Tidal dissipation within large icy satellites: Applications to Europa and Titan

By Gabriel Tobie, A. Mocquet, Christophe Sotin. 2005

225 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/45f51b2e58a0555ef965152eec486decefec855f

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. F. Nimmo
2. John H. Roberts
3. Kaizhong Zhang
4. P. Thomas
5. Jonathan I. Lunine
6. J. Castillo‐Rogez
7. Christophe Sotin
8. T. Guillot

In Geophysics

1. F. Nimmo
2. John H. Roberts
3. Kaizhong Zhang
4. P. Thomas
5. J. Castillo‐Rogez
6. Christophe Sotin
7. Gaël Choblet
8. Gabriel Tobie

In Molecular Biology

1. F. Nimmo
2. John H. Roberts
3. Kaizhong Zhang
4. Gary A. Glatzmaier
5. B. Buffett
6. U. Christensen

Citations in the corpus

• Iapetus’ geophysics : rotation rate, shape, and equatorial ridge (2007, methodology): “At the low temperatures (<200 K) in the early history of the satellite, a Maxwell model tends to greatly overestimate the dissipation factor whereas other models might be more accurate (Tobie et al., 2005).”
• Long-Term Stability of a Subsurface Ocean on Enceladus (2007, methodology): “Following Sabadini and Vermeersen (2004) and Tobie et al. (2005), we have treated Enceladus as a Maxwellian viscoelastic solid [see Eq.”
• Tidal heating in icy satellite oceans (2014, background): “…dissipation are typically calculated assuming a viscoelastic rheology, such as Maxwell, Andrade or Burgers (e.g. Ross and Schubert (1989); Tobie et al. (2005); Efroimsky and Williams (2009); Castillo-Rogez et al. (2011); Nimmo et al. (2012)), though other processes (such as frictional…”
• New constraints on Saturn’s interior from Cassini astrometric data (2015, methodology): “The viscoelastic deformation in the solid viscoelastic core is computed using the compressible elastic formulation of Takeuchi & Saito (1972), adapted to viscoelastic media (see Tobie et al., 2005 for more details).”
• Enceladus's internal ocean and ice shell constrained from Cassini gravity, shape, and libration data (2016, background): “…ice shell, except in the SPT. Due to the small size of Enceladus, the amplitude of tidal deformation is very sensitive to the ice shell thickness, which contrasts with big moons like Europa or Titan, where tidal deformation only slightly depends on ice shell thickness [e.g., Tobie et al., 2005].”