rill

Rille (German for 'groove') is typically used to describe any of the long, narrow depressions in the lunar surface that resemble channels. Typically a rille can be up to several kilometers wide and hundreds of kilometers in length. However, the term has also been used loosely to describe similar structures on a number of planets in the Solar System, including Mars, Venus, and on a number of moons. All bear a structural resemblance to each other.

Rimae on the floor of the lunar crater Gassendi, from Apollo 16.

Mamers Vallis rille on Mars.

Rima Ariadaeus is categorized as a straight and branching rille and is over 300 km in length.

Structures

Three types of rille are found on the lunar surface:

• Sinuous rilles meander in a curved path like a mature river, and are commonly thought to be the remains of collapsed lava tubes or extinct lava flows. They usually begin at an extinct volcano, then meander and sometimes split as they are followed across the surface. Vallis Schröteri in Oceanus Procellarum is the largest sinuous rille.

• Arcuate rilles have a smooth curve and are found on the edges of the dark lunar maria. They are believed to form when the lava flows that created a mare cool, contract, and sink. These are found all over the moon, examples can be seen near the south-western border of Mare Tranquillitatis and on the south-eastern border of Mare Humorum.

• Straight rilles follow long, linear paths and are believed to be grabens, sections of the crust that have sunk between two parallel faults. These can be readily identified when they pass through craters or mountain ranges. Vallis Alpes is by far the largest graben rille, indeed it is regarded as too large to be called a rille and is itself bisected by a straight rille; Rupes Recta in Mare Nubium is a clearer example.

Rilles which show more than one structure are termed hybrid rilles. Rima Hyginus in Sinus Medii is an example, initially formed through a fault and subsequently subject to volcanic activity.

Formation

Precise formation mechanisms of rilles have yet to be determined. It is likely that different types formed by different processes. Common features shared by lunar rilles and similar structures on other bodies suggest that common causative mechanisms operate widely in the solar system. Leading theories include lava channels, collapsed lava tubes, near-surface dike intrusion, nuee ardente (pyroclastic cloud), subsidence of lava-covered basin and crater floors, and tectonic extension. On-site examination would be necessary to clarify exact methods.

Potential

In 2009, a hole was found in the lunar surface near the Marius Hills that may connect to an underground lava tube. The hole is 65 metres in diameter and may extend downward at least 80 metres. The lava tube may have a diameter of 370 metres. This tube could provide radiation shielding for an underground lunar colony. However, it is unclear whether the tube is open or accessible. Two other lunar sites have been found by remote sensing, including on the far side's Mare Ingenii. ^[1]

References

General

See also

• Arachnoid (astrogeology)
• Chaos terrain
• Dark dune spot
• List of features on the Moon
• Lunar lava tube
• Martian spiders
• Planetary geology
• Splitting of the moon