Abstract
Shock wave data, thermodynamic and phase diagram data for ice, porous ice, and water are taken together with a Rice-Walsh-Bakanova equation of state to define the shock pressures and impact velocities required to induce incipient melting (IM) (6 GPa), complete melting (CM) (10 GPa), and passage through the vapor-liquid critical point (CP) upon isentropic release (22.5 GPa). Upon expanding along the isentrope which passes through CP ~0.61 kPa (6.1 mbar) is achieved. Below this pressure, ice sublimates and ~0.4 mass fraction H2O gas is in equilibrium with ice I. The minimum impact velocity required to induce IM, CM, and isentropic release through CP is 2.1, 3.0, and 4.5 km/sec for silicate impactors. For icy projectiles, Hugoniot states achieved in icy targets or projectiles depend only weakly on initial temperature of ice. The IM, CM, and CP isentropes are achieved upon impacting with an icy projectile an icy surface at velocities of 3.4, 4.4, and 7.2 km/sec, respectively. We observe that at a partial H20 pressure below 0.61 kPa and temperatures below 273K, ice partially vaporizes and requires ~3000 kJ/kg of heat of vaporization for complete sublimation. We examine the hypothesis that the smaller satellites of Saturn having mean densities in the 1.1 to 1.4 Mg/m3 range represent primordial accreted planetesimal condensates (60% (wt.) H2O, and 40% (wt.) silicate) formed in the proto-Jovian and Saturnian accretionary planetary discs. These densities are in the range expected for water-ice/silicate mixtures constrained to the solar values of O/Si and O/Mg atomic ratios. If the large satellites accreted from the same group of planetesimals which formed the small Saturnian satellites, impact vaporization of water upon accretion into a porous regolith at low H2O partial pressure can account for the increase in mean planetesimal density from 1.6 Mg/m3 (43% H20 + 57% silicate) to a mean planetary ,density of 1.9 Mg/m3 for Ganymedean-sized water-silicate objects. If impact-volatilization of initially porous planetesimals is assumed, we demonstrate that starting with planetesimals composed of 54% H2O and 40% silicate (1.35 Mg/m3) partial devolatilization upon accretion will yield a Ganymede-sized planet, having a radius of 2600 km and a density of 1.85 kg/m3, similar to that of Ganymede, Callisto, and Titan.
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Ahrens, T.J., O’Keefe, J.D. (1985). Shock Vaporization and the Accretion of the Icy Satellites of Jupiter and Saturn. In: Klinger, J., Benest, D., Dollfus, A., Smoluchowski, R. (eds) Ices in the Solar System. NATO ASI Series, vol 156. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5418-2_43
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DOI: https://doi.org/10.1007/978-94-009-5418-2_43
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