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Saturn
 

Saturn

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lecture delivered in class on 16 Feb 2011

lecture delivered in class on 16 Feb 2011

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    Saturn Saturn Presentation Transcript

    • Saturn
    • Orbital and Physical Properties Mass: 5.7 × 10 26 kg (97 times Earth) Radius: 60,000 km (9.5 times Earth, .8 times Jupiter) Density: 700 kg/m 3 – less than water! Rotation: rapid and differential, enough to flatten Saturn considerably Rings: very prominent; wide but extremely thin
    • Saturn’s Atmosphere
      • Saturn’s atmosphere also shows zone and band structure, but coloration is much more subdued than Jupiter’s
      • Mostly molecular hydrogen, helium, methane, and ammonia; helium fraction is much less than on Jupiter
    • Saturn’s Atmosphere
      • Similar to Jupiter’s, except pressure is lower
      • Three cloud layers
      • Cloud layers are thicker than Jupiter’s; see only top layer
    • Saturn’s Cloud Structure
    • Saturn’s Atmosphere Wind patterns on Saturn are similar to those on Jupiter, with zonal flow :
    • Saturn’s Atmosphere Jupiter-style “ spots ” rare on Saturn; don’t form often and quickly dissipate if they do
    • A Storm on Saturn
    • Saturn, False Color
    • Saturn’s Interior and Magnetosphere Interior structure similar to Jupiter’s:
    • Saturn’s Interior and Magnetosphere
      • Like Jupiter, Saturn also radiates more energy than it gets from the Sun, but not because of cooling.
      • Helium and hydrogen are not well-mixed; helium tends to condense into droplets and then fall
      • Gravitational field compresses helium and heats it up
    • Saturn’s Interior and Magnetosphere Saturn also has a strong magnetic field , but only 5% as strong as Jupiter’s Creates aurorae :
    • Saturn’s Spectacular Ring System Saturn has an extraordinarily large and complex ring system , which was visible even to the first telescopes
    • Saturn’s Spectacular Ring System Ring features visible from Earth:
    • Saturn’s rings are not in order
    • Saturn's rings change their appearance to terrestrial observers as the tilted ring plane orbits the Sun.
    • Saturn’s Spectacular Ring System
      • Ring particles range in size from fractions of a millimeter to tens of meters
      • Composition : water ice – very similar to snowballs
      • Why rings?
      • Too close to planet for moon to form – tidal forces would tear it apart
    • Roche Limit
    • Saturn’s Spectacular Ring System Closest distance that moon could survive is called Roche limit ; ring systems are all inside this limit
    • Saturn’s Spectacular Ring System Voyager probes showed Saturn’s rings to be much more complex than originally thought Earth is shown on the same scale as the rings
    • Saturn’s Spectacular Ring System Voyager also found radial “ spokes ” that formed and then dissipated; this probably happens frequently
    • Saturn’s Spectacular Ring System Cassini division turns out not to be completely empty: It is caused by an orbital resonance with other ring particles and Saturn’s innermost moon
    • Saturn’s Spectacular Ring System Strangest ring is outermost, F ring: It appears to have braids and kinks .
    • Saturn’s Spectacular Ring System F ring’s oddities probably caused by two shepherd moons , one of which can be seen here:
    • Saturn’s Spectacular Ring System
      • Details of formation are unknown
      • Too active to have lasted since birth of solar system
      • Either must be continually replenished , or are the result of a catastrophic event
    • The Moons of Saturn Saturn’s many moons appear to be made of water ice Besides the small moons, Saturn has: Six medium-sized moons ( Mimas , Enceladus , Tethys , Dione , Rhea , and Iapetus ) One large moon ( Titan ) which is almost as large as Ganymede
    •  
    • The Moons of Saturn: Titan Titan has been known for many years to have an atmosphere thicker and denser than Earth’s; mostly nitrogen and argon Makes surface impossible to see; the picture at right was taken from only 4000 km away:
    • The Moons of Saturn: Titan Trace chemicals in Titan’s atmosphere make it chemically complex
    • The Moons of Saturn: Titan Due to difficulty of getting information, little is known about either the surface or the interior structure of Titan. This image, taken with an infrared telescope, shows some indication of surface features :
    • Cassini–Huygens Probe
    • On the surface of Titan
      • Huygens discovered a semi-liquid surface with rocks
      • Large bodies of liquid
    • Huygens to Titan
    • The Moons of Saturn: The Medium-Sized Moons
    • The Moons of Saturn: The Medium-Sized Moons
      • Mimas , Enceladus , Tethys , Dione , and Rhea all orbit between 3 and 9 planetary radii from Saturn, and all are tidally locked – this means they have “ leading ” and “ trailing ” surfaces.
      • Iapetus orbits 59 radii away, and is also tidally locked.
    • The Moons of Saturn: The Medium-Sized Moons Rhea , the largest, has a highly reflective, heavily cratered surface: Wispy features are on trailing side but not leading; origin not yet understood:
    • The Moons of Saturn: The Medium-Sized Moons Dione and Tethys are similar, having icy, heavily cratered surfaces:
    • The Moons of Saturn: The Medium-Sized Moons Mimas is the closest moon to Saturn, and has a crater covering one-third of its surface, the result of an impact that must have almost destroyed the moon: That’s no moon! Oh, no. It totally is a moon.
    • The Moons of Saturn: The Medium-Sized Moons Enceladus orbits close to Mimas, but is very shiny , indicating a surface covered with ice crystals:
    • The Moons of Saturn: The Medium-Sized Moons Iapetus is two-faced: its leading side is very dark (reflects 3% of incoming light), while its trailing side is bright (reflects 50% of incoming light). Cause is unknown.
    • Iapetus
    • Seeing Saturn
      • Galileo was the first to see Saturn’s rings.
      • He did not know what they were.
    • Seeing Saturn
      • 1655 - Christiaan Huygens first to propose that Saturn is surrounded by a solid ring
      • Huygens also discovered Titan
    • Seeing Saturn
      • Giovanni Domenico Cassini was the first to observe 4 of Saturn’s moons
        • Theorized (correctly) that Iapetus had a bright side and a dark side
      • Discovered the Cassini Division in the rings
    • Exploring Saturn
      • The Voyager missions flew by Saturn in 1980 and 1981
      • Cassini is currently in orbit around Saturn
      • The Huygens probe was parachuted onto the surface of Titan in 2005
    • The Other Side of Saturn
    • Summary
      • Saturn, like Jupiter, rotates differentially and is significantly flattened
      • Saturn’s weather patterns are in some ways similar to Jupiter’s, but there are far fewer storms
      • Saturn generates its own heat through the compression of “helium raindrops”
      • Saturn has a large magnetic field and extensive magnetosphere
    • Summary
      • Saturn’s most prominent feature is its rings, which are in its equatorial plane
      • The rings have considerable gross and fine structure, with segments and gaps; their particles are icy and grain- to boulder-sized
      • Interactions with medium and small moons determines the ring structure
      • The rings are entirely within the Roche limit, where larger bodies would be torn apart by tidal forces
    • Summary
      • Titan is the second-largest moon in the solar system
      • Titan has an extremely thick atmosphere, and little is known about its surface or interior
      • Medium-sized moons are rock and water ice; their terrains vary
      • These moons are tidally locked to Saturn