icy moons of jupiter, saturn, and beyond rosaly lopes, jpl · europa: interplay of surface colors...
TRANSCRIPT
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Icy Moons of Jupiter, Saturn, and
Beyond
Rosaly Lopes, JPL
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Galilean satellites: Io, Europa, Ganymede, and Callisto
Io: hot volcanoes, colorful surface, lots of sulfur, no impact
craters
Europa: icy crust, possible ocean underneath, few craters
Ganymede: largest of all, surface is bright (icy) and dark (rocky)
Callisto: many craters, impact basin 4,000 km diameter
(Valhalla)
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Europa: cracks on an icy crust
Young, thin, cracked and ruptured ice shell probably moving slowly over a liquid
ocean. Cracks and ridges (linear brown features) can be 1000s of km long.
Chaotic terrain (mottled brown) exists where surface was disrupted and ice
blocks moved.
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Internal structure of Europa
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Artist’s view of Europa’s interior: thin or thick crust (M. Carroll)
Chaos regions may have formed when liquid water melted its way
through a thin (< 6 km) ice shell or formed through the interaction
of rising ice diapirs with the relatively thick (15-30 km) ice shell
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Europa: interplay of surface colors and ice structures
Small region (Conamara Chaos, 70 km across) shows fine ice particles
(white/blue) from an impact cover some of the surface. Reddish-brown surface
has been altered by minerals carried by water vapor released when the crust
was broken.
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Europa: Chaos
regions may
have been
formed by the
movement of
trapped pools
of water in the
ice (Schmidt
et al., 2011)
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Ganymede in enhanced color
Bright, grooved terrain and dark, furrowed older terrain
Galileo instruments detected atmosphere and magnetic field
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Callisto: a cratered world
Small bright spots in global view are large craters in medium resolution view.
Local view shows smooth dark materials that cover much of the surface.
Close up views show evidence of erosion, probably due to sublimation of
volatiles from the surface ice.
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Saturn on July 2008
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A
B
C
C D F
Rings in detail never before seen
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Rings: small
particles (microns
to meters) form
clumps
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Rings in forward scattering
we are here
The E-ring is created by Enceladus
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Icy Moons
• The Saturn system has 62 confirmed satellites, most are
small and far away from the planet.
• Titan is by far the largest
• There are 8 major other satellites: Mimas, Enceladus,
Tethys, Dione, Rhea, Hyperion, Iapetus, and Phoebe
Rhea diameter 1528 km (955 mil)
Saturn’s second largest moon
Image from August 2007
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Last Rhea Flyby
9 March 2013
North polar regions
Graben
(extensional faulting)
indicates ice crust
pulled apart
Surface Temperature
-210 C (-281 F)
Density 0.93 g cm-3
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Michael Carroll’s Enceladus-Earth size comparison
Saturn’s Moon Enceladus: small, but active
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Cassini Enceladus fly-by:
July 2005
Showed south polar “tiger
stripes”
Flyby at 168 km (105 mi)
Enceladus diameter 504
km (315 mi)
Thermal data (CIRS)
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Avg Earth
87 mW/m2
Enceladus
South Polar Terrain
250 mW/m2
Tiger Stripes
13,000 mW/m2
Planetary Heat Flow
Yellowstone
2500 mW/m2
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Enceladus Jets and Plume
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UVIS detected 4 high density water vapor jets.
Jet sources < 300 x 300 m, water molecules, safe for Cassini close flybys of
plumes (August 2008 flyby c/a 50 km!)
UVIS stellar occultation (Zeta
Orionis), October 2007
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GEYSER COMPOSITION (Waite et al. 2006; Hansen et al., 2006)
H2O 91 ± 3 % wt.
CO2 3.2 ± 0.6 % wt.
N2 4 ± 1 % wt.*
CH4 1.6 ± 0.4 % wt.
CO < 0.9 % wt
NH3, HCN, C2H2, C3H8 < 0.5 % wt. (i.e., detected)
*Inferred from a combination of INMS and UVIS data
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• Gas: mostly water vapor, with other gaseous molecules mixed in (e.g. CO2, N2, CH4,
CO, C2H6, NH3)
• Many ice particles (particularly close to Enceladus) contain sodium, potassium, and
carbonates, which may indicate they originate in an ocean deep below the icy crust
• Plumes may be material escaping through surface cracks from an internal salty ocean
or lake
• Cosmic Dust Analyzer on Cassini showed sodium within ice grains in the E ring and
plumes, consistent with ocean hypothesis (Postberg et al. 2009)
• Ground based observations showed no sodium gas in vapor cloud (Schneider et al.,
2009) – not consistent with rapid boiling near surface
• Alternatively, ice along cracks may sublime or melt, followed by escape of water vapor
and icy particles
• Plumbing still now known: near surface reservoirs or is material boiling more slowly
over larger areas?
