular anisotropy (Em) cannot explained directional d regolith. is less affected resolution. regional size significantly improves agreement between observations. Conclusions. demonstrated good performance and, thus, ready for testing current hypotheses processing moons, changes size.