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Planetary Atmospheres II: Jupiter and Saturn Comparison

Explore the unique atmospheric characteristics of Jupiter and Saturn, including their temperature balance, cloud formations, internal heat differences, and composition enhancements. Discover how these gas giants differ from other planets in terms of atmospheric dynamics and density variations. Learn about the impact of seasonal forcing on Neptune and the tenuous atmospheres of various planets in our solar system.

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Planetary Atmospheres II: Jupiter and Saturn Comparison

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  1. Where is this?

  2. Planetary Atmospheres II

  3. Jupiter STRATO/MESO: ~ 150K, temp balance heating of photochemical smog cooling by CH4 C2H2 C2H6 8-14 μm TROPO: multiple cloud layers we see convection

  4. Jupiter

  5. Jupiter

  6. Saturn similar to Jupiter, except less convection … weaker internal heat colder by ~ 30K He 12% (Sat) vs. 14% (Jup) vs. 16% (protosun) C, N, S species enhanced by 2-3X puffed out atm results in lower density

  7. 420 nm 628 nm Saturn’s North Pole 939 nm 728 nm

  8. Saturn’s Polar Vortex

  9. Jupiter vs. Saturn: pressure

  10. Jupiter vs. Saturn: height at 1 bar HJup = 24 km HSat = 47 km

  11. Wind Speeds

  12. Neptune and Uranus significant cloud features super bland! internal heat source no internal heat source no NH3 clouds observed (as seen on Jup and Sat) CH4, H2S, and NH4SH clouds instead H + He only ~10% mass of planet, unlike Jup and Sat at ~90%

  13. Uranus HST NICMOS 1998

  14. Neptune Neptune: fastest winds in SS > 2000 km/hr HST

  15. Seasonal Forcing at Neptune 1/900th Earth solar flux: Sun’s effect weaker 165 year orbit: changes slower than Earth obliquity 29o: hemisphere toward Sun brightens temp 59K: cannot reach rapid thermal equilibrium … delayed dynamic response of 15 yr Sromovsky et al. 2002 Icarus 163

  16. atmospheric aerosols created 165 yr cycle UV photons: 11 yr cycle Galactic cosmic rays: 1-2 yr cycle Seasonal Forcing at Neptune Aplin & Harrison. 2016

  17. Jovian Compositions Jupiter Saturn Uranus Neptune at least 1% ppm

  18. Tenuous Atmospheres temporary, due to sputtering --- physical lifting off surface (but not vesc) energetic particles from solar wind energetic particles from nearby planet/magnetosphere micrometeorite bombardment … all 8 tenuous atmospheres capture of solar wind … Mercury, Moon volcanoes (Io … SO2) and/or geysers (Enceladus … H2O … Triton … N2) sublimation of ices … Mars, Io, Triton, Pluto

  19. Clouds Venus H2SO4 (sulfuric acid) evaporates Earth H2O Mars CO2 (high, 50 km) H2O (low, 10 km) Titan hydrocarbon smog CH4 below Jupiter NH3 + NH4SH Saturn H2O “solution cloud” Uranus CH4 + H2S Neptune NH4SH H2O “solution cloud” form on all planets where the temp drops below condensation point of gases in the atmosphere 1. non-equilibrium conditions in atm 2. absorbed incoming radiation heats 3. can alter surface heating pattern 4. can block outgoing infrared photons theoretical for Jovians! NH3 + H2S  NH4SH “solution cloud” = H2O+NH3+H2S note trend: further from Sun … colder more cloud decks

  20. Solar System Explorers 05 for Tuesday, September 25 look over equation sheet be ready to answer a few questions

  21. Solar System Explorers 06 Describe one feature of a non-solar atmosphere in the Solar System that makes it different from EVERY other non-solar atmosphere. (spectral features ok) 1. 2. 3. 4. 5. 6. 7. 8. 9. 10. 11. 12. 13. 14. 15. 16. 17. 18. 19. 20.

  22. …………………………

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