The ESA Voyage 2050 program has identified Saturn's moon Enceladus as a primary target for
future outer Solar System missions aimed at assessing its potential habitability and internal
structure. To investigate Enceladus' interior, a novel mission concept is proposed, comprising an
orbiter tracked by surface landers. This study quantifies the attainable accuracy in the estimation of
key geophysical parameters by analyzing a range of mission architectures and design
configurations. From the derived uncertainties in selected parameters — including the tidal Love
numbers and libration amplitude — the analysis demonstrates how these observables can constrain
Enceladus' interior, assuming a three-layer structural model. The findings indicate that the proposed
mission architecture enables stringent estimates for Enceladus' geophysical parameters, thereby
yielding refined constraints of its internal properties, including the ice shell thickness, the densities of the core and subsurface ocean, the core radius, and the ice shell shear modulus.

Ceres is a small dwarf planet in the asteroid belt between the orbits of Mars and Jupiter. In this work, its interior density, interior temperature, crust thickness and crust density are modelled with the aim of determining possible formation mechanisms for the cryovolcanic bright spots on its surface. The results imply that Ceres has a muddy subsurface ocean from which the cryovolcanic material originates.

Of the four Galilean satellites the only one without ice is Io. While it is possible that Io never contained any ice the starting point of this research work is an icy Io. As present-day Io does not contain any ice, icy Io must have lost its ice through some sort of ice loss mechanism. In this work the assumed ice loss mechanism is geysers driven by tidal heating. Tidal dissipation of sufficient magnitude is able to melt part of an icy layer creating a subsurface ocean and is also able to crack the overlying icy shell. The subsurface ocean then acts as a reservoir from which water vapor molecules and icy grains accelerate upwards through the cracks and are erupted from the surface. Erupted material with a sufficient velocity is able to escape from icy Io resulting in ice loss.