The concept of Earth as the sole body in the Solar System with liquid water that can harbor microbial life has been overturned by the discovery of multiple 'ocean worlds'. The Solar System is home to several planetary bodies with subsurface oceans of liquid water, including icy satellites such as Europa, Ganymede, Callisto, Enceladus, Titan and Triton, as well as dwarf planets like Pluto, and chief among these ocean worlds, the Earth. Furthermore, new icy and ocean worlds are being continuously discovered in other planetary systems as well. Like Earth, the exploration of these oceans includes both aspects of planetary evolution and habitability. The geodynamic role of oceans in planetary evolution is thus a crucial aspect of understanding not only planet formation, but the onset of biological activity as well. In what ways can the oceans of Earth serve as analogs for other oceans of the Solar System? What instrumentation can be implemented on the Earth now to further our understanding of these ocean worlds, and what technological advances might we expect in future exploration of subsurface liquid water environments beyond Earth?

This session focuses on analog sites, laboratory simulation, modeling, instrumentation and mission proposals. Coordination between Earth, marine and planetary science communities is encouraged, as well as emphasis on upcoming (e.g. JUICE and Dragonfly) and proposed missions (e.g. Enceladus Orbilander). Analog sites might encompass either geological or biological themes in the broader frame of habitability. Interfaces of ice-water (e.g. underside of floating ice shelfs and subglacial lakes), clathrate-water (e.g. ocean floor sediments, veins/fractures/faults, layered horizons and atmosphere particulates), seafloor-ocean, and rock-ice (i.e. glaciers) are of particular curiosity. Instrumentation includes sensors, buoys, submersibles, drilling and coring, as well as satellite instrumentation (e.g. spectrometers, magnetometers and gravimeters).