Aitken Crater Region of Interest
A lobate scarp (the visible part of a deep fault that distorts the surface) in the mare basalts of Aitken Crater on the moon's far side. Aitken Crater is one of 50 regions of interest in NASA’s Constellation Program. The smooth mare basalts that flooded the floor of Aitken Crater are relatively few in number on the lunar far side. Mare basalts often have wrinkle ridges and lobate scarps, tectonic landforms that express contraction of the volcanic flows. Future missions to Aitken Crater will explore this formation in search of clues to how this and other lobate scarps form. Image width is 4.5 km, NAC frame M103374879RE. Credit: NASA/Goddard/Arizona State University|
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Mare basalt-filled craters (basins) are few in number and small in size on the farside. Aitken crater is about 135 km in diameter. It is located on the northern rim of the South Pole-Aitken Basin, the largest preserved basin on the moon. The crater has a central peak and much of its original floor has been buried by younger rock. Enigmatic, reflective features called swirls are found on the floor of Aitken. Scientists are not sure how these features formed, but think they may be related to weak variations in lunar magnetism. Hummocky floored craters, impact craters formed in Aitken's mare basalt infill, have strange, bulbous hills. Their origin is also not well understood. These are some of the reasons why a Constellation Program region of interest is located within Aitken Crater. The wealth of unusual features in Aitken make it an exciting location for exploration.
The moon, like Earth and the other terrestrial planets and many of the other solid bodies in the Solar System, exhibits tectonic landforms. Tectonic landforms result from forces that have either contracted and pushed crustal material together, or extended and pulled crustal material apart. Most of the tectonic landforms on the moon are found in and around the nearside mare basins. Two contractional tectonic features, wrinkle ridges and lobate scarps, are found in mare basalts, volcanic rock that flooded the floors of the nearside impact basins after their formation. The forces that created these landforms in the mare basins are thought to be from the weight of the dense basalts that caused them to subside and contract.
Like the mare basalts in nearside basins, those in Aitken have been deformed resulting in wrinkle ridges similar in form to those on the nearside, although much smaller in scale. Near the southeastern rim of Aitken, close to the contact between the mare basalts and hummocky crater rim material, is a linear, low-relief scarp. This scarp, about 3 km in length, is very similar in size and morphology to lobate scarps found elsewhere on the Moon. Lobate scarps are relatively young landforms thought to be the surface expression of thrust faults, formed when an upper fault block is pushed up and over a lower fault block.
Outside of a mare basin, what is the origin of the tectonic forces that formed this lobate scarp? The thickness of the mare basalts in Aitken crater is small compared to the thickness in the much larger nearside basins. Is there enough mare basalt to cause subsidence and contraction? The contraction that formed the lobate scarp in Aitken crater may be from a much broader and deeper source. Lobate scarps are the most common tectonic landforms in the lunar farside highlands. The forces that formed these thrust fault scarps may come from slow cooling of the lunar interior that led to global contraction. Thus, the lobate scarp in the mare basalts of Aitken is likely due to thermal contraction of the Moon.
Examination of the base of the scarp might reveal a subtle break and offset of the basalt regolith or soil that could be evidence of the underlying thrust fault, providing important insight into when the lobate scarp formed.
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