The interiors of inner Saturnian moons observed with the Cassini interferometer (ISS) satellite imaging system (CASINO). I. Observational constraints
Some of the authors are Lainey, Rambaux, Cooper, N., and Zhang. Characterizing the interior of five inner Saturnian moons using Cassini ISS data. Astron. Astrophys. 670, L25 (2023).
Viswanathan, V., Rambaux, N., Fienga, A., Laskar, J. & Gastineau, M. Observational constraint on the radius and oblateness of the lunar core–mantle boundary. Geophys. Res. Lett. 46, 7 295–303 was published this year.
Tobie, G., Grasset, O., Lunine, J. I., Mocquet, A. & Sotin, C. Titan’s internal structure inferred from a coupled thermal–orbital model. Icarus 175, 496–502 (2005).
Noyelles, B., Baillié, K., Charnoz, S., Lainey, V. & Tobie, G. Formation of the Cassini Division—II. Possible histories of Mimas and Enceladus. Mon. Not. R. Astron. Soc. 486, 2947–2963 (2019).
Zandanel, A. et al. Implications for hydrogen production are associated with short lifespans of serpentinization in the rocky core. The book is titled “Incisors 409, 114411.”
Source: A recently formed ocean inside Saturn’s moon Mimas
Caviar – A software package for the simulation of small Saturnian inner moons. Astronomy, physics, and tidal history
Cooper, N. J. et al. The description and examples of the Caviar software package can be found here. Astron. Astrophys. 610, A2 (2018).
Rambaux, N., Lainey, V., Cooper, N., Auzemery, L. & Zhang, Q. F. Spherical harmonic decomposition and interpretation of the shapes of the small Saturnian inner moons. Astron. Astrophys. 667, A78.
Rambaux, van Hoolst, and Karatekin analyzed the response of Europa, Callisto and Ganymede to the ocean. Astron. Astrophys. 527, A118 (2011).
The elasticity of a 3-layer Titan perturbed by non- keplerian and atmospheric couplings was studied. We are a planet. Space Sci. 93, 22–34 (2014).
Castillo-rogez, Efroimsky, M. and Lainey are related. The tidal history of Lapetus: spin dynamics in the light of a refined dissipation model. J. Geophys. The Res. 1160900 and E8 were published in 2011.
In the 2024 study, Lainey and his colleagues seem to have nailed the case. They went deeper than they did in the first half of the year by looking at other things, such as how Mima’s rotation changed over time. The team combined Cassini observations with simulations of Mimas’s interior and its orbit to conclude that there must be an ocean 20–30 kilometres below Mimas’s surface.