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HORIZONTAL FORCES WITHIN LUNAR CRUST: INTRIGUING A QUESTIONING MIND
Nilanjan Dasgupta ([email protected]), Trishit Ruj ([email protected]), Anup Das ([email protected]), Sriram Saran 1 1 2 2
1 2 Presidency University, Kolkata-700073, India, Space Application Centre, Ahmedabad-380015, India.
Fig. 7: Figure showing the systematic development of horse.(redrawn after Ramsay and Huber,
1997, p. 533).
HBridge
Step 1 Step 2
Remnant
1. INTRODUCTION
Surface morphological features of planetary bodies have been extensively used for
structural and kinematic studies by comparing such features with similar looking [1], [2], [3]
terrestrial ones; the later act as analogues and aid to a better understanding of the
processes of their formation.
The basic assumption for such a correlation is that we believe the processes that led to the
formation of any earthly regional scale feature remains same for the development of a
similar feature on planetary bodies.
We here describe a topographic feature on the lunar crust that is found in the active strike
slip zones of the earth, where the faults accommodate the horizontal displacement [4], [5],
[6]. The term 'en-echelon faults' refers to closely spaced, parallel or sub-parallel,
overlapping in a step-like minor faults in rock, which lie oblique to the overall structural trend
of the strike slip fault system. We describe similar features from the Earth's moon and
discuss on its tectonic significance. The paradox lies in the fact that presence of dynamic
stresses are absent within Earth's moon.
10km N
E
S
W
2 km
N
H
50km
o5 E o8 E
o9 N
o7 NRima Hyginus
Hyginus crater
Rima Ariadaeus
g g’
1
2
3
Fig. 1, 2, 3: LRO-WAC mosaic image of Hyginus crater (HC) showing Rima Hyginus (RH) and Rima
Ariadius (RA). Note that the RH and RA are arranged in en-echelon pattern with a cross graben similar
to a transverse fault. Within the segment 'a' sharp change in the strike of the graben margin from NW-
SE to almost E-W is seen,implying a change in the orientation of the principal stress within the overall
stress regime. Segment 'b' is a blown up image showing thickening of the graben wall within the RH.
2. STUDY AREA
We concentrate on the geometry and fracture pattern of one such rille, Rima Hyginus (RH),
located south of the Mare Vaporum in the near side of the moon (Fig.1). RH is situated
within Imbrium basin, structurally a broad structural trough, believed to have a fault related
origin, extending for km and nearly 3 km in width. The depth of the graben is around 220
500±80 m. The general topography is gently undulating (Fig. 4).
3. DATA SET USED
We have utilized Digital Elevation Models (DEM) from the LOLA and LRO-WAC
(100m/pixel), LRO-NAC datasets from the Lunar Reconnaissance Orbiter (LRO) and
processed them with J-Mars , ENVI. [7]
SUMMARY
We suggest from the study of en-echelon faults and related
features, a local scale horizontal transport is visible in lunar
crust, devoid of plate tectonics.
f’f0.00 1.00 2.00 3.00 4.00 5.00 6.00 7.00 8.00 9.00 10.00
Distance in km
H
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g g’
RH
Fig. 4: This section is drawn in E-W section from
LRO-WAC equatorial DTM. 100 times vertically
exaggerated.
Fig. 5: 3D section showing the presence of the
horse in the study area.
4. STRUCTURAL GEOMETRY OF THE STUDY AREA
Close inspection reveals RH is segmented into smaller linear grabens, arranged in en-
echelon pattern often with a sharp change in the trend of these grabens (Fig. 1, 2 and 3).
