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  • 1. 4.5JOVIAN PLANETS
  • 2. The OUTER PLANETS
    All larger than Terrestrial Planets with thick atmospheres and very inhospitable.
    No solid surfaces
    Mostly Hydrogen and Helium
    Strong atmospheric circulation (winds/storms)
    Ring systems
    Multiple moons (Regular vs. Irregular satellites)
  • 3.
  • 4. jupiter
    Largest and most massive planet of the solar system.
    Contains almost ¾ of all planetary matter within the solar system.
    Mostly liquid Hydrogen.
    Most striking features visible from Earth  Multi-colored cloud belts; Great Red Spot
  • 5. jupiter
    Explored in detail by several space probes:
    Pioneer 10
    Pioneer 11
    Voyager 1
    Voyager 2
    Cassini
    Galileo
  • 6. VOYAGER 1
    Video data from approach to Jupiter in 1979
  • 7. Mass of jupiter
    Can be inferred from the radius and orbital period of Io, the innermost of the 4 Galilean moons.
    Using NVK3L  MJupiter = 318 MEarth
  • 8. Chemical compositionjupiter vs. saturn
  • 9. Jupiter’s interior
    Average density ~ 1.34 g/cm3
    Therefore, cannot be made of mostly rock like Earth-like planets.
    Rock has a density of 2.5  4 g/cm3.
  • 10. Jupiter’s rotation
    Most rapidly rotating planet in the solar system.
    Rotation ~ 9.92 h
    Revolution ~ 11.87 y
    Appears slightly flattened and is 6% larger in diameter through equator than through its poles; referred to as oblateness.
  • 11. Jupiter’s magnetic field
    Discovered through observations of decimeter (radio) observations.
    Created by the liquid metallic Hydrogen interior.
    Good electrical conductor.
    Believed to be 10 times stronger than Earth’s.
    Very intense radiation belts.
    Extremely high-energy particles can be trapped  radiation doses corresponding to 100 times lethal doses for humans!
  • 12. JUPIter’s magnetic field
    Just like on Earth, Jupiter’s magnetosphere produces aurora concentrated in the rings around the magnetic poles.
    1000 times more powerful than the aurora on Earth.
  • 13. Jupiter’s atmosphere
    Liquid Hydrogen ocean has no surface.
    Pressure and temperature higher than the critical point for Hydrogen, meaning there is no difference between gaseous and liquid Hydrogen.
    Very thin atmosphere above cloud layers.
    Cold outer layers; interior layers warm but pressure is immense.
    Transition to liquid Hydrogen zone ~ 1000 km below clouds.
  • 14. Jupiter’s atmosphere
  • 15. Jupiter’s cloud belts
    • On Jupiter, the poles and equator have about the same temperature; no wave-shaped winds but rather bands called belts and zones.
    On Earth, the temperature difference b/w poles and equator drives a wave-shaped wind organizing high and low pressure areas.
  • 16. Jupiter’s cloud belts
    DARK BELTS
    Lower Altitude
    Warmer Temperatures
    LIGHT ZONES
    Higher Altitude
    Cooler Temperatures
  • 17. The Great red spot
    Several bright and dark spots mixed in with cloud structure.
    Cyclones/Anticyclones
    Largest and most prominent: Great Red Spot.
    Visible for over 300 years.
    Formed by rising gas carrying heat from below the clouds, creating a vast, rotating storm.
    • For the first time, very recently, a new similar red storm system has been observed, Red Jr.
  • Jupiter’s rings
    Discovered in 1979 by Voyager 1.
    Dark and reddish in color; rocky rather than icy (mostly microscopic particles).
    Orbit inside the Roche Limit, the distance from a planet within which a moon cannot hold itself together by its own gravity.
    International Space Station can orbit inside Earth’s Roche Limit; held together by bolts and welds.
    Can’t be old  pressure of sunlight and Jupiter’s extensive magnetic field cause ring particles to spiral into cloud layers of Jupiter.
    Frequently replenished.
    Fainter rings known as gossamer rings, extend twice as far from Jupiter than the main ring.
  • 18.
  • 19. History of jupiter
    JUPITER
    “King of Gods”
    Formed from cold gas in the solar nebula, where ice particles could condense.
    Rapid growth.
    In the interior, Hydrogen becomes metallic due to pressure (good electrical conductor).
