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Neptune and Triton

Neptune and Triton. Bit of Administration …. Reading BSNV Chap. 12 Homework 9 Due Friday, April 23, in box by Mathieu office door (6522) Sterling Change in Portfolio Points and Course Grade Scale Portfolio is worth 50 pts instead of 70 Same as 6- and 12-week exams

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Neptune and Triton

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  1. Neptune and Triton

  2. Bit of Administration …. • Reading • BSNV Chap. 12 • Homework 9 • Due Friday, April 23, in box by Mathieu office door (6522) Sterling • Change in Portfolio Points and Course Grade Scale • Portfolio is worth 50 pts instead of 70 • Same as 6- and 12-week exams • Course grade scale will be same percentages • A 342/380 • AB 332 • B 285 • BC 275 • C 228 • D 190

  3. Plate tectonics is critical to Earth atmosphere Planetary Evolution • Comparative Planetology - Earth Ozone O3 washed out with H20 rain

  4. Planetary Evolution • Comparative Planetology - Mars at 1 billion yr • (end of geologic activity) UV O,C H2O rain washes CO2 into surface - permanently Greenhouse effect reduced Colder temperatures lead to enhanced rain, less gaseous CO2, less greenhouse (“Runaway Icehouse Effect”) Most CO2 in carbonate rocks, most H2O in permafrost UV sunlight breaks up molecules and provides energy of escape

  5. Planetary Evolution • Comparative Planetology - Earth and Venus • VenusEarth • Active volcanos Active volcanos

  6. Planetary Evolution • Comparative Planetology - Earth and Venus • VenusEarth • Active volcanos Active volcanos • Vesc = 10.3 km/sec Vesc = 11.2 km/sec • CO2 atmosphere N2/O2 atmosphere • (90 atmos) (1 atmos) • Dry (10-4 Earth H20) Water at present • Note: Based on measurements of deuterium (“heavy water”) • Venus had substantially more water in the past • Consistent with outgassing from volcanos and large • escape velocity

  7. Light from Sun or CO2, H2O from rocks from oceans Planetary Atmospheres • Comparative Planetology - Venus • Suppose Venus were “Earth-like” (liquid water) and … Temperature CO2, H2O “Runaway Greenhouse Effect”

  8. Planetary Atmospheres • Runaway Greenhouse Effect • once RGE begins … Escape H2 UV from Sun H20 in atmos RGE + O2 Surface Compounds Irreversible!!

  9. Planetary Atmospheres • Comparative Planetology - Venus at 4.5 billion yr Dry (10-4 Earth H20)

  10. Planetary Evolution - Summary Earth 77% N2, 21% O2 15 oC 1 atmosphere Mars 95% CO2 -50 oC 0.01 atmospheres Venus 96% CO2 470 oC 90 atmospheres Mercury Trace of He, Na, O Moon Trace of He, Na, Ar

  11. Atmospheric Evolution • Moon, Mercury - low escape velocity, hot, atmos escapes • Venus RGE, massive CO2 atmos • Earth CO2, H2O , N2 N2, O2 • Mars Runaway Icehouse, • thin CO2 atmos Planetary Evolution - Summary • Geological Evolution • Mercury, Moon - smallest radii => dormant, cratered • Mars - active for 109 yr, now dormant (shield volcanoes) • Venus - current volcanos (shield volcanoes) • Earth - convection => plate tectonics

  12. Jovian Planets

  13. Jovian Planets (Methane, Ammonia at surface) (Methane, Ammonia at surface) Methane CH4, Ammonia NH3 2.5 x rest of Solar System (excepting Sun)

  14. Jovian Planets • Rotation • Jupiter - 9 hours, 55 minutes at equator • Saturn - 10 hours, 20 minutes • Differential • Rotation

  15. Jovian Planets • Rotation • Jupiter - 9 hours, 55 minutes at equator • Saturn - 10 hours, 20 minutes • Oblateness and Internal Structure • Jupiter - 4% in solid core (13 x Earth mass) • Saturn - 26% in solid core

  16. Jovian Planets • Oblateness and Internal Structure - Jupiter

  17. Jovian Planets • Jovian Weather

  18. Jovian Planets • Jovian Weather

  19. Jovian Planets • Jovian Weather Infrared Visible Jupiter emits 2x the energy it receives from the Sun!

  20. Jovian Planets • Jovian Weather Convection

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