Marius Hills

The Marius Hills are a set of volcanic domes located in Oceanus Procellarum on Earth's Moon. The domes are thought to have formed from lavas fairly more viscous than those that formed the Lunar mare. These domes average approximately 200–500 m (660–1,640 ft) in height. The Marius Hills take their name from the nearby 41 km (25 mi) diameter crater Marius. These hills represent the highest concentration of volcanic features on the Moon.

An abundance of domes, cones, and volcanic rilles and channels is characteristic of the Marius Hills. The Lunar Reconnaissance Orbiter photographed a pit that could be a skylight in an underground lava tube, indicating that part of its roof has collapsed, as often happens after lava tubes cease to be active.

Data from the Lunar Reconnaissance Orbiter has been used to identify two different varieties of domes among the Marius Hills: (1) large, irregularly shaped domes and (2) smaller domes with steep sides and diameters of about 1–2 km (0.62–1.24 mi). Another feature, possibly pyroclastic, or primarily volcanic in composition, has a roughly circular shape and steep sides. Bright, high albedo boulders have been shown to be characteristic of lava flows in the Marius Hills. This suggests blocky lava with a high silica content formed these features. This hypothesis, however, is not supported by data obtained from the Clementine lunar orbiter. Analysis of lower albedo, or less reflective boulders suggest that many domes in the area may contain two layers of material: (1) an upper layer of thin, dark material covering (2) a layer of thick, bright material.

The Marius Hills region was at one time considered a possible landing site for a lunar landing mission during the American Apollo program (eventually becoming the alternative site for Apollo 15), with the possibility of gaining insight about the volcanic history of the Moon from domes in the area.

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