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12 - Formation & Evolution of the Solar System

12 - Formation & Evolution of the Solar System. 4 Terrestrial Planets. Mercury. Venus. Earth. Mars. 4 Jovian Planets. (ice giants). Uranus Neptune. Jupiter Saturn. (gas giants). Terrestrial Mercury Venus Earth Mars Small Diameters Small Masses

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12 - Formation & Evolution of the Solar System

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  1. 12 - Formation & Evolution of the Solar System

  2. 4 Terrestrial Planets Mercury Venus Earth Mars

  3. 4 Jovian Planets (ice giants) Uranus Neptune Jupiter Saturn (gas giants)

  4. Terrestrial Mercury Venus Earth Mars Small Diameters Small Masses Large Densities Few Moons No Rings Rock & Metals Jovian Jupiter Saturn Uranus Neptune Large Diameters Large Masses Small Densities Many Moons Rings H, He, (C, N. O) Differences in the 2 Main Classes of Planets To Sun

  5. Numerous moons, asteroids, comets, “Kuiper belt objects”, “centaurs”, and Pluto (actually a KBO) Ganymede Hyperion Titan Eros Kuiper Belt Hale-Bopp

  6. Formation & Evolution of the Solar System Planets, asteroids (minor planets), Kuiper Belt Objects (another form of minor planet) General Structure

  7. Planets gradually form out of the rotating disk of gas & dust Beyond the “frost line” ice can condense, allowing more massive planets to form Nebular Model Refractories (rock, metal) volatiles (ices & gas) and refractories

  8. Two possible sequences of formation of terrestrial (rocky) planets: • Merge homogeneous collection of planetesimals, then differentiate • Form planets while condensation is still happening

  9. Do the Big Planets form Differently?

  10. Asteroids, also called Minor Planets Same as planetesimals that formed the terrestrial planets • Meteorites are pieces of asteroids that have made it to Earth. Type: • Stony • Iron • Stony-Iron • Some stony ones • contain organics Ida, with its moon Dactyl

  11. Sampling the Early Solar System

  12. Kuiper Belt & Oort Cloud

  13. Kuiper Belt ObjectsTrans-Neptunian Objects Eris & Dysnomia (official names) (Eris) Eris (larger than Pluto)

  14. Comets Comet Hale-Bopp C/2002 Q2 NEAT

  15. forsterite (Mg2SiO4)

  16. Comet Dust Silicates “CHON” Comet Gases H, O, OH, CN, CH, NH2, C2, C3, CO, CH3OH (methanol), HCN (hydrogen cyanide), H2O, H2S, CS, H2CO (formaldehyde), CH3CN, HNC, etc. Giotto spacecraft image of the nucleus of Comet Halley (1986)

  17. Interplanetary Dust Particles shed by comets & collected in Earth’s atmosphere - silicates & organics

  18. Stardust Spacecraft @ Comet Wild 2 in Jan. 2004Returned to Earth with Dust Sample in Jan. 2006 Captured forsterite (Mg2SiO4) grain!

  19. Deep Impact - Comet Tempel 1

  20. Deep Impact spectral analysis

  21. Comet 73P/Schwassmann-Wachmann 3 Fragmented in 1995 Seen again in 2000

  22. 2006 - Returned In Many Pieces! Deep Impact-like analysis in preparation - Sitko et al.

  23. Eruption of Comet 17P/Holmes in 2007 Deep Impact-like analysis in preparation - Lisse et al.

  24. While many details are not yet known: • basics of the formation of the SS is understood • chemical/mineral content of early SS becoming known • no unusual or “freak” events necessary • the early SS had organics • we see the same things around other stars • We expect planetary systems to be common, and many may be similar to our own

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