Escaping ions over polar cap. Inner magnetosphere, Bow shock/Foreshock, and Ancient magnetosphere.
Chapter 12 Saturn. 12.1 Orbital and Physical Properties 12.2 Saturn’s Atmosphere 12.3 Saturn’s...
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Transcript of Chapter 12 Saturn. 12.1 Orbital and Physical Properties 12.2 Saturn’s Atmosphere 12.3 Saturn’s...
![Page 1: Chapter 12 Saturn. 12.1 Orbital and Physical Properties 12.2 Saturn’s Atmosphere 12.3 Saturn’s Interior and Magnetosphere 12.4 Saturn’s Spectacular Ring.](https://reader036.fdocuments.in/reader036/viewer/2022081506/56649c865503460f9493d3c9/html5/thumbnails/1.jpg)
Chapter 12Saturn
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12.1 Orbital and Physical Properties
12.2 Saturn’s Atmosphere
12.3 Saturn’s Interior and Magnetosphere
12.4 Saturn’s Spectacular Ring System
12.5 The Moons of Saturn
Dancing Among Saturn’s Moons
Units of Chapter 12
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Mass: 5.7 × 1026 kg
Radius: 60,000 km
Density: 700 kg/m3—less than water!
Rotation: Rapid and differential, enough to flatten Saturn considerably (oblate)
Rings: Very prominent; wide but extremely thin
12.1 Orbital and Physical Properties
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12.1 Orbital and Physical Properties
View of rings from Earth changes as Saturn orbits the Sun
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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
12.2 Saturn’s Atmosphere
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12.2 Saturn’s Atmosphere
This true-color image shows the delicate coloration of the cloud patterns on Saturn
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Similar to Jupiter’s, except pressure is lower
•calmerFewer storms
Three cloud layers
Cloud layers are thicker than Jupiter’s; see only top layer
12.2 Saturn’s Atmosphere
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12.2 Saturn’s Atmosphere
Structure in Saturn’s clouds can be seen more clearly in this false-color image
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Wind patterns on Saturn are similar to those on Jupiter, with zonal flow
•Note the speed
•3x faster! Than Jupiter
12.2 Saturn’s Atmosphere
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Jupiter-style “spots” rare on Saturn; don’t form often and quickly dissipate if they do
12.2 Saturn’s Atmosphere
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12.2 Saturn’s AtmosphereThis “dragon storm” was first spotted in 2004; it is believed to be a long-lived phenomenon but is usually hidden under the clouds
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12.2 Saturn’s Atmosphere
As expected for a planet with an atmosphere, there is a vortex at Saturn’s south pole.
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Interior structure similar to Jupiter’s
12.3 Saturn’s Interior and Magnetosphere
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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
12.3 Saturn’s Interior and Magnetosphere
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Saturn also has a strong magnetic field, but only 5% as strong as Jupiter’s•Magnetic Field Strength
•1000 x earths’
•Surface of Atmosphere (10 Earth Radii)
= Earth Surface
Creates aurorae:
12.3 Saturn’s Interior and Magnetosphere
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Saturn has an extraordinarily large and complex ring system, which was visible even to the first telescopes
12.4 Saturn’s Spectacular Ring System
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Overview of the ring system:
12.4 Saturn’s Spectacular Ring System
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Ring particles range in size from fractions of a millimeter to tens of meters
Composition: Water ice—similar to snowballs
Why rings?
• Too close to planet for moon to form—tidal forces would tear it apart
12.4 Saturn’s Spectacular Ring System
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Closest distance that moon could survive is called Roche limit; ring systems are all inside this limit
12.4 Saturn’s Spectacular Ring System
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Roche Limit
• The external tidal forces on an object become greater than the internal forces that hold it together.
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Voyager probes showed Saturn’s rings to be much more complex than originally thought
(Earth is shown on the same scale as the rings)
Cassini Division has several ringlets
12.4 Saturn’s Spectacular Ring System
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12.4 Saturn’s Spectacular Ring System
This backlit view shows the fainter F, G, and E rings
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Voyager also found radial “spikes” that formed and then dissipated; this probably happens frequently
12.4 Saturn’s Spectacular Ring System
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• Other edges and divisions in rings
are also the result of resonance
• “Shepherd” moon defines outer
edge of A ring through gravitational
interactions
•Confine a narrow ring
12.4 Saturn’s Spectacular Ring System
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Strangest ring is outermost, F ring; it appears to have braids and kinks
12.4 Saturn’s Spectacular Ring System
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F ring’s oddities probably caused by two shepherd moons, one of which can be seen here:
12.4 Saturn’s Spectacular Ring System
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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
12.4 Saturn’s Spectacular Ring System
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Saturn’s many moons appear to be made of water ice
In addition to 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
12.5 The Moons of Saturn
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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 upper picture at right was taken from only 4000 km away
12.5 The Moons of Saturn
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Trace chemicals in Titan’s atmosphere make it chemically complex
12.5 The Moons of Saturn
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12.5 The Moons of Saturn
Some surface features on Titan are visible in this Cassini infrared image:
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12.5 The Moons of Saturn
The Huygens spacecraft has landed on Titan and is returning images directly from the surface
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12.5 The Moons of Saturn
Based on measurements made by Cassini and Huygens, this is the current best guess as to what the interior of Titan looks like:
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Discovery 12-1: Dancing Among Saturn’s Moons
The Cassini spacecraft uses multiple “gravitational slingshots” to make multiple close passes around Saturn’s moons. Precise orbits are decided on the fly.
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12.5 The Moons of Saturn
This image shows Saturn’s mid-sized moons
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• 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
12.5 The Moons of Saturn
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12.5 The Moons of Saturn
Global maps of Rhea and Dione, from Cassini:
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Masses of small moons not well known
Two of them share a single orbit:
12.5 The Moons of Saturn
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Two more moons are at the Lagrangian points of Tethys
12.5 The Moons of Saturn
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Hyperion, orbiting between Titan and Iapetus, is so affected by their gravitational fields that its orbital speed and the orientation of its axis are constantly changing in a never-repeating pattern.
This tumbling is an example of chaotic motion!
12.5 The Moons of Saturn
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• 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 of Chapter 12
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• 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 determine the ring structure
• The rings are entirely within the Roche limit, where larger bodies would be torn apart by tidal forces
Summary of Chapter 12 (cont.)
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• 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
• Several of the small moons share orbits, either with each other or with larger moons
Summary of Chapter 12 (cont.)