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Seismology allows for direct observational constraints on the interiorstructures of stars and planets. Recent observations of Saturn's ring systemhave revealed the presence of density waves within the rings excited byoscillation modes within Saturn, allowing for precise measurements of a limitedset of the planet's mode frequencies. We construct interior structure models ofSaturn, compute the corresponding mode frequencies, and compare them with theobserved mode frequencies. The fundamental mode frequencies of our models matchthe observed frequencies (of the largest amplitude waves) to an accuracy of$\sim 1 \%$, confirming that these waves are indeed excited by Saturn'sf-modes. The presence of the lower amplitude waves (finely split in frequencyfrom the f-modes) can only be reproduced in models containing gravity modesthat propagate in a stably stratified region of the planet. The stablestratification must exist deep within the planet near the large densitygradients between the core and envelope. Our models cannot easily reproduce theobserved fine splitting of the $m=-3$ modes, suggesting that additional effects(e.g., significant latitudinal differential rotation) may be important.

Saturn Ring Seismology: Evidence for Stable Stratification in the Deep Interior of Saturn