Ice on Mars:

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Ice on Mars Using Spacecraft Data to Understand
the Amazonian
Jay Dickson Brown University
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Mars Geologic History
Three epochs, defined and characterized by -
Impact crater flux - Fluvial modification
Defined using Viking and Mariner data. Could be
redefined by mineral types (Bibring et al., 2006).
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Mars Geologic History
Three epochs, defined and characterized by -
Impact crater flux - Fluvial modification
Defined using Viking and Mariner data. Could be
redefined by mineral types (Bibring et al., 2006).
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Mars Geologic History
Three epochs, defined and characterized by -
Impact crater flux - Fluvial modification
Defined using Viking and Mariner data. Could be
redefined by mineral types (Bibring et al., 2006).
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Noachian
Heavy impact cratering rate. Formation of
Hellas, Utopia, other major impact basins.
Channels thousands of kilometers long, standing
bodies of water in giant lakes.
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Noachian
Heavy impact cratering rate. Formation of
Hellas, Utopia, other major impact basins.
Channels thousands of kilometers long, standing
bodies of water in giant lakes.
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Noachian
Heavy impact cratering rate. Formation of
Hellas, Utopia, other major impact basins.
Channels thousands of kilometers long, standing
bodies of water in giant lakes.
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Noachian/Hesperian Boundary
Chains of crater lakes for thousands of
kilometers.
(Fassett and Head, 2008)
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Noachian/Hesperian Boundary
Chains of crater lakes for thousands of
kilometers.
(Fassett and Head, 2008)
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Noachian/Hesperian Boundary
Noachian/Hesperian Lakes (N 208) (Fassett and
Head, 2008)
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Hesperian
Decrease in cratering rate. Extensive
volcanic resurfacing. Formation of major
outflow channels.
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Hesperian
Decrease in cratering rate. Extensive
volcanic resurfacing. Formation of major
outflow channels.
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Hesperian
Decrease in cratering rate. Extensive
volcanic resurfacing. Formation of major
outflow channels.
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Amazonian - The Viking View (1970s)
Low impact cratering rate. Eolian dominated
erosion. Thin CO2 atmosphere. Water unstable
at the surface except as ice at the poles.
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Amazonian - The Viking View (1970s)
Low impact cratering rate. Eolian dominated
erosion. Thin CO2 atmosphere. Water unstable
at the surface except as ice at the poles.
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Amazonian - The Viking View (1970s)
Low impact cratering rate. Eolian dominated
erosion. Thin CO2 atmosphere. Water unstable
at the surface except as ice at the poles.
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Amazonian - The Viking View (1970s)
Low impact cratering rate. Eolian dominated
erosion. Thin CO2 atmosphere. Water unstable
at the surface except as ice at the poles.
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Amazonian - The Viking View (1970s)
Low impact cratering rate. Eolian dominated
erosion. Thin CO2 atmosphere. Water unstable
at the surface except as ice at the poles.
Has higher resolution data confirmed that the
Amazonian has been dry and cold (and BORING)?
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Amazonian - The MGS View (2000)
Not so fast!
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Amazonian - The MGS View (2000)
Gullies provide evidence for recent flow of
water.
(Malin and Edgett, 2000)
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Amazonian - The MGS View (2000)
The Amazonian may have been dry for the most
part, but water has flowed on the surface in the
last 10 million years in very local areas -
Poleward of 30 latitude. - Mostly on
pole-facing slopes. - Only on steep slopes (gt
26). - Only up to a certain altitude.
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Amazonian - The MGS View (2000)
The Amazonian may have been dry for the most
part, but water has flowed on the surface in the
last 10 million years in very local areas -
Poleward of 30 latitude. - Mostly on
pole-facing slopes. - Only on steep slopes (gt
26). - Only up to a certain altitude. So if
gullies formed in the last 10 million years, what
happened before that?
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Amazonian - ICE!
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Amazonian - More Ice!
(Head et al., 2005)
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Amazonian Ice - Where?
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Amazonian Ice - Where?
First proposed by Lucchitta, 1981
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Amazonian Ice - Mars Odyssey
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Amazonian Ice - Mars Odyssey
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Amazonian Ice - Mars Phoenix
Phoenix was built to sample the upper meter of
soil where we have detected massive amounts of
hydrogen.
(Mellon et al., 2004)
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Amazonian Ice - Mars Odyssey
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MRO HiRISE imaging Mars Phoenix during descent
through the Martian atmosphere.
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MRO HiRISE imaging Mars Phoenix during descent
through the Martian atmosphere.
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Could it be salts or other minerals?
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Nope.
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- Phoenix has proven that poleward of 60, Mars
contains massive amounts of ice in the very
near-surface, today.
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Amazonian Ice - Topography
Blue 0.6 km baseline Green 2.4 km baseline Red
9.2 km baseline
Softening of slopes at high-latitudes.
Mars Global Roughness - Kreslavsky and Head, 2000
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Amazonian Ice - Latitude-Dependant Features
Dissected Terrain - Mustard et al., 2001
