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SATURN’S RINGS

SATURN’S RINGS. Beatriz Frisón Máster en Astrofísica. 1610- Galileo: satellites ? 1655 – Christian Hygens : rigid matter disk 1675– Cassini : Cassini division XVIII- Laplace: thin rings 1857- Maxwell: little mass 1895- Keeler y Campbell: velocity. OBSERVATIONS.

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SATURN’S RINGS

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  1. SATURN’S RINGS Beatriz Frisón Máster en Astrofísica

  2. 1610- Galileo: satellites? 1655 – Christian Hygens: rigidmatter disk 1675– Cassini: Cassinidivision XVIII- Laplace: thinrings 1857- Maxwell: littlemass 1895- Keeler y Campbell: velocity OBSERVATIONS

  3. Alphabeticorderbydiscovery date 9 mainrings. Total ≈ 140 Dense rings: 7,000 km – 80,000 km (Req) Thickness≈ 10m – 30,000km Total Mass = 3 x 1019 kg ?? Thingaps &ringlets MAIN CHARACTERISTICS

  4. MAIN RINGS STRUCTURE

  5. Frominsidetooutside: • D ring: faint, small. Ringlets • C ring: • Inner: Colombo Gap, TitanRinglet • Outer: Maxwell Gap, Maxwell Ringlet • B ring: brilliant, massive • CassiniDivision: 2:1 Mimas • Huygens Gap: innerborder, 2:01 Mimas • A ring: Atlas. 7:06 with Jano and Ephimeteo. • Encke Gap: Pan inside • Keeler Gap: Dapthnisinside • RockeDivision • F ring: thick, shepherdmoons(Prometeus, Pandora). INNER RINGS

  6. Frominsidetooutside: • Janus/ Epimetheus ring: faint, 5,000 km • G ring: thin, • Ring arc at 7:6 Mimas (Aegaeon) • Methone Ring arc: 14:15 Mimas • AntheArc Ring: 10:11 Mimas • PaleneArc Ring: 2500 km • E Ring: from Mima toRhea. OUTER RINGS

  7. 06/10/2009 – Spitzer i = 27˚ R= 6 -12 x 106 km Thickness: 20 Dsaturn PHOEBE RING Phoebeinside

  8. Above: Waves in Saturn's A ring. The bands in the lower left are spiral density waves, and the bands in the upper right are bending waves. This image was taken by the Cassini spacecraft in 2004. (Saturn is off to the lower left.) RING WAVES

  9. 99% ice Tolins Silicates ThinAtmosphere: O2, H2, OH COMPOSITION

  10. Roche: satellite – tidalforzes Nebular material Canup RM theory RINGS FORMATION THEORIES

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