Slipher is an

impact crater An impact crater is a depression (geology), depression in the surface of a solid astronomical body formed by the hypervelocity impact event, impact of a smaller object. In contrast to volcanic craters, which result from explosion or internal c ...

in the Thaumasia quadrangle of

Mars Mars is the fourth planet from the Sun. It is also known as the "Red Planet", because of its orange-red appearance. Mars is a desert-like rocky planet with a tenuous carbon dioxide () atmosphere. At the average surface level the atmosph ...

, located at 47.3°S latitude and 84.6°W longitude. It measures in diameter and was named after American astronomers Vesto and Earl Slipher. The naming was approved by IAU's Working Group for Planetary System Nomenclature in 1973.

Description

Gullies are visible on the walls of a crater that is on the rim of Slipher. They can be seen in the pictures below. Martian gullies are small, incised networks of narrow channels and their associated downslope

sediment Sediment is a solid material that is transported to a new location where it is deposited. It occurs naturally and, through the processes of weathering and erosion, is broken down and subsequently sediment transport, transported by the action of ...

deposits, found on the planet of Mars. They are named for their resemblance to terrestrial gullies. First discovered on images from Mars Global Surveyor, they occur on steep slopes, especially on the walls of craters. Usually, each gully has a dendritic ''alcove'' at its head, a fan-shaped ''apron'' at its base, and a single thread of incised ''channel'' linking the two, giving the whole gully an hourglass shape.Malin, M., Edgett, K. 2000. Evidence for recent groundwater seepage and

surface runoff Surface runoff (also known as overland flow or terrestrial runoff) is the unconfined flow of water over the ground surface, in contrast to ''channel runoff'' (or ''stream flow''). It occurs when excess rainwater, stormwater, meltwater, or other ...

on Mars. Science 288, 2330–2335. They are believed to be relatively young because they have few, if any craters. A subclass of gullies is also found cut into the faces of sand dunes which themselves considered to be quite young. On the basis of their form, aspects, positions, and location amongst and apparent interaction with features thought to be rich in water ice, many researchers believed that the processes carving the gullies involve liquid water. However, this remains a topic of active research. As soon as gullies were discovered, researchers began to image many gullies over and over, looking for possible changes. By 2006, some changes were found. Later, with further analysis it was determined that the changes could have occurred by dry granular flows rather than being driven by flowing water. With continued observations many more changes were found in Gasa Crater and others. With more repeated observations, more and more changes have been found; since the changes occur in the winter and spring, experts are tending to believe that gullies were formed from dry ice. Before-and-after images demonstrated the timing of this activity coincided with seasonal carbon-dioxide frost and temperatures that would not have allowed for liquid water. When dry ice frost changes to a gas, it may lubricate dry material to flow especially on steep slopes. In some years frost, perhaps as thick as 1 meter. File:Slipher crater 053A56.jpg, Viking Orbiter 1 image with Slipher crater at bottom File:Wikislipher.jpg, Slipher crater on Mars, as seen by MRO's CTX camera File:Wikisliphergullies.jpg, Gullies in crater on the rim of Slipher. This is an enlargement of the previous image. File:Pedestal crater in Slipher crater F04 037244 1323 XN 47S085W.jpg, The small pedestal crater in the northwestern floor of Slipher

References

{{Geography of Mars Thaumasia quadrangle Impact craters on Mars

Description

See also

References