Good lighting and high resolution cameras in the SMART-1 satellite are making it possible to put together the story linking geological and volcanic activity on the Moon.
“Thanks to low-elevation solar illumination on these high-resolution images”, says SMART-1 Project Scientist Bernard Foing, “it is now possible to study fine, small-scale geological features that went undetected earlier.”
The study provides new information on the thermal and tectonic history of the Moon and the processes following the formation of the large basins. There are approximately 50 recognizable lunar basins more than 300 km in diameter. They are believed to be created by the impact of asteroids or comets during the Lunar Late Heavy Bombardment period, 350-750 million years after the formation of the Moon. Some of these basins (mostly on the near side) were then filled in by lava originating from volcanic activity.
The positions of Mare Humorum (in green) and Oceanus Procellarum (in red) are indicated on a Mercator map of the Moon centred on the near-side. Credits: ESA/Space-X (Space Exploration Institute)
The Humorum basin is an ‘ideal’, circular, compact and moderately thick basin that was created by a simple impact event, showing a thin crust and mass concentration within a small area (from Clementine topography and gravity data).
The Procellarum basin, or Oceanus Procellarum, is a large, extended, complex basin that is moderately thick and shows no mass concentration. It may have been formed by faulting associated with the formation of the adjacent Imbrium crater (3.84 thousand million years ago), rather than by a ‘gargantuan’ impact.
The Humorum basin shows concentric graben, or elongated, trench-like erosional features around the edge of the basin. These are formed as the crust is deformed due to the presence of a mascon (mass concentration or ‘local overweight’).
This image shows graben features (red), strike slip faults (green) and wrinkle ridges (blue) as determined with SMART-1 AMIE in a context Clementine image of the Humorum basin. Graben features are elongated, trench-like erosional structures which form as the crust is deformed due to the presence of a mascon (mass concentration or 'local overweight'). Strike-slip faults are faults where the rupture is vertical and one side slides past the other. An example is the San Andreas fault along the western United States, however there is no multi-plate tectonic activity on the Moon. Wrinkle ridges in the Humorum basin are believed to be caused by thermo-mechanical deformation of the mare basalts, rather than mascon tectonics (due to mass concentration, or local 'overweight'). Credits: NASA/ Clementine
“Lunar crust is like a fragile skin, wrinkled due to local mascons or its thermal history”, says Bernard Foing, “as doctors, we searched for these skin-imprints but some may be masked underneath the last layers of basalt.”
For the first time, strike-slip faults have been observed with SMART-1 in the Humorum basin. These are faults where the rupture is vertical and one side slides past the other. An example is the San Andreas fault along the western United States. However, there is no multi-plate tectonic activity on the Moon.
Procellarum is an extended basin, where the crust is thin enough to allow magma to arise from under the surface, 4 to 2 thousand million years ago. SMART-1 images do not show geological faults, or surfaces where the rock ruptures due to differential movement, in the Procellarum basin.
This Clementine image shows wrinkle ridges detected with SMART-1 in the Procellarum basin. The wrinkle ridges are not distributed radially around the basin. Due to their location, they do not seem associated with mass concentration tectonics, but mostly are results of thermal and mechanical deformations resulting from volcanic activity - due to compression from basalt extruded by the lava. The Procellarum basin contains the youngest basalt found on the Moon so far, up to two thousand million years old. Credits: NASA/ Clementine
Procellarum shows wrinkle ridges that are not distributed radially around the basin. Due to their location, they do not seem associated with mascon tectonics, but are mostly results of thermal and mechanical deformation resulting from volcanic activity - basalt extruded by the lava causes compression in the area. The Procellarum basin contains the youngest basalt found on the Moon so far, up to 2 thousand million years old.
Different ‘pulses’ of volcanic activity in lunar history created units of lava on the surface. The flooding of mid-sized craters with lava due to volcanic activity in the region is reflected in the mineralogical map. Differences in the mineralogical composition provide a tool to study the geological history of the region. Flooded as well as unflooded craters are found in the region, reflecting the evolution of volcanic activity with time.
This picture shows the craters Hansteen (top) and Billy (bottom), both lying in the Procellarum basin. Billy is an example of a crater flooded due to volcanic activity, whereas Hansteen remains unflooded. The craters are 45 km in diameter. Credits: ESA/Space-X (Space Exploration Institute)
“This analysis shows the potential of the AMIE camera”, says Jean-Luc Josset, Principal Investigator for the AMIE camera, “and we are still analysing other datasets that make use of the varying illumination conditions during the operation of SMART-1 over one and half years”.
Article: ‘Coupling between impacts and lunar volcanism for Humorum and Procellarum basins’ by S. Peters, B. Foing, D. Koschny, A. Rossi and the SMART-1 AMIE team, presented at the European Planetary Science Congress on 22 August 2007.