  Our understanding of the surface porosity of icy moons and its evolution with
depth remains limited, including the precise scale at which ice compaction
occurs under self-weight pressure. This parameter is of crucial interest for
the correct interpretation of current remote sensing data (spectroscopy in the
visible, infrared to passive microwave) but also for planetary exploration when
designing a lander, a rover or a cryobot. In situ exploration of the ice crust
would require knowledge about subsurface porosity. This study employs a
compaction model solely driven by overburden pressure based on prior research.
The formulation for density as a function of depth, incorporates an essential
parameter: the ice compaction coefficient. To determine this coefficient, we
fit our depth-dependent density model to existing data obtained from
Earth-based measurements of ice cores in Antarctica and North Greenland. Our
results yield a typical lengthscale for ice compaction on Earth of
approximately 20.1 $\pm$ 0.6 m , consistent with the existing literature. We
apply the model to Europa, which due to its lower gravity, has a typical ice
compaction scale of 150 $\pm$ 4 m. We compare it with the depths scanned by
current spaceborne data and find that porosity can be considered constant when
accounting only for gravity-induced compaction.
