1. Jovian Planets: Jupiter and Saturn Shortened Version Feb 15, 2011

2. Jovian Planets (Gas Giants) 12,757 km (1 D E ) 142,984 km (11 D E ) 120,536 km (9.4 D E ) 51,118 km (4.0 D E ) 49,528 km (3.8 D E ) The outer planets are much bigger than the terrestrial ones, and are gigantic low-density gas balls unlike the high density rocky terrestrial planets. 2

3. Distance Comparison 1 AU 5.2 AU9.6 AU 19.2 AU30.1 AU 3.7% as much sunlight as Earth 1.1% as much sunlight as Earth 0.3% as much sunlight as Earth 0.1% as much sunlight as Earth Sun 3

4. Jupiter: Atmosphere 3 - Composition 1930s (Rupert Wildt) based on low density (1.3 g/cm 3 ), suggests primarily made of Hydrogen (H) and Helium (He) Confirmed by spacecraft in 1970s –Why couldn’t we see spectral lines of H & He from the earth? atmosphere (by mass):75% H, 24% He, 1% other atmosphere + interior:71% H, 24% He, 5% other Note Sun: 73% H, 25% He, 2% other Hence its similar to original solar nebula! 4

5. Jupiter: Storms Great Red Spot –about size of Earth –At largest, has been seen at 3x Earth size –Rotates ccw –more than 300 yrs old White ovals –smaller, less long-lived –also rotate ccw 5

6. Storms in Saturn’s atmosphere seem to be shorter-lived 6

7. Jupiter’s atmosphere is divided into light-colored zones and dark-colored belts. High-speed winds blow eats or west at the boundaries between them. 7

8. Saturn: Atmosphere 3 Composition of clouds same as Jupiter Atmosphere depleted in He (96.3% H, 3.3% He, 0.4% other) => where is missing He? Similar easterly and westerly winds, but at equator, Saturn’s winds are much faster ~1100 miles/hr!!! Wind speed in meters/second 8

9. Jupiter: Belts and Zones Alternating light/dark stripes in atmosphere Convection – warm air rises from below, cools off, then sinks (same as Earth’s troposphere) Rapid rotation stretches these convection cells across the planet 9

10. Saturn: Atmosphere 2 10

11. Internal heat drives convection Jupiter & Saturn radiate more heat than they receive from the sun. Energy from formation (accretion). Saturn being smaller than Jupiter should have cooled off more by now. Helium Rain –Saturn is cold enough that He can condense into droplets –These droplets “rain” down through the H release energy (convert gravitational energy to heat) => Also explains why atmosphere is depleted in He 11

12. The oblateness of Jupiter and Saturn reveals their rocky cores Jupiter probably has a rocky core several times more massive than the Earth The core is surrounded by a layer of liquid “ices” (water, ammonia, methane, and associated compounds) On top of this is a layer of helium and liquid metallic hydrogen and an outermost layer composed primarily of ordinary hydrogen and helium Saturn’s internal structure is similar to that of Jupiter, but its core makes up a larger fraction of its volume and its liquid metallic hydrogen mantle is shallower than that of Jupiter 12

13. Jupiter: Magnetic Field Enormous – 30 million km across –if we could see it from Earth, it would appear 16x larger than the full moon in the sky Also very strong, but more variable in strength than Earth’s First detected by “synchrotron radiation” –radar signals emitted by charged particles trapped in magnetic field lines These particles also cascade into Jupiter’s atmosphere creating aurora, like on Earth 13

14. Saturn: Magnetic Field Weaker than Jupiter’s –probably because liquid metallic H region is smaller Aligned perfectly with rotation axis Contains fewer charged particles –no Io-like active moon to supply –icy ring material takes particles out of magnetic field lines => weaker aurora 14

15. 1610: Galileo looks at Saturn, notices it is not circular. Bulges on sides disappear in 1612, reappear in 1613 1655: With a better telescope, Huygens discovers ring, tilted by 27° Saturn’s Rings 15

16. Last crossing 1995-6 Next crossing 2008-9 Rings estimated to be only 30 meters thick! Saturn’s Rings are Thin 16

17. Huygens explains why the rings disappear. They are very thin, and when seen edge twice a saturn year, they vanish! 17

18. 1675 Cassini observes the “division” in the rings, separating the brighter “B” ring from the fainter outer “A” ring Cassini Division 18

19. Earth-based observations reveal three broad rings encircling Saturn 19

20. A more subtle division is found in the “A” ring Encke Division (1838) 20

21. 1857 Maxwell argues cannot be solid (centrifugal forces would tear it apart) 1895 Keeler measures Doppler velocities, each “ringlet” has different speed Rings consist of many “moonlets”, each orbiting the central planet. 80% reflectivity implies they are icy particles Probably from an icy moon pulled apart, only 100 million years ago. Rings are not solid! 21

22. The moon’s own gravity tends to hold it together. Tidal forces from planet tend to pull it apart The “Roche Limit” is the critical distance where the two balance Saturn’s moons are (mostly) outside of Roche Limit Saturn’s rings are (mostly) inside the Roche limit. Roche Limit (2.4 Saturn Radii) 22

23. From scattering of radio signals through the rings, estimate average particles are 10 cm in size Some are as small as 1 cm, some as big as 5 meters. In comparison the ring particles of the other planets are: –Jupiter’s are small dust particles smaller than 1 mm –Uranus particles are perhaps 1 meter in size –Neptune size unknown (similar to Uranus?) 1970 Voyager Probes 23

24. Cassini Saturn Orbit Insertion (SOI) June 30, 2004, 7:30 - 9:15 PDT 24

25. Spectra of Saturn’s main rings showing only H 2 O ice 25

26. Rings of Jupiter View of Jupiter from behind, looking toward the Sun 26

27. Jupiter’s rings 27 Jupiter has three very thin rings As with Neptune and Uranus, Jupiter’s rings are made of tiny black particles The material in Jupiter’s rings is probably coming from the small moons Metis, Adrastea, and others. Material is being blasted off those small moons by the impact of micrometeoroids attracted to Jupiter.

28. Saturn’s Rings: Natural Color 28

29. Gaps in Saturn’s Rings Gaps in the rings are caused by resonances with the satellites Example: Mimas causes the Cassini Division Mimas makes one revolution in 23 hours. A ring particle in The Cassini Division makes one revolution in 11 ½ hours, or two revolutions in one Mimas period. This is resonance. 29

30. What is “resonant motion”? When you push someone in a swing, each time they come back, you give a new push to keep them going. This is resonant motion. Each time a ring particle comes between Saturn and Mimas, it gets a pull from Mimas, causing its orbit to become eccentric. This increases the likelihood that it will collide with another particle and be destroyed. 30

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32. Encke Division Probably created not by resonance, but by the small moon “Pan” which shares the orbit. 32

33. F Ring from Cassini probe close approach, July 3, 2004 33

34. Saturn’s F-ring from Cassini 34

35. F Ring Shepherd Moons These two moons keep the narrow F ring in place. 35

36. Things to do Add more Pioneer and Voyager history (follow “the planets” video), along with Galileo and Cassini probe results. Should we separate Jupiter from Saturn?