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Amazonian Ice - Latitude-Dependant Features
Viscous Flow Features - Milliken et al., 2003
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Amazonian Ice - More Glaciation
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Amazonian Ice - More Glaciation
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Amazonian Ice - More Glaciation!
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Amazonian Ice
Lobate Debris Aprons
Lineated Valley Fill
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Amazonian Ice
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Amazonian Ice
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Amazonian Ice
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Amazonian Ice - Phantom Lobate Debris Aprons!
(Hauber et al., 2008)
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Amazonian Ice - Phantom Lobate Debris Aprons!
(Hauber et al., 2008)
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Amazonian Ice
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Amazonian Ice
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
Ice must have filled the valley to such an
extent that the neighboring canyon would be a
local low.
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Amazonian Ice - Coloe Fossae
920m of ice would be necessary to fill the
valley and induce flow into the adjacent
canyon. The ice then sublimates into the
atmosphere.
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
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Amazonian Ice - Coloe Fossae
A series of parallel, low-albedo lineations
observed on the valley wall. Similar to glacial
valleys on earth (trimlines or marginal
moraines). Suggestive of episodic glacial
activity. Need higher resolution imagery!
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Amazonian Ice - Coloe Fossae
A series of parallel, low-albedo lineations
observed on the valley wall. Similar to glacial
valleys on earth (trimlines or marginal
moraines). Suggestive of episodic glacial
activity. Need higher resolution imagery!
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Amazonian Ice - Coloe Fossae
A series of parallel, low-albedo lineations
observed on the valley wall. Similar to glacial
valleys on earth (trimlines or marginal
moraines). Suggestive of episodic glacial
activity. Need higher resolution imagery!
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Amazonian Ice - Coloe Fossae
A series of parallel, low-albedo lineations
observed on the valley wall. Similar to glacial
valleys on earth (trimlines or marginal
moraines). Suggestive of episodic glacial
activity. Need higher resolution imagery!
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Amazonian Ice - Coloe Fossae
A series of parallel, low-albedo lineations
observed on the valley wall. Similar to glacial
valleys on earth (trimlines or marginal
moraines). Suggestive of episodic glacial
activity. Target HiRISE!
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Amazonian Ice - Coloe Fossae
Use geologic relationships to tell a story
about a landscape. This region recently had
kilometer-scale glaciation on its surface. This
period stopped, and was followed by smaller,
episodic glaciation.
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Amazonian Ice - Coloe Fossae
Use geologic relationships to tell a story
about a landscape. This region recently had
kilometer-scale glaciation on its surface. This
period stopped, and was followed by smaller,
episodic glaciation.
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Amazonian Ice - Coloe Fossae
Use geologic relationships to tell a story
about a landscape. This region recently had
kilometer-scale glaciation on its surface. This
period stopped, and was followed by smaller,
episodic glaciation.
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Amazonian Ice - Phlegra Montes
Different terrain on the other side of the
planet. Small crater to the west of Phlegra
Montes. Extensive glacial deposits. Filling
the larger crater and flowing to the north.
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Amazonian Ice - Phlegra Montes
Different terrain on the other side of the
planet. Small crater to the west of Phlegra
Montes. Extensive glacial deposits. Filling
the larger crater and flowing to the north.
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Amazonian Ice - Phlegra Montes
Different terrain on the other side of the
planet. Small crater to the west of Phlegra
Montes. Extensive glacial deposits. Filling
the larger crater and flowing to the north.
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Amazonian Ice - Phlegra Montes
Different terrain on the other side of the
planet. Small crater to the west of Phlegra
Montes. Extensive glacial deposits. Filling
the larger crater and flowing to the north.
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Amazonian Ice - Phlegra Montes
Different terrain on the other side of the
planet. Small crater to the west of Phlegra
Montes. Extensive glacial deposits. Filling
the larger crater and flowing to the north.
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Amazonian Ice - Phlegra Montes
Different terrain on the other side of the
planet. Small crater to the west of Phlegra
Montes. Extensive glacial deposits. Filling
the larger crater and flowing to the north.
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Amazonian Ice - It was in the mid-latitudes
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Amazonian Ice - It was at the equator
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Amazonian Ice - Its currently at high latitudes
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Amazonian Ice - Where did it come from??
Today (obliquity 25) Mars is warm at the
equator, cold at the poles. Ice is stable at
the poles.
Recent Past (obliquity 45) Mars is warm at
high-latitudes, colder at equator. Ice can
accumulate at lower latitudes!
Laskar, 2004
Mars_at_ obliquity45
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Amazonian Ice - Where did it come from??
Mars has no large moon, so its obliquity varies
wildly.
Laskar, 2004
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Amazonian Ice - Where did it come from??
Mars has no large moon, so its obliquity varies
wildly.
Laskar, 2004
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Amazonian Ice - Where did it come from??
Mars may be a little more like the Earth than
we thought!
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Amazonian Ice - Remember those gullies?

