Lava Flows in Mare Imbrium - Brown University · Stephanie Quintana GEOL 2860 Schaber, G. (1973)...
Transcript of Lava Flows in Mare Imbrium - Brown University · Stephanie Quintana GEOL 2860 Schaber, G. (1973)...
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Stephanie Quintana
GEOL 2860 Schaber, G. (1973) Lava flows in Mare Inbrium: Geological evaluation for Apollo orbital photography Bugiolacchi, R. and Guest, J. (2008) Compositional and temporal investigation of exposed lunar basalts in the Mare Imbrium region
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Background Three primary lava emplacement periods Special focus on Period III Summary Discussion Questions
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Magma ocean extensive differentiation bottom-up fractional crystallization
Mafic materials settle ferriferous and titaniferous ultramafic cumulate settle KREEP crystallization
Late production of picritic and ultramafic liquids at 130-480 km
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Basin formed around 3.85 Ga in relatively thin crust Did not penetrate down to
the mantle Extensive structural
modification Basin infilling over 800
million years Did not commence soon
after excavation phase 2nd largest basaltic region
on Moon Complex suite of low to
high-Ti basaltic lava units
NASA/JPL Galileo Spacecraft PIA00405
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Bugiolacchi & Guest (2008)
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Bugiolacchi & Guest (2008)
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Bugiolacchi & Guest (2008)
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Bugiolacchi & Guest (2008)
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Three periods of emplacement
Slightly decreasing levels of Ti and Fe with age
Bugiolacchi & Guest (2008)
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Bugiolacchi & Guest (2008)
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Period Age Extent (km)
Schaber ’73
TiO2 (wt%)
Bugiolacchi and Guest ‘08
FeO (wt%)
Bugiolacchi and Guest ‘08
Average age (Ga)
Bugiolacchi and Guest ‘08
Average age (Ga) Schaber ‘73
I Late Imbrian Epoch
1200 1.4–6.2 15.2–17.5 3.3 ± 0.1 3.0 ± 0.4
II ‘Early’ Eratosthenian Period
600 2.5–7.1 16.0–17.9 3.0 ± 0.2 2.7 ± 0.3
III ‘Middle’ Eratosthenian Period
400 2.5–9.8 15.2–18.8 2.3 ± 0.5 2.5 ± 0.3
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Source between Imbrian and “Copernican” ring structures Control migration to
surface Source could be
associated with locus of one active lunar seismic region
Morphology: Scarps 30-35 m high
Leveed channels ~20 km
Apollo 17 M-2450 Photograph
Euler
Copernicus
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Columbia River and Hawaii
Lava viscosity is less on Moon compared to Earth
Flow Velocity (Moon compared to Hawaii/Columbia River)
▪ Laminar: 1.0-1.5 times greater / 1.5-3.0 times greater
▪ Turbulent: 1.75-2.5 times less / 1.6-3.0 times less
Flow Thickness (Moon compared to Columbia River)
▪ Moon has lower gravity and a higher density lava: 1.7 times greater
Rate of extrusion likely more significant than viscosity —extrusion rate must have been large on Moon
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Three primary phases of eruption
Possibly from same source
Large flow lengths mean a high extrusion rate Extrusion rate decreased over time Ti and Fe content increased over time
Follow a trend and appear correlated
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How does eruption in a vacuum affect the flow features we are used to seeing?
What evidence do we have of magma storage beneath the surface? What kind of structure do we expect? What does the scope and composition of the lavas say about the
storage of magma beneath the surface? What evidence do we see for lava produced by
vents/fissures/volcanoes? How does flow thickness and extrusion rate change for these
features? How does the evidence for lava flows and magma storage
change in other regions of the Moon? Why might basin infilling have commenced after basin
formation?
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Bugiolacchi and Guest use craters >500m in their crater counting statistics, and avoid obvious secondary craters. Is this size still too small to obtain an accurate count (or is it still skewed by secondaries)?
Apparent bimodal distribution of TiO2
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Bimodal distribution examples Left: Clementine Right: Samples