Shape, Mean Radius, Gravity Field, and Interior Structure of Callisto

By J. Anderson, R. Jacobson, T. Mcelrath, W. Moore, Gerald Schubert, P. Thomas. 2001

201 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/cc5bc8332a180d16354fe5a7f6efe3a471e7adfc

How researchers see this paper

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

In Aerospace Engineering

1. William McKinnon
2. J. Anderson
3. Gerald Schubert
4. Tilman Spohn
5. Mark A. Wieczorek
6. Christophe Sotin
7. Gabriel Tobie
8. F. Nimmo

In Astronomy and Astrophysics

1. William McKinnon
2. J. Anderson
3. Tilman Spohn
4. Mark A. Wieczorek
5. Gerald Schubert
6. P. Thomas
7. W. Ward
8. R. Canup

Citations in the corpus

• Interior composition, structure and dynamics of the Galilean satellites (2004, background): “At least for Callisto, the inferred existence of an ocean is surprising since this satellite is incompletely differentiated (Anderson et al. 2001c, Sohl et al. 2002) and devoid of endogenic activity (as witnessed by its old surface).”
• Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2009 (2011, methodology): “Sizes and shapes have been updated in Table 5 for the Galilean satellites of Jupiter based on Thomas et al. (1998) (Io); Anderson et al. (2001a) (Ganymede), Anderson et al. (2001b) (Callisto), and Nimmo et al. (2007) (Europa).”
• Formation of the Galilean Satellites: Conditions of Accretion (2002, background): “The most recent measurements (Anderson et al. 2001) of the moment of inertia of Callisto find I=MR2 0:3549 0:0042, i.e., too small for a homogenous Callisto ðI=MR2 0:4Þ, but too large for a completely differentiated object according to two- and three-layer interior models that assume hydrostatic…”
• Gravity and Topography of the Terrestrial Planets (2015, background): “Thus, although regional topographic models have been constructed for some moons and asteroids (such as Phobos (Wählisch et al., 2010), 433 Eros (Gaskell et al., 2008; Zuber et al., 2000a), Itokawa (Abe et al., 2006; Gaskell et al., 2008), Vesta ( Jaumann et al., 2012), Ganymede (Giese et al., 1998)”
• Oceans in the icy Galilean satellites of Jupiter (2002, background): “This limitation does not apply to Ganymede and Callisto, whose bulk densities and moment of inertia factors indicate a thick water shell (e.g., Anderson et al., 2001; Sohl et al., 2002).”