Jupiter's Dusty Rings

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Jupiter’s Dusty Rings Faint, dusty rings: Made of micron-sized dark dust particles. –12 Mass is <10 ME Sources: Material knocked of small moons by meteoritic impacts Captured debris from comets Jovian Ring System (schematic) Saturn Ring System 67,000 km to 140,000 km (1.1 – 2.3 RSaturn) ~30m thick Water ice particles ~1 cm to ~3 m (pebbles to boulders) Main rings are inside Saturn’s Roche Radius for icy bodies Earth from Cassini 2013 July 19 Earth from Saturn Saturn’s Rings backlit by the Sun (Cassini) Cassini Division Cassini 2:1 resonance with Mimas Division Mimas Encke Gap Keeler Gap Encke Gap Thin Rings of Uranus Dark, narrow rings only a few km wide. Wide “epsilon ring” is only ~100 km wide. ε Ring Uranus’ Rings back-lit by the Sun (Voyager 2) Neptune’s Rings Adams Ring Galle Ring LeVerrier Ring Arcs in the Adams Ring Liberté Egalité Fraternité Iceball-moon encounter: Iceball on an inner (faster) orbit Overtakes the moon and is deﬂected towards the moon After the encounter, the ice ball falls back and oscillates around its original orbit But as it passes back into the ring, it hits other iceballs, damping the oscillation By the next encounter, it is back on its original orbit Reference frame of Saturn To Saturn Reference frame of the gap moon Keeler Gap – cleared by small moon Daphnis Thin rings can be gravitationally conﬁned by a pair of “shepherd moons” Shepherd moons of Saturn’s F-ring Pandora Prometheus http://photojournal.jpl.nasa.gov/animation/PIA07712 Close up of Prometheus and the F-Ring Shepherd Moons of Uranus’ Opheli Epsilon Ring a Cordeli a .

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Cassini Update
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