    Rapid rotation  strong magnetic field.
    Heavy materials sink to center.
    Dust from meteorite impacts onto inner moons trapped to form rings.
  • 20. Jupiter’s family of moons
    Has 63 known moons; new ones still being discovered.
    4 largest moons discovered by Galileo (Galilean Moons):
    IO
    EUROPA
    GANYMEDE
    CALLISTO
  • 21. Io: roaring volcanoes
    Innermost and most active of all Galilean moons.
    No impact craters visible.
    Hundreds of active volcanoes.
    Activity powered by tidal interactions with Jupiter.
    Average density ~ 3.55 g/cm3
    Mostly rock.
  • 22. Europa: hidden ocean
    Almost completely free of impact craters.
    Active surface erases craters almost as fast as they form.
    • Bright face tells you surface is young.
    • 23. Albedo of 0.69, meaning it reflects 69% of the light hitting its surface.
  • Surface of europa
    Long cracks in the icy crust and sections moving apart as if they were icebergs floating on water provide further evidence for tectonic activity.
  • 24. Interior of europa
    Too small to retain internal heat.
    Heating comes from tidal interactions with Jupiter.
    Core not molten No magnetic field.
    Europa has a liquid water ocean ~ 15 km below the icy surface.
  • 25. Ganymede: a hidden past
    Largest moon in the solar system; larger than Mercury itself.
    Average density ~ 1.9 g/cm3.
    Underwent differentiation.
    Rocky core, ice-rich mantle, crust of ice 500 km thick.
    • Bright, parallel grooves across the surface indicate an active past.
    • 26. Surface once flooded.
    • 27. Experiences 2 unusual processes due to its size and closeness to Jupiter:
    • 28. Tidal Heating
    • 29. Inward Focusing of Meteorites
  • Callisto: the ancient face
    Average density ~ 1.8 g/cm3
    Mixture of ice and rocks.
    Old, dark surface heavily cratered.
    Measurements show it never fully differentiated to form a dense core and lower-density mantle.
    Interaction with Jupiter’s magnetic field suggests is has a layer of liquid water.
    Heat from interior through slow radioactive decay.
    • Impact scar shown above is one of the largest in the solar system (4000 km ~ 2500 mi).
  • the galilean moons
    Minor moons are believed to be captured asteroids.
    Galilean moons probably formed with Jupiter.
    Formed from a disk of material surrounding Jupiter (mini “solar nebula”).
    Earliest moons may have spiraled into Jupiter.
    Galilean moons are probably a 2nd generation of moons for Jupiter.
  • 30. Saturn
    Average density ~ 0.69 g/cm3
    Less dense than water (1.0 g/cm3)  Would float on water!
    Rotation ~10.66 h
    Revolution ~ 29.46 y
  • 31. Saturn’s atmosphere
    Hydrogen and Helium rich with heavy element core.
    Displays belt-zone circulation, similar patterns to Jupiter (not as distinct).
    Actually exhibits faster wind speeds, but fewer wind zones.
    • Much colder atmosphere than Jupiter’s (twice as far from the Sun, receives only ¼ as much solar energy per square meter).
  • Saturn’s rings
    An astronomer once said:
    “ The rings are made of beautiful physics.”
    In 1609, Galileo became the first to see the rings, but didn’t recognize them as individual rings.
    Drew Saturn as a central body with two smaller bodies surrounding it.
  • 32. Saturn’s rings
    Consists of 3 main segments: A, B, and C
    Separated by empty regions called divisions (Cassini  A /B; Encke  A)
    Rings replenished by passing comets and meteoroids.
    Just as with Jupiter, Saturn’s rings lie inside Roche Limit.
    Some smaller moons, known as shepherd moons, orbit close to the rings and keep the ring material confined.
  • 33. Saturn’s rings
    Made of billions of ice particles (microscopic specks  chunks larger than a house).
    Voyager 1
    Voyager 2
    Cassini
    Rings could not have formed when Saturn formed  once hot and ring material would have vaporized.
  • 34. Saturn’s moon - titan
    2nd largest moon in the solar system.
    Rocky core; abundant ice.
    Only natural satellite with an atmosphere; thick  hides the surface.
  • 35. Saturn’s moon - titan
    Explored extensively by Cassini spacecraft, which released the Huygens probe.
    Landed on surface of Titan in 2005 and radioed back images.
