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50km mapping orbit Sept 15
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Terabits
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Lunar Topography: Status
From July 13 to Oct 21 LOLA obtained ~ 480 million
successful altimeter measurements. (For comparison
Kaguya obtained ~10 million, total during mission life).
LOLA global DEM’s released to LRO Instrument teams at
1/4, 1/8, 1/16 degree/pixel with 90%, 48% and 28%
coverage.
Mean spacing at equator so far is 7.6 km (~1/4 degree).
In mapping orbit LOLA is acquiring ~ 105 observations per
second with an average along-track spacing of 15 meters
across the 5 profiles.
LOLA DEM Examples
Global LOLA DEM at 1/8 deg resolution
LOLA global topography supplemented
with WAC equatorial topography will allow
definitive identification of ancient degraded
basins - important information for
addressing lunar cataclysm hypothesis.
Section of LOLA DEM showing rim of South Pole Aitken
Preliminary Surprises (?)
Many craters and features have steep slopes (>30°)
Floors of many craters exhibit low slopes and have large
rms undulations (5 to10 m) on baselines of 25 to 50
meters
Higher resolution topography is suggesting a larger
number of smaller permanently shadowed areas than
previously thought
Examples: WAC DTM vs. Kaguya-LALT
Mare Orientale, 1 km DTM grid (650 x 650 km, Dh = 10.2 km)
LROC-WAC
LROC WAC Stereo DEM, J. Oberst (DLR)
Kaguya-LALT
Diviner 8-!m Region Global Composition Results
• Diviner provides direct measurements of silicate composition
• Several localized regions of unusually enriched silicate
composition have been identified
• Diviner’s measurements confirm presence of non-mare silicic
volcanism pre-dating or contemporaneous with mare volcanism
"Silicic
Basaltic#
cFb?
bFYY
cFAb
Christiansen Frequency (!m)
Diviner Polar Results
• Complete thermal maps
at both poles
• Diurnal and seasonal
thermal variability
defines the locations of
the Moon’s surface and
subsurface polar cold
traps
• Results show extensive
regions capable of
serving as cold traps for
water ice and other
volatiles
• Coldest areas in the
south polar region never
exceed 35K
• Comparison with
neutron and radar data
suggests that most of the
Moon’s “niches” for water
ice are not currently filled
Summer Solstice
!"#'84+-6'730(.3(
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LROC NAC Oblique
view rim of Cabeus
Diviner viewing LCOSS
– Q424O6-2L='$!#!T:'D0.0R"K&
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24+-6'6(O04.)
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AB
D-60*)'P0++)
E()5$.$*,(9&F:G
Vertical relief: 573 meters
DEM resolution: 5 m/pixel
2 km
Region of proposed basaltic
and silicic volcanic centers
15 km
1.5 km
1./=./D59CKC8.<5#/=5)IC66C5B.87B
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Apollo 11 landing site
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Apollo 14 Saturn IVB booster impact crater. The booster was intentionally
impacted into the lunar surface on 4 February 1971 to serve as an energy
source to probe the interior structure of the Moon with Apollo seismometers.
"(2(-,'91-O0.O
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On the left the Sun was midway to the horizon (50° incidence) and
on the right the Sun was higher (25°). Under lower Sun, surface
roughness is quite evident; under higher sun (right) variations in
brightness (reflectance) dominate the scene.
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,01(+0.('O*0/('4*6'*./(6),-./0.O'45'L(-,'G*/O(,
700 m diameter crater
K6()L'%6-,(6)
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• a('3-.')(('(<0/(.3(',L-,'G4*+/(6)
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Impact melt flow GB
!-,V'RAFc?m'!4.V'WcFAYm
197BE5!9#8795VJI#<80J768517#8>97B&
W.C9=#/C5Z9>/C5!9#8795F225MJ5=.#JH
UT%'91-O(V'D>?WbW>b\?"
UT%'91-O(V'D>?WbW>b\?!
912-3,'D(+,)
Impact melt textures are commonly well preserved in Copernican craters.
High resolution LROC topography enables modeling of viscosity and temperature of melts.
Giordano Bruno crater (22 km diameter)
Image ~2 km wide
912-3,'D(+,'$NH&
Image 2 km wide
%412-60)4.)',4'D-6)
Gullies on steep inner
slope of Byrgius A.
Probably formed from a
combination of impact
melt drainage and mass
wasting.
Martian mid-latitude
gullies typically have
larger alcoves and fans,
and channels on shallower
slopes.
Lunar geomorphology
provides a dry control
experiment for comparison
to processes on Mars that
may have required
volatiles.
M107293947L
%412-60)4.)',4'D-6)
Polygons in impact melt pond on near-rim ejecta of Jackson crater (left)
and on Elysium Planitia, Mars (interpreted as an equatorial frozen sea of
water or as extensive lava flows).
Polygons are common in ice-rich ground, but can form in other ways.
Jackson polygons here are likely due to thermal contraction (also found
on terrestrial lava flows.)
LROC M103216633L and HiRISE ESP_013526_1895
7-12+('45'SX2(3,(/'"()*+,)'5641'!"#
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Synergy of all seven LRO instruments that will push major advances!
#<(65+4J'7+0/()
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