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We present a review of Saturn's interior structure and thermal evolution,with a particular focus on work in the past 5 years. Data from the Cassinimission, including a precise determination of the gravity field from the GrandFinale orbits, and the still ongoing identification of ring wave features inSaturn's C-ring tied to seismic modes in the planet, have led to dramaticadvances in our understanding of Saturn's structure. Models that match thegravity field suggest that differential rotation, as seen in the visibleatmosphere, extends down to at least a depth of 10,000 km (1/6$^{\rm th}$ theplanet's radius). At greater depths, a variety of different investigations allnow point to a deep Saturn rotation rate of 10 hours and 33 minutes. There isvery compelling evidence for a central heavy element concentration (``core''),that in most recent models is 12-20 Earth masses. Ring seismology stronglysuggests that the core is not entirely compact, but is dilute (mixed in withthe overlying H/He), and has a substantial radial extent, perhaps out to aroundone-half of the planet's radius. A wide range of thermal evolution scenarioscan match the planet's current luminosity, with progress on better quantifyingthe helium rain scenario hampered by Saturn's poorly known atmospheric heliumabundance. We discuss the relevance of magnetic field data on understanding theplanet's current interior structure. We point towards additional future workthat combines seismology and gravity within a framework that includesdifferential rotation, and the utility of a Saturn entry probe.

Saturn's Interior After the Cassini Grand Finale