Physico-chemical models of the internal structure of partially differentiated Titan

The Liquidus Temperature for Methanol‐Water Mixtures at High Pressure and Low Temperature, With Application to Titan

“…Important impurities likely include ammonia, but methanol may also be present (Hogenboom et al, 1997;Kargel, 1992) and is included in models such as Neveu et al (2017), Dunaeva et al (2016), Lefevre et al (2014), Fortes (2012), Tobie et al (2012), Davies et al (2010), and Deschamps et al (2010). Important impurities likely include ammonia, but methanol may also be present (Hogenboom et al, 1997;Kargel, 1992) and is included in models such as Neveu et al (2017), Dunaeva et al (2016), Lefevre et al (2014), Fortes (2012), Tobie et al (2012), Davies et al (2010), and Deschamps et al (2010).…”

“…Detailed models of the interior of Titan rely on the properties of aqueous solutions at the low temperatures and high pressures found within such an ocean, and such properties would be affected by the presence of impurities. Important impurities likely include ammonia, but methanol may also be present (Hogenboom et al, 1997;Kargel, 1992) and is included in models such as Neveu et al (2017), Dunaeva et al (2016), Lefevre et al (2014), Fortes (2012), Tobie et al (2012), Davies et al (2010), and Deschamps et al (2010). More broadly, methanol is also an important volatile found in the outer solar system nebula (Sekine et al, 2014), on the surfaces of some trans-Neptunian objects (Merlin et al, 2012), and in some star-forming regions (Dartois et al, 1999;Shimonishi et al, 2016).…”

Thermal evolution of trans‐Neptunian objects, icy satellites, and minor icy planets in the early solar system

“…This could indicate that the satellite is either partially differentiated having an ice–rock mixture in its interior (Dunaeva et al. ), or it has a hydrated core deep inside the fully differentiated satellite (Iess et al. ; Fortes ; Mitri et al.…”

“…Titan, the largest satellite of Saturn with a size comparable to Ganymede, has a larger MoI of~0.34 as compared to Ganymede (Iess et al 2010). This could indicate that the satellite is either partially differentiated having an ice-rock mixture in its interior (Dunaeva et al 2016), or it has a hydrated core deep inside the fully differentiated satellite (Iess et al 2010;Fortes 2012;Mitri et al 2014). The Cassini mission also detected powerful gravitational tides of Titan, which suggests the presence of water ocean beneath the surface of the satellite (Iess et al 2012).…”