Iapetus’ geophysics : rotation rate, shape, and equatorial ridge
By J. Castillo‐Rogez, D. Matson, Christophe Sotin, T. Johnson, Jonathan I. Lunine, P. Thomas. 2007
142 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics, Geophysics
View Paper: https://www.semanticscholar.org/paper/4883c54f7ff75e0dbb8bd6a90e185254dad570e0
How researchers see this paper
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In Astronomy and Astrophysics
- J. Castillo‐Rogez
- L. Dones
- Jean-Loup Bertaux
- P. Thomas
- G. Kovacs
- Stefano Mottola
- Nicolas Gonzalez Thomas
- S. Mathis
In Geophysics
- L. Dones
- P. Thomas
- J. Castillo‐Rogez
- Stefano Mottola
- Matteo Massironi
- Gabriele Cremonese
- Gabriel Tobie
Citations in the corpus
- The primordial nucleus of comet 67P/Churyumov-Gerasimenko (2015, background): “Among these, Iapetus appears to provide the strongest support for the presence of 26Al beyond the snowline and Castillo-Rogez et al. (2007, 2009) constrain the formation time of Iapetus to 3.4–5.4 Myr after CAI.”
- Sizes, shapes, and derived properties of the saturnian satellites after the Cassini nominal mission (2010, background): “Its oblate spheroid shape probably was frozen at a much shorter spin period ( 16 h; Castillo-Rogez et al., 2007).”
- Accretion of Saturn's mid-sized moons during the viscous spreading of young massive rings: Solving the paradox of silicate-poor rings versus silicate-rich moons (2011, background): “Charnoz et al. (2010) introduced the idea that the smallest inner moons could form from the spreading of the rings’ edge while Salmon et al. (2010) showed that the rings could have been initially massive, and so was the ring’s progenitor itself.”
- The pH of Enceladus’ ocean (2015, background): “…which suggests that the inferred lack of a basaltic ocean floor and metal inner core can constrain models of the thermal evolution of Enceladus (Castillo-Rogez et al., 2007b; Schubert et al., 2007; Neveu et al., 2014) and origin of the Saturnian system (Castillo-Rogez et al., 2007a; Canup,…”
- Constructing the secular architecture of the solar system II: The terrestrial planets (2009, unknown): “…the most prominent impact basins on Mars occurred after the disappearance of Martian magnetic field (Lillis et al. 2006, 2007); (iv) impact basins on Iapetus occurred after the formation of its equatorial ridge, which is estimated to have formed between t = 200−800 Myr (Castillo-Rogez et al. 2007).”