The topography is gently undulating with a thin veneer of pyroclastic material resting upon
the basaltic floor . Our analyses of RH reveal that the trend of the graben rotates from E-[8]
W to NW-SE indicating rotation of the stress regime. This is accompanied by thickening of
the graben wall on its either flank. Profile sections drawn indicate presence of horses
(marked by H) (Fig. 5) on the southern flanks of RH. We infer that the extensional stress has
produced small scale faults en-echelon to the major fracture responsible for graben
formation (Fig. 3). The tip lines of two adjacent en-echelon faults rotate and join to form a
continuous graben and these horses remain as central remnant of en-echelon fractures
(Fig. 5). Horses, within the median portions of two en-echelon faults, are reported from the
moon for the first time.
It is seen that in some regions affected by normal faulting too, the fault propagate along
strike in an en-echelon pattern with a cross fault joining the tips of the laterally offset faults
(Fig. 6). In such cases, differential slip along the lengths of the fault may ultimately lead to
the formation of tectonic horses within the fault zone .[9]
a
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a’0.25 0.50 0.75 1.00 1.25 1.50 1.75 2.00 2.25 2.50 2.75 3.00 3.25 3.50 3.75 4.00 4.25 4.50 4.75 5.00 5.25 7.757.507.257.006.756.506.256.005.755.50
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Distance in km
H
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-980-970
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Fig. 6: LRO-WAC mosaic image of Rima Hyginus draped on LOLA DEM (100m), the elevation profiles
across four transects, a-a'; b-b'; c-c'; and d-d' are shown below. Note the presence of horses (marked by H on d-d'
profile plot) on Rima Hyginus (3D generated by ACT).
5. DISCUSSION
The en-echelon fault systems are mainly associated with the active strike slip tectonic zones
of the earth where simple shear plays a dominant part in the overall stress regime of the
area. Some recent reports [10] of incipient stresses leading to new fracture formation in the
lunar crust has spurted new thoughts in believing the existence of tectonic activity in the
lunar crust. Our study shows that some amount of shear stress is operative on the lunar crust
leading to limited horizontal displacement of crustal blocks.
The tectonic horses within the lunar crust can therefore form in either of the two stress
regimes a) under shear stress regime or b) tensile stress regime. The two stress regimes
greatly differ in the principal stress vector orientations [11]. Large scale horizontal
displacement as seen on earth is unlikely in moon for the absence of plate tectonics. The
major stress is impact induced [2] and this stress gets transmitted through long distances
within the lunar crust producing fractures [1] in the lunar crust. These fractures are typically
segmented and often in an en-echelon pattern to the major fault zone (Fig. 7). The obliquity
of such fracture system to the major graben wall and the slip along these oblique fracture
planes probably lead to a concentration of shear stress on a local scale. We suggest that
small scale horizontal transport occurred within the lunar crustal blocks, at least to a local
scale, even in the absence of plate tectonics.
6. REFERENCES
[1] Melosh H. J. (2010) Planetary Surface Processes, Cambridge University Press, 500p., [2] Greeley
R. (2013) Introduction to Planetary Geomorphology, Cambridge University Press, pp 1-90, [3] Watters
T. R. and Schultz R. A. (2010) Planetary Tectonics, Cambridge University Press p.518, [4] Twiss R. J. ndand Moores E. M. (2007) Structural Geology 2 Ed. Susan Finnemore Brennan p [5] Davis G. H. and .
rdReynolds S. J. (2011) Structural Geology of Rocks and Regions, 3 Edition p. 864, [6] Van Der Pluijm B. ndA. and Marshak S. (2004) Earth Structure An Introduction to Structural Geology and Tectonics, 2 Ed.
pp 656, [7] Christensen P. R. JMARS – A Planetary GIS, http://adsabs.harvard. edu/abs/2009 AGUFMI
M2 2A.06C [8] http://www.lpi.usra.edu/resources/mapcatalog/usgs/I945/ [9] Ramsay. J. G. and
Huber. M. I. (1997) The techniques of Modern Structural Geology, v2, Folds and fractures, Academic
Press, 2nd edition. [10] Watters T. R. et al. (2012) Nature Geosciences, 5, 181-185.