• Very recent (10 million years or younger)
  fluvial features.
• Two main hypotheses
• Water is erupting out of the ground.
• Water is from snow melting on the surface.

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Amazonian Ice - Remember those gullies?

• Very recent (10 million years or younger)
  fluvial features.
• Two main hypotheses
• Water is erupting out of the ground.
• Water is from snow melting on the surface.

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Amazonian Ice - Remember those gullies?

• Very recent (10 million years or younger)
  fluvial features.
• Two main hypotheses
• Water is erupting out of the ground.
• Water is from snow melting on the surface.

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Amazonian Ice - Remember those gullies?

• Very recent (10 million years or younger)
  fluvial features.
• Two main hypotheses
• Water is erupting out of the ground.
• Water is from snow melting on the surface.

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Amazonian Ice - Remember those gullies?
Frequently found in these glacial landscapes.
Could be the product of glacial recession during
an obliquity change (Head et al., 2008).
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Amazonian Ice - Remember those gullies?
Frequently found in these glacial landscapes.
Could be the product of glacial recession during
an obliquity change (Head et al., 2008).
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Amazonian Ice - Gullies forming today??
Malin et al., 2006
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Mars Reconaissance Orbiter - Testing Hypotheses
HiRISE Camera (25 cm/px) CTX Camera (6
m/px) CRISM imaging spectrometer SHARAD radar
sounder
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Mars Reconaissance Orbiter - Testing Hypotheses
HiRISE Camera (25 cm/px) CTX Camera (6
m/px) CRISM imaging spectrometer SHARAD radar
sounder
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Mars Reconaissance Orbiter - Testing Hypotheses
HiRISE Camera (25 cm/px) CTX Camera (6
m/px) CRISM imaging spectrometer SHARAD radar
sounder
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Mars Reconaissance Orbiter - Testing Hypotheses
HiRISE Camera (25 cm/px) CTX Camera (6
m/px) CRISM imaging spectrometer SHARAD radar
sounder
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Mars Reconaissance Orbiter - Testing Hypotheses
SHARAD radar sounder Emits radar pulses from
orbit and measures the amount reflected back to
the spacecraft. The time the pulse takes to
return to the spacecraft gives you information
about surface structure.
(Plaut et al., 2008)
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Mars Reconaissance Orbiter - Testing Hypotheses
SHARAD radar sounder Emits radar pulses from
orbit and measures the amount reflected back to
the spacecraft. The time the pulse takes to
return to the spacecraft gives you information
about surface structure.
(Plaut et al., 2008)
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Mars Reconaissance Orbiter - Testing Hypotheses
HiRISE Camera Acquires 25 cm/px images of the
surface. Outcrop geology on Mars!
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Mars Reconaissance Orbiter - Testing Hypotheses
HiRISE Camera Acquires 25 cm/px images of the
surface. Outcrop geology on Mars!
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Mars Reconaissance Orbiter - Testing Hypotheses
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Mars Reconaissance Orbiter - Testing Hypotheses
CRISM Measures the wavelength of light
reflected off the surface. That data can be
compared to spectra measured in laboratories.
Mineral maps generated from interpreted surface
composition.
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Mars Reconaissance Orbiter - Testing Hypotheses
CRISM Measures the wavelength of light
reflected off the surface. That data can be
compared to spectra measured in laboratories.
Mineral maps generated from interpreted surface
composition.
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Mars Reconaissance Orbiter - Testing Hypotheses
CRISM Measures the wavelength of light
reflected off the surface. That data can be
compared to spectra measured in laboratories.
Mineral maps generated from interpreted surface
composition.
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Mars Reconaissance Orbiter - Testing Hypotheses
Clay minerals detected in same location as
layered deposits!
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Mars Reconaissance Orbiter - Testing Hypotheses
What about those new, bright gully deposits?
CRISM finds no evidence for hydrated minerals or
salt deposits. Appear spectrally indistinct
from surrounding crater wall.
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Mars Reconaissance Orbiter - Testing Hypotheses
What about those new, bright gully deposits?
CRISM finds no evidence for hydrated minerals or
salt deposits. Appear spectrally indistinct
from surrounding crater wall.
Nobody knows if these were wet or dry
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Mars - Terrain Inversion!
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Mars - Hearts!
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Mars - Fish!
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Mars - Have a Nice Day
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