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Marius Hills
Marius Hills (click to enlarge)
 
 

Marius Hills

Exploring Marius Hills will reveal more on the geologic processes that form sinuous rilles and develop new insights about lunar and planetary volcanic processes. One of the longest sinuous rilles on the Moon, the unnamed rille to the right is one of 20 rilles in the Marius Hills region. The incredible geologic diversity of the Marius region--where mare deposits, volcanic domes, sinuous rilles, and small localized pyroclastic deposits are all in easy roving distance from one another--makes the Marius Constellation site a geologist's paradise and a prime candidate for a human lunar sortie mission.

Black and white image of a ridge on the moon.
Rim of a large sinuous rille on the western edge of the Marius Hills

Viewable through terrestrial telescopes, the Marius Hills region of the Moon has been a high-priority target for human lunar exploration for almost 50 years. In fact, the Marius Hills region was one of the top candidates for an Apollo landing site (and, as memorably recounted by Don Wilhelms in To a Rocky Moon, was very nearly the choice for the Apollo 15 landing site). Had the Apollo landings not come to a premature end, it is likely that Americans would have explored the region during the early 1970s.

The geology of the Marius Hills region is very complicated. Located in southwest Oceanus Procellarum west of Marius crater (lending the region its name) and northeast of the famous Reiner Gamma formation, the Marius Hills complex represents the largest concentration of volcanic features on the Moon. Over 250 volcanic domes are found here, along with sinuous rilles, as well as some steeper-sided, roughly cone-shaped positive relief features that previous scientific investigations of the region have suggested are composed of pyroclastic materials. Unlike the domes created by nonmare volcanic processes (such as the Gruithuisen Domes, also a Constellation region of interest) which occur in the lunar highlands, near mare-highlands boundaries, the Marius Hills complex is located on a plateau that is completely surrounded by Oceanus Procellarum. Multispectral data from the 1994 Clementine mission indicates that the composition of the domes and cones in the Marius Hills complex are very similar to the surrounding mare basalts.

So, what geologic process concentrated all of these volcanic features in this region? We simply don't (yet) know the answer to that question, although based on the available data we can make a reasonable hypothesis: that the Marius Hills domes were produced billions of years ago by episodic eruptions of low effusion rate, low-temperature, viscous, high crystal content mare lavas contemporaneously with emplacement of the surrounding mare basalts. That model would require some sort of long-lived, shallow, and occasionally replenished source reservoir for the dome-forming lavas, with the sinuous rilles being formed later by subsequent eruptions of higher-effusion rate, less viscous mare materials that didn't form domes. However, we need further exploration to ascertain whether this model is accurate--or not. Important contributions to understanding the geology of the Marius Hills will be made with long-lived teleoperated surface mobility systems that can survey and explore the many geologic features in the Marius region. But, we won't know for certain until human explorers reach the region to do the fieldwork and collect the samples that we'll need to answer these key scientific questions.

Check out the full-resolution NAC frame to plan your own adventure in the Marius Hills.

For more information, see:
D. J. Heather, S. K. Dunkin, and L. Wilson (2003) Volcanism on the Marius Hills plateau: Observational analyses using Clementine multispectral data, Journal of Geophysical Research, Vol. 108, NO. E3, 5017.

Credit: NASA/GSFC/Arizona State University



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Last Updated: 3 Jan 2013