lobateness of martian ejecta craters using thermal imaging nicholas kutsop dr. nadine g. barlow nasa...
TRANSCRIPT
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Lobateness of Martian Ejecta Craters Using Thermal Imaging
Nicholas KutsopDr. Nadine G. Barlow
NASA Space GrantNorthern Arizona University Department of Physics and
Astronomy
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Some info
• Lobateness Sinuosity How Flowery vs Circular the Ejecta Blanket Looks
• Γ=P/(4πA)1/2 • THEMIS - Thermal Emission Imaging System
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AS ONE INCREASES IN LATITUDE, ONE WOULD EXPECT AN INCREASE IN WATER ICE CONTENT IN THE NEAR SURFACE REGION, LEADING ONE TO EXPECT TO OBSERVE A PROPORTIONAL INCREASE IN LOBATENESS OF THE EJECTA.
Original Proposition
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MLER,DLER,SLER
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Ok well why?• Martian craters differ significantly from those on the Moon or
Mercury
Lunar Ballistic
Martian Rampart
• Could be due to atmospheric turbulence following impact, or could be due to volatiles in the regolith
• Atmospheric theory falls short following investigation of icy satellites
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What does it mean?
• Water ice on Mars? (Snapshots in Time)
• Water deep below the surface? (Mother Natures Tunnel Boring Machine)
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A new look for old data• THEMIS resolution
(100m/p) vs. Viking resolution
(300m/p)• Layer types
lobateness consistent with previous studies
• Multiple differences between 1994 and 2010 data
Layer Type Lobateness
MLER AVG 1.56
MLER MIN 1.15
MLER MAX 2.18
SLER AVG 1.35
SLER MIN 1.10
SLER MAX 2.24
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Significant Differences• 382 SLER, 137 MLER, 519
Total from 0-30°• 2008 SLER, 937 MLER, 2945
Total from 0-30°
Layer TypeMedian Values as of
2012
MLER Median 0-10 N 1.54
MLER Median 10-20 N 1.48
MLER Median 20-30 N 1.42
SLER Median 0-10 N 1.54
SLER Median 10-20 N 1.48
SLER Median 20-30 N 1.42
Layer TypeMedian Values as of
1994
MLER Median 0-10 N 1.19
MLER Median 10-20 N 1.19
MLER Median 20-30 N 1.19
SLER Median 0-10 N 1.10
SLER Median 10-20 N 1.10
SLER Median 20-30 N 1.11
Average % Difference = 77.446
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The data thus far…
0 60 120 180 240 300 360
0
5
10
15
20
25
30
Lon
Lat
Plot of All Craters
1.2
1.3
1.4
1.5
1.6
1.7
1.8
1.9
2
2.1
2.2
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10 20 30 40 50 60 70 80 90 1001
1.5
2
2.5
Diameter
Loba
tene
ss
Lobateness vs Diameter
y = 0.002*x + 1.5
vs. Dia
linear
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0 5 10 15 20 25 30-1
-0.5
0
0.5
1residuals
Linear: norm of residuals = 8.3625
0 5 10 15 20 25 301
1.5
2
2.5
Latitude
Loba
tene
ss
Lobateness vs Latitude
y = - 0.0057*x + 1.6
vs Lat.
linear
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0 5 10 15 20 25 30
1.4
1.45
1.5
1.55
1.6
Latitude
Lobate
ness
SLER Lobateness vs Latitude (5 Avg)
y = - 0.0058*x + 1.6
vs Lat
linear
0 5 10 15 20 25 30
1.4
1.45
1.5
1.55
1.6
Latitude
Lobate
ness
MLER Lobateness vs Latitude (5 Avg)
y = - 0.0047*x + 1.6
vs Lat
linear
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Γ=NEGATIVE(≈.0055)Lat+1.6?
0 5 10 15 20 25 301.42
1.44
1.46
1.48
1.5
1.52
1.54
1.56
1.58
Latitude
Lobate
ness
Lobateness vs Latitude (5 Avg)
y = - 0.0055*x + 1.6
vs Lat
linear
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Where are we and what next?
• Is the previously put forth model for lobateness accurate?
• What new hypothesis can we generate from this data?
• Lobateness at higher latitudes• The southern hemisphere• Compare to older data• Correlation between age and lobateness
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And thank you…
• Dr. Nadine G Barlow• NAU Department of Physics and Astronomy• NASA Space Grant• Wikipedia for the pictures• MatLab for the graphs• The team of JMars
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Quick Info
• Total Craters = 3029• DLER=3%• SLER=66%• MLER=31%• Residual = Goodness of Fit
n
1i
2id)2/1()^2).^d(abs(sum)2,d(norm
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Bonus Pictures
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MLER Avg
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MLER Max
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MLER Min
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SLER Avg
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SLER Max
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SLER Min