    Few craters  suggests geologic activity?
    Most of its atmosphere is Nitrogen; smaller amounts of methane.
    Sunlight converts methane (CH4) into the gas ethane (C2H6) plus a collection of other organic molecules.
    Produces smog-like haze  settles into goo.
    Methane/ethane rain?
  • 36.
  • 37. Saturn’s smaller moons
  • 38. History of saturn
    SATURN
    “God of Harvest”
    Most of Saturn’s story parallels Jupiter’s.
    Smaller with less liquid metallic Hydrogen, thus producing a weaker magnetic field.
    Rings are not primordial, meaning the material in them now has not been in its current form since the formation of the planet.
    Permanent or temporary?
  • 39. uranus
    Chance discovery made by William Herschel in 1781 while scanning the sky for nearby objects with measurable parallax.
    Until that time, astronomers only knew of five planets aside from Earth.
    “Luck is what happens to the people who work hard.”
  • 40. Motion of uranus
    Just over 19 AU’s from the Sun.
    Rotation ~ 17.23 h
    Revolution ~ 84.0 y
    Rotation axis inclined 97.9° from the perpendicular to its orbit (tilted on its side  retrograde rotation).
    Impact during planetary development?
    Extreme seasons.
    Rotation between eternal sunlight and extreme darkness for many years.
    First good photographs taken in 1986 as Voyager 2 flew past.
    97.9o
    19.18 AU
  • 41. Atmosphere of uranus
    Like Jupiter and Saturn, no surface exists on Uranus.
    Mostly Hydrogen, with 15% Helium, and about 2% methane, ammonia, and water vapor.
    Gradual transition from gas (molecular) state to fluid-like interior.
    • Blue-green color comes from methane  good absorber of longer wavelength photons.
    • 42. Cloud structures visible after computerenhancements form optical images.
  • Atmosphere of uranus
    Only 1 layer of methane clouds, as opposed to 3 cloud layers on Jupiter and Saturn.
    Difficult to see because of thick atmosphere.
    Also shows belt-zone structure.
    Result of planet’s rotation rather than sunlight incidence angle.
  • 43. Atmosphere of uranus
    Keck Telescope in Mauna Kea (Hawaii) show clear variability of the cloud structures.
    Possibly due to extreme seasonal changes
  • 44. Interior of uranus
    Average density ~ 1.29 g/cm3
    Larger portion of rock and ice than Jupiter and Saturn, thus higher density.
  • 45. Uranus’ magnetic field
    Lower mass than Jupiter; internal pressure not high enough to create liquid metallic Hydrogen.
    No magnetic field was expected.
    Voyager 2 detected slight magnetic field (75% of Earth’s).
    Theorists say it is generated by a dynamo effect not from the interior like on Earth and other planets, but from surface layers of liquid water with dissolved ammonia and methane (convection currents)  good conductor of electricity, rotation coupled together = magnetic field.
  • 46. Uranus’ magnetic field
    Rapid rotation and large inclination deform the magnetosphere into a corkscrew shape.
    Aurora and radiation belts detected.
  • 47. Rings of uranus
    Similar to Jupiter’s rather than Saturn’s.
    Dark/faint, not easily visible, and contained by shepherd satellites.
    Like all Jovian rings, they cannot survive for long periods; need to be replenished with material from impacts on moons.
  • 48. Rings of uranus
  • 49. Moons of uranus
    5 largest moons visible from Earth.
    Tidally locked to Uranus.
    10 more discovered by Voyager 2.
    Dark surfaces; probably ice darkened by dust from meteorite impacts.
    Large rocky cores surrounded by icy mantles.
    Titania
    Largest moon of Uranus
  • 50. Moons of uranus
    Miranda is the innermost and most unique of the moons of Uranus.
    • Originally believed to be broken apart and accreted back together.
    • 51. Consists of ovoids, or oval-grooved patterns most likely associated with convection currents in the mantle, not with impacts.
    • 52. Old surface features suggest Miranda is no longer active.
  • HISTORY OF URANUS
    URANUS
    “God of the Sky”
    Difficult to study and observe.
    Far away/peculiar in many ways.
    Computer models suggest it probably formed closer to the Sun, along with Neptune, in the field of Jupiter and Saturn.
    Gravitational interactions may have eventually moved them outward to their present locations.
    Interesting hypotheses exist.
