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- W1619024858 abstract "Introduction: Despite similar sizes and mean densities, the surfaces and interiors of Jupiter’s large ice/rock satellites Ganymede and Callisto suggest that they have followed different evolutionary pathways. Ganymede shows signs of global endogenic resurfacing [1], but Callisto’s surface is ancient and shows no signs of resurfacing [2]. Ganymede’s low moment of inertia suggests complete ice/rock separation [3], but Callisto’s higher moment of inertia suggests incomplete ice/rock separation in its interior [3,4]. Previous work suggests that differences in accretion environment [e.g., 5,6,7,8,9,10], thermal evolution [5, 10], and/or tidal dissipation [11] can create the Ganymede/Callisto dichotomy. In each model, the dichotomy depends on small differences in satellite properties or restrictive evolution scenarios [9,12]. Here, we construct geophysical models of impactinduced ice/rock separation to show that the Ganymede/Callisto dichotomy can be created during an outer solar system “late heavy bombardment” (LHB). Outer Solar System Late Heavy Bombardment: Many of the large impact basins on Earth’s moon have similar ages, suggesting a period of intense bombardment known as the “late heavy bombardment” (LHB), ~700 Myr after the Moon formed. A leading theory for the origin of LHB impactors, the so-called Nice model, suggests that the event was triggered by the early dynamical evolution of the outer solar planets, driven by their interaction with a disk of icy planetesimals. If the planetesimal disk is initially ~35M⊕ (earth-masses), and is whittled down to ~20M⊕ at the time of the LHB, ~10 22 g of icy objects will impact the Moon [13, 14], comparable to the lunar LHB mass estimated from the cratering record [13]. During an outer solar system LHB, Ganymede receives 80x the mass of objects delivered to the Moon, some ~6x10 g of cometary material [13,14,15], delivered at a characteristic impact velocity vi=20 km/s. Callisto experiences fewer impacts at a lower vi=15 km/s. Methods: Impacts. A heliocentric cometary impactor that strikes a moon with a characteristic velocity of ~ tens of km/s creates a shock wave that compresses the satellite’s interior, performing PΔV work on a quasihemispherical region beneath the impact site. At locations where the peak shock pressure exceeds the pressure to melt ice, a buried pool of melt water and ice crystals is created. At locations where the volume fraction of melt exceeds 50% [16, 17, 18], the water/crystal slurry has a viscosity comparable to that of liquid water. In this region, concomitant rock particles > 30 μm sink rapidly to the pool’s base before it solidifies. Figure 1. Heterogeneous density structures inside Ganymede (top) and Callisto (bottom) after the LHB. Colors indicate density." @default.
- W1619024858 created "2016-06-24" @default.
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- W1619024858 date "2010-03-01" @default.
- W1619024858 modified "2023-09-28" @default.
- W1619024858 title "Origin of the Ganymede/Callisto Dichotomy by Impacts During an Outer Solar System Late Heavy Bombardment" @default.
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