Lecture #11: Plan. Terrestrial Planets (cont d) Jovian Planets

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1 Lecture #11: Plan Terrestrial Planets (cont d) Jovian Planets

2 Mercury (review) Density = 5.4 kg / liter.. ~ Earth s Rocky mantle + iron/nickel core Slow spin: 59 days (orbital period = 88 days) No satellites No atmosphere: T day = 800 F / 700 K T night = -280 F / 100 K

3 Mercury R ~ 0.4 R E Heat loss more efficient than Earth s M ~ 0.06 M E Less radioactive heating than Earth Cooler interior No plate activity few volcanoes in the past

4 Mercury few volcanoes Virtually no gas production Low escape velocity Gas escapes easily + Proximity to Sun Any gas would be hot & escape easily No Atmosphere!

5 Venus Density = 5.3 kg / liter.~ Earth s Rocky crust & mantle + iron/nickel core Very thick atmosphere 96.5% CO 2 Clouds of sulfuric acid! T surface = 900 F / 750 K (hot enough to melt lead!) Slow & retrograde spin 243 Earth days tilt of spin axis = 177 o Collision???

6 Images of Venus from Russian Venera spacecraft The spacecraft only lasted about an hour due to the extreme temperatures and pressure!

7 Recent radar map of Venus Surface of Venus seems to be relatively young Volcanic activity resurfaces the planet rapidly Few impact craters, due both to the thick atmosphere and volcanic activity

8 Venus R ~ 0.95 R E Heat retention ~ Earth s M ~ 0.8 M E Radioactive heating ~ Earth s Hot interior limited plate activity Many hot spots Many volcanoes

9 Venus Many volcanoes Abundant gas (e.g., CO 2 ) production Escape velocity ~ Earth s Gas retention ability ~ Earth s Thick atmosphere! (100 x Earth s atmospheric pressure!) Very strong greenhouse effect Water rain didn t pick up CO 2 from atmosphere because Venus is too close to the Sun (H 2 O is photodissociated)!

10 Density ~ 4 kg / liter Rocky crust & mantle + iron/nickel core (?) Spin period & tilt ~ Earth s Mars

11 Mars R ~ 0.5 R E Heat loss is more efficient than Earth s M ~ 0.1 M E Radioactive heating is less than Earth s Moderately hot interior limited plate activity Some volcanoes

12 Mars Some volcanoes Some gas (e.g., CO 2 ) production Escape velocity lower than Earth s Gas retention ability < Earth s thinner atmosphere (95% CO 2, 3% N 2 ) weaker greenhouse effect T average = -67 F (T day = 50 F) (strong seasonal changes due to tilt = 25.2 o )

13 Polar Ice Caps CO 2 + H 2 O ice Size of caps varies with seasons

14 Canyons Example: Valles Marineris 5000 km long 100 km wide 10 km deep Rift? Plate activity?

15 Volcanoes Few but big! Olympus Mons 25 km high!

16 Desert / Dunes with dust storms!

17 Currently a dry, dusty place Plains covered with rocks ranging from pebble-sized to boulder sized! The Surface of Mars

18 Channels Carved by liquid water billions of years ago! Mars was once wet and warmer

19 Splash Craters

20 Gullies

21 Streaks: Liquid Water?

22 Where did H 2 O of Mars go? 1. Impact of huge asteroid?! vaporized H 2 O? 2. Slow loss of gas because of low escape velocity Lost gas was not fully replenished by volcanic activity Greenhouse effect became weaker Atmosphere and surface cooled Loss of H 2 O to surface & subsurface ice

23 Comparative Planetology Mercury Venus Earth Mars Distance (AU) Radius Mass Density (kg/lit) Volcanoes? No Yes Yes Yes Plate Activity none some much little

24 Comparative Planetology

25 Comparative Planetology Venus Earth Mars Temperature too hot just right too cold H 2 O in atm? No Yes No (evaporated & (frozen ice) UV photodissociated) Greenhouse Effect? Runaway! Moderate Weak (too much CO 2 ) (ok) (too little) On Earth: (1) rain picks up CO 2 from atmosphere (2) plants also transform CO 2 O 2

26 Temperatures are cold enough that water vapor can condense into ices Outer planets are primarily composed of hydrogen and ices These planets have no surfaces! The Outer Planets

27 Jupiter and Saturn Jupiter 5 AU from the Sun 11x Earth s diameter 300x Earth s mass Density ~ 1.3 kg / liter Saturn 9.5 AU from the Sun 9.5x Earth s diameter 100x Earth s Mass Density ~ 0.9 kg / liter < 1!

28 Jupiter Parallel bands of clouds 90% H 2, 10% He, traces of methane, ammonia and water Rotates once every 9.9 hrs Visibly flattened!

29 Saturn Parallel bands of clouds Similar to Jupiter s, but partly hidden beneath frozen ammonia 96% H 2, 4% He, traces of H-rich compounds Rotates once every 10.7 hrs Even flatter than Jupiter!

30 Jupiter & Saturn: Interior Heating More heat radiated than received from Sun Might be leftover heat from formation, or shrinkage! Heating stirs liquid interior & atmosphere Generates wind currents, vortices in atm (Great Red Spot)

31 The Great Red Spot This storm has lasted for at least 300 years!

32 Uranus & Neptune Uranus 19 AU from the Sun 4x Earth s diameter 15x Earth s mass Density ~ 1.2 kg / liter Neptune 30 AU from the Sun 3.8x Earth s diameter 17x Earth s mass Density ~ 1.7 kg / liter

33 Atmospheres of Uranus & Neptune Rich in hydrogen and helium Bluish color from methane Neptune radiates more heat than it receives from Sun, but not Uranus Uranus is featureless Neptune had the Great Dark Spot; another dark spot has appeared in the northern hemisphere

34 Uranus: Rotation & Orbit 17 hrs 84 yrs Rotation axis is tilted by 90 o (due to a collision???) Consequences: bizarre seasons & length of day

35 Satellites in the Outer Solar System Ring Captured Moons Ring Ring Ring Galilean.. satellites

36 Satellite Properties Satellites with D > 400 km Strong enough gravity to pull themselves into a spherical shape Low densities mostly ice and rock Produced at the same time as the planet or later captured

37 Jupiter s Moon Io

38 Activity #5 Why do we think that Mars was once wet (with liquid water running on its surface)?

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