  • 53. neptune
    Discovered in 1846 at a position predicted from gravitational disturbances on Uranus’ orbit.
    J.C. Adams
    U.J. Leverrier
    Blue-green color exists from methane gas being present; similar to Uranus.
    30.1 AU’s from the Sun.
    Approximately 4 times the Earth’s diameter.
    Rotation ~ 16.05 h
    Revolution ~ 164.8 y
  • 54. Neptune’s atmosphere
    Belt-zone structured clouds with high speed winds; similar to other Jovians.
    Great Dark Spotsimilar cyclonic disturbance to Jupiter’s Great Red Spot.
    White cloud features on the planet are methane-ice crystals.
  • 55. Neptune’s rings
    Voyager 2 revealed rings of Neptune, as expected.
    Can’t be primordial they couldn’t have lasted in their present form since the formation of Neptune.
  • 56. Moons of neptune
    2 largest moons of Neptune visible from Earth-based telescopes; Tritonand Nereid.
    6 more discovered by Voyager 2.
    The orbit of Nereid is highly eccentric compared to the orbit of Triton.
  • 57. triton
    Only satellite in the solar system to orbit clockwise (retrograde - backwards).
    Low surface temperature ~ 35 K
    Surface composed of ices: Nitrogen, Methane, Carbon Monoxide, Carbon Dioxide.
    The cycle of Nitrogen on Triton resembles in some ways the cycle of Carbon Dioxide on Mars.
  • 58. HISTORY OF NEPTUNE
    NEPTUNE
    “God of the Sea”
    Like Uranus, Neptune’s hazy atmosphere with changing cloud patterns, hides a mantle of partially frozen ices  astronomers predict dynamo effect generating a magnetic field.
    Satellite system suggests a peculiar history:
    Triton  retrograde rotation
    Nereid  long-period; highly elliptical orbit.
  • 59. pluto
    PLUTO
    “God of the Underworld”
    Discovery  Clyde Thombaugh; 1930.
    Sensed something was wrong from the first moment he saw it.
    2.5 magnitudes too faint.
    Not the 7-Earth mass planet as predicted.
    Difficult to observe from Earth.
    Average density ~ 2.0 g/cm3
    65% the diameter of Earth’s moon.
    Most planetary orbits are nearly circular; Pluto’s is highly eccentric.
    1979– 1999  Pluto was actually close to the Sun than Neptune was.
    Never collide because Pluto’s orbit is inclined 17; don’t come close.
  • 60. Surface of pluto
    Little surface detail is shown, even from the Hubble Space Telescope.
    If all goes well, the New Horizons probe, due to arrive in 2015, will send the first close-up images of Pluto and its moons.
    Cold enough to freeze most compounds you think of as gases.
    Maximum daytime temperature ~ 55K (-360 F); enough to vaporize some of the Nitrogen and Carbon Monoxide and some Methane to form a thin atmosphere around Pluto.
    Atmosphere first detected in 1988.
  • 61. Pluto’s moons
    Largest moon, Charon, was discovered in 1978.
    Half the diameter of Pluto.
    Believed to contain 35% ice and 65% rock material.
    Two smaller moons, Nix and Hydra, were found in 2005 and confirmed in 2006 by the Hubble Space Telescope.
  • 62. Origin of pluto
    Believed to have a very different history than its neighboring four Jovian planets.
    Pluto and its moons are now considered members of the Kuiper Belt, icy objects beyond Neptune’s orbit (similar to Asteroid Belt between Mars and Jupiter only much larger).
    • Because of its different origin from the planets, Pluto is now classified as a dwarf planet.
  • Objects Beyond Neptune
    In recent years, astronomers have discovered hundreds of objects beyond Neptune’s orbit and have termed them Trans-Neptunian Objects (TNO’s).
    Most are just small chunks of ice.
    TNO’s exist in a region known as the Kuiper Belt.
  • 63. Family of Dwarf planets
    In order to be considered a dwarf planet, the object must meet the following criteria:
    Orbits the Sun
    Is round because of its own gravity (mass-related)
    Has not cleared the region around its orbit
    Is not a satellite of another planet
    CERES
    The largest asteroid
    Member of the Asteroid Belt
    900 km diameter
    ERIS
    The “10th” planet
    4% larger than Pluto
    27% more massive than Pluto
    70% further away from the Sun than Pluto