Enceladus Plumes
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A: Salty water boils explosiverly. Unlikely because sodium gas would have been detected
B: Slow evaporation. Unlikely as conduit would become clogged by sodium left behind
C: Salty particles stored near surface, incorporated in plume by gases. Hard to dislodge old ice
grains from walls.
D: liquid water stored near surface, salinity increases as water evaporates. Plausible.
E: liquid water salty, comes from ocean in contact with rocky core. Water evaporates slowly into a
pressurized chamber, from which water and ice particles (inc. sodium) escape along narrow
fissures. Plausible.
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Enceladus: summary
• NASA’s Cassini spacecraft has
observed plumes of material
escaping from Saturn’s small icy
moon, Enceladus
• The plume is mostly water vapor,
with tiny ice particles and other
gaseous molecules mixed in (e.g.
CO2, CH4, C2H6)
• The plume supplies ice particles to
one of Saturn’s rings
• Some ice particles contain salt,
which may indicate they originate in
an ocean deep below the icy crust
Image mosaic of Enceladus taken by Cassini,
showing individual plumes of gas and ice
escaping from the surface. The plumes
extend 100’s of km into space from the ~500
km diameter moon.
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Michael
Carroll’s
view of
plumes on
Enceladus
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Earth: Submarine volcanism
Most of the Earth’s
volcanoes are under
the ocean, such as in
the East Pacific Rise
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Iapetus: A
Strange Icy
World
If this “Belly Band” were on Earth
to scale it would be:
• 20 time higher than Mt. Everest
• 2.3 times longer than the Andes
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Iapetus' Albedo Contrast
ISS, 10 Sept. 2007
Darker areas are warm enough that ice sublimes and then is re-deposited
in the bright regions
Dark areas have different composition (more CO2)
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One Moon Coats its Neighbor in Dust
• The trailing face of Saturn’s moon
Iapetus is ~10 times brighter than its
leading face
• For 300 years, astronomers debated
whether the cause was internal (e.g.
eruption of dark material on one face)
or external (e.g. debris from a nearby
impact)
• The discovery of a giant ring around
Saturn and close-up Cassini images
confirm an external cause: dust
particles coat one side and drive ice to
the other by sublimation Saturn’s moon Iapetus has a dark leading side,
while its polar regions and trailing side are
bright. The dividing line follows a pattern like the
stitching on a baseball.
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• Impactors strike one of several distant
dark Saturn moons (such as Phoebe),
supplying a ring of dark particles that
orbit Saturn ‘backwards’, like Phoebe
• Sunlight pushes the ~10 micron
particles inward over thousands of
years
• Particles collide with Iapetus and
other inner moons, making their
leading face slightly darker
• The darkened ice absorbs more
sunlight, warms up, and sublimes,
recondensing as bright frost on the
trailing side and poles
A Ring Creates Iapetus contrast
Dust from backwards-orbiting (captured)
Phoebe coats the leading side of Iapetus
Sun-warmed dust causes sublimation,
driving ice to the poles and trailing side
Phoebe
Trailing
Leading
Dust Iapetus
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The Big Picture: the Phoebe ring
• Planetary moons can be “painted”
at a global level by external causes
such as dust and even charged
particles
• Dark dust and bright ice can
segregate on a moon’s surface, as
sun-warmed dust drives ice to
brighter, icier regions
• New telescopes and instruments
keep discovering new phenomena:
The “Phoebe ring” is the largest
and most distant from its parent
body
Artist’s conception of huge ring around Saturn,
discovered at IR wavelengths by the Spitzer Space
Telescope. The inset indicates scale by showing
an enlarged ground-based IR image of Saturn.
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Hyperion
26 Sept. 2005
514 km flyby
Dark Material in crater floors
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Image of the Year (2005): color view of
Dione from October 11, 2005, flyby
• TIME magazine’s 2005 best “Editor’s Choice Picture of the Year”
• MSNBC’s best “Space Photo of the Year”
• Aviation Week and Space Technology’s “Best of the Rest” contest
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Dione’s Bright “Wisps”
revealed to
be fractures
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Methone at 4500 km on May 20, 2012
Janus at 28,000 km on March 27, 2012
Saturn’s Bizarre Small Moons
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And further out…
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Neptune’s Triton: cryovolcanism
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Michael Carroll’s view of geysers on Triton
Pink nitrogen ice melts directly into gas leaving strange shapes
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Where next? New Horizons will
arrive at Pluto on 14 July 2015…
This is the most detailed view to date of the entire surface
of the dwarf planet Pluto, as constructed from multiple
NASA Hubble Space Telescope photographs taken from
2002 to 2003.
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