Enceladus' plume: Compositional evidence for a hot interior

By D. Matson, J. Castillo, Jonathan I. Lunine, T. Johnson. 2007

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The composition and structure of the Enceladus plume (2011, background): “, 2006, 2009] along with N2 could indicate internal liquid water temperatures of 500–800 K causing dissociation of NH3, and/or percolation of liquid through hot rock [Matson et al., 2007].”
Ceres’ evolution and present state constrained by shape data (2010, background): “Castillo-Rogez et al. (2007a,b) showed that, depending on the rock mass fraction, the effect of short-lived radioactive isotopes (SLRI), and especially 26Al decay, can tremendously affect the long-term evolution of Iapetus and Enceladus, as was also pointed out for asteroid belt objects by Grimm and”
The pH of Enceladus’ ocean (2015, background): “Understanding the geochemistry of the ocean is critical for advancing our understanding of the origin and evolution of Enceladus (Zolotov, 2007; Matson et al., 2007; Glein et al., 2008; Zolotov et al., 2011); for gaining insights into geochemical processes on other icy bodies in the outer Solar…”
Long-Term Stability of a Subsurface Ocean on Enceladus (2007, background): “The extent to which heat can be dissipated within the silicate core is important for investigating whether localized seas can be generated due to basal heating of the ice shell (Collins and Goodman, 2007) and whether ammonia can be broken down to form the N2 observed in the plume (Matson et al., 200”