Transcript Jupiter and Saturn Power Point 2016

Jupiter and Saturn
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Jupiter
Crash course Jupiter
https://www.youtube.com/watch?v=
Xwn8fQSW7-8
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Orbital and Physical
Properties
This figure shows the solar system from a vantage point
that emphasizes the relationship of the jovian planets to
the rest of the system
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11.1 Orbital and Physical
Properties
Three views of Jupiter: From a small telescope on Earth;
from the Hubble Space Telescope; and from the Cassini
spacecraft
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Orbital and Physical
Properties
• Mass: 1.9 × 1027 kg (twice as much as all other
planets put together)
• Radius: 71,500 km (11.2 times Earth’s)
• Density: 1300 kg/m3—cannot be rocky or metallic
as inner planets are
• Rotation rate: Problematic, as Jupiter has no
solid surface; different parts of atmosphere rotate
at different rates
• From magnetic field, rotation period is 9 hr, 55
min
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The Atmosphere of Jupiter
Bands of clouds; Great Red Spot existed for 300 years
•Atmosphere has bright zones and dark belts
• Zones are cooler, and are higher than belts
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Wind speed with
respect to internal
rotation rate
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Composition of atmosphere:
mostly molecular hydrogen and
helium; small amounts of
methane, ammonia, and water
vapor
No solid surface
Lowest cloud layer cannot be
seen by optical telescopes
Measurements by Galileo probe
show high wind speeds even at
great depth—probably due to
heating from planet, not from
Sun
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Lightning-like flashes have
been seen; also shorterlived rotating storms
One example: Brown Oval,
really a large gap in clouds
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Recently, three white storms were observed to merge into a
single storm, which then turned red. This may provide some
clues to the dynamics behind Jupiter’s cloud movements.
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Internal Structure
Find that Jupiter radiates
more energy than it
receives from the Sun:
• Core is still cooling off
from heating during
gravitational compression
Main components are
hydrogen and helium, The
central portion is a rocky
core.
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Discovery 11-2: Almost a Star?
Jupiter is much too small to have become a star—needs
80 times more mass!
But its energy output was larger in the past; could have
been 100 times brighter than the Moon as seen from
Earth
Dwarf star in Jupiter’s place probably would have made
stable planetary orbits impossible
Jupiter played invaluable role in sweeping solar system
clear of debris before too much reached Earth—otherwise
life on Earth might not have been possible
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Jupiter’s Magnetosphere
Jupiter is surrounded by belts of charged particles
Magnetosphere is 30 million km across
Magnetosphere can extend beyond the orbit of Saturn
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The Moons of Jupiter
Jupiter with Io and Europa. Note the relative sizes!
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A bit about Jupiter’s moons
History of Jupiter moons
https://www.youtube.com/watch?v=N6W9RDK-jkk
Europa
http://www.space.com/27854-jupiter-moon-europaamazing-photo.html
Crash course Jupiter Moon
https://www.youtube.com/watch?v=HaFaf7vbgpE
Sound of Jupiter
https://www.youtube.com/watch?v=e3fqE01YYWs
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11.5 The Moons of Jupiter
63 moons have now been found orbiting Jupiter, but most
are very small
The four largest are the Galilean moons, so called because
they were first observed by Galileo:
• Io, Europa, Ganymede, Callisto (I Eat Green Carrots)
Galilean moons have similarities to terrestrial planets:
orbits have low eccentricity, largest is somewhat larger than
Mercury, and density decreases as distance from Jupiter
increases
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The Moons of Jupiter
Interiors of the Galilean moons
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Io is the densest of Jupiter’s moons, and the most
geologically active object in the solar system: Many active
volcanoes, some quite large Can change surface features
in a few weeks
• No craters; they fill in too fast—Io has the youngest
surface of any solar system object
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The Moons of Jupiter
Orange color is probably from sulfur compounds in
the ejecta
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IO’s Cause of volcanism:
Gravity!
Io is very close to
Jupiter and also
experiences
gravitational forces
from Europa.
The tidal forces are
huge and provide the
energy for the
volcanoes.
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Europa has no craters;
surface is water ice, possibly
with liquid water below
Tidal forces stress and crack
ice; water flows, keeping
surface relatively flat
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Ganymede is the largest
moon in the solar system—
larger than Pluto and
Mercury
History similar to Earth’s
Moon, but water ice instead
of lunar rock
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Callisto is similar to Ganymede; no evidence of plate
activity
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Jupiter’s Ring
Jupiter has been found to have a small, thin ring
Made of dark fragments of rock and dust possibly
chipped off the innermost moons by meteorites.
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Do the Jupiter moon activity in
the computer room
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Gas Giant tutorial
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Saturn
Crash course
https://www.youtube.co
m/watch?v=E8GNde5n
CSg
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Orbital and Physical
Properties
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
Rings: Very prominent;
wide but extremely thin
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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
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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
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Saturn’s Atmosphere
Wind patterns on Saturn
are similar to those on
Jupiter, with zonal flow
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Jupiter-style “spots” rare on Saturn; don’t form often and
quickly dissipate if they do
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Saturn’s Interior and Magnetosphere
Interior structure similar to
Jupiter’s
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 and heat up
due to gravity.
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Saturn also has a
strong magnetic
field, but only 5% as
strong as Jupiter’s
Creates aurorae at
poles during solar
storm
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Saturn’s Spectacular Ring System
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
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http://www.discovery.com/tvshows/other-shows/videos/howthe-universe-works-saturns-rings/
Closest distance that moon could survive is called
Roche limit; ring systems are all inside this limit
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The Moons of Saturn
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) and One large
moon (Titan), almost as large as Jupiter’s Ganymede
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Moons in the news
https://www.youtube.com/watch?v=U8WM
O6lHM1Q
http://www.space.com/28265-saturn-moontitan-landing-anniversary.html
https://www.youtube.com/watch?v=nqsP5xI
uS1I
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Titan is the second-largest
moon in the solar system
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
Trace chemicals in Titan’s
atmosphere make it
chemically complex
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Titan
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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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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•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
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The Rings of Saturn
Do the Scale model activity following the Advanced
Procedure
And make sure to do the going further activity in the
computer room.
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