Intriguing differences and similarities in the surface compositions of the icy Saturnian and Galilean satellites

Many materials in addition to water ice have been discovered in the surfaces of the icy Galilean and Saturnian satellites. Spacecraft infrared spectroscopy show intriguing differences and similarities suggestive of variations in primordial compositions and subsequent alteration. However, within the diverse compositions in their surfaces are similarities that cross between the systems. For instance, when nonice material is detected on these satellites, it is always hydrated. CO2 is detected in both systems where it is trapped in a host material except possibly for Enceladus where it may be deposited as ice from plumes [1-7]. Satellites in both systems contain aromatic hydrocarbons [8] and possibly CN-bearing materials [9]. The surfaces of Callisto, Ganymede, Europa, Iapetus, Phoebe, Hyperion, and Dione each contain some low albedo non-ice materials. The spectra have a broad 3-micron absorption feature due to structural OH or adsorbed water. However, the band is not sharp like a well-ordered clay mineral but broad, similar in some regards to less well-structured palagonite, goethite, or Murchison meteorite. The hydration of Jovian satellite nonice materials is greater for surfaces that have experienced more tectonism and alteration (i.e. increases from Callisto inward to Europa). The nonice material on Callisto appears to be a single composition (though itself possibly a mixture) that is slightly hydrated [10]. The nonice material on Europa is also of uniform composition everywhere observed, a very heavily hydrated material, perhaps a salt, hydrated SO4 (i.e. sulfuric acid), or both, that either originates from the subsurface ocean, radiolytically altered surface material, or both [11-13]. Ganymede appears to contain two types nonice materials; one an unidentified heavily hydrated material spectrally distinct from the Europa hydrate [11] and a second much less-abundant, less hydrated material spectrally similar to the Callisto nonice material that is largely associated with dark ray craters, possibly impactor contamination or desiccated Ganymede hydrate. The nonice materials on Phoebe and Iapetus is redder (from 1-2.5 microns) than the reddest material on the Galilean satellites (on Callisto) and compositionally different from each other. Iapetus appears to contain some (more) tholin material than Phoebe [14]. The CO2 on both satellites is similar to the CO2 detected in the nonice materials on Callisto and Ganymede with a reflectance minimum ~ 4.258 microns. The spectrum of the CO2 detected on Hyperion and Dione is distinct from that on Iapetus and Phoebe, having a reflectance minimum 10nm shorter at ~ 4.246 microns. This suggests a different bonding energy and possibly a different host material. In summary, the compositions of the icy Galilean satellites reflect the evolutionary state of their surfaces. The compositions of the icy Saturnian satellites are also complex, but with the exception of Enceladus, do not yet show any obvious dependencies on surface structure. There may some commonality in primordial compositions between the satellites of the two systems. References: [1]1Carlson et al., (1996) Science; [2] McCord et al., (1998) J. Geophys. Res.;[3] Hibbitts et al., (2000), J. Geophys. Res; [4] Hibbitts et al., (2003) J. Geophys. Res; [5] Clark et al., (2005) Nature; [6] Buratti et al., (2005) Astrophys. J.; [7] Brown et al., (2006) , Icarus; [8] Clark et al., (2005), Fall AGU; [9] Cruikshank et al., (2005), DPS [10] Calvin et al., (1991), Icarus; [11] McCord et al., 2000; [12]Carlson et al., 1999; [13]Orlando et al., (2005) Icarus; [14] Owens et al., (2001) Icarus;.