# Slipher (Martian crater)

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This article is about the crater on Mars. For the lunar crater, see [Slipher (lunar crater)](/source/Slipher_(lunar_crater)).

Crater on Mars

Slipher Crater Topographic location map of Slipher Crater. Planet Mars Coordinates 47°18′S 84°36′W / 47.3°S 84.6°W / -47.3; -84.6 Quadrangle Thaumasia Diameter 127 km (79 mi) Eponym Vesto and Earl Slipher

**Slipher** is an [impact crater](/source/Impact_crater) in the [Thaumasia quadrangle](/source/Thaumasia_quadrangle) of [Mars](/source/Mars), located at 47.3°S latitude and 84.6°W longitude. It measures 127 kilometres (79 mi) in diameter and was named after American astronomers [Vesto](/source/Vesto_Slipher) and [Earl Slipher](/source/Earl_Slipher). The naming was approved by IAU's [Working Group for Planetary System Nomenclature](/source/Working_Group_for_Planetary_System_Nomenclature) in 1973.[1]

## 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](/source/Gullies_on_Mars) are small, incised networks of narrow channels and their associated downslope [sediment](/source/Sediment) deposits, found on the planet of Mars. They are named for their resemblance to terrestrial [gullies](/source/Gully). First discovered on images from [Mars Global Surveyor](/source/Mars_Global_Surveyor), they occur on steep slopes, especially on the walls of craters. Usually, each gully has a [dendritic](/source/Dendritic_drainage#Drainage_patterns) *alcove* at its head, a [fan-shaped](/source/Alluvial_fan) *apron* at its base, and a single thread of incised *channel* linking the two, giving the whole gully an hourglass shape.[2] 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,[2] researchers began to image many gullies over and over, looking for possible changes. By 2006, some changes were found.[3] Later, with further analysis it was determined that the changes could have occurred by dry granular flows rather than being driven by flowing water.[4][5][6] With continued observations many more changes were found in Gasa Crater and others.[7]

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.[8][9][10] In some years frost, perhaps as thick as 1 meter.

		- [Viking Orbiter 1](/source/Viking_program) image with Slipher crater at bottom

		- Slipher crater on Mars, as seen by [MRO](/source/Mars_Reconnaissance_Orbiter)'s CTX camera

		- Gullies in crater on the rim of Slipher. This is an enlargement of the previous image.

		- The small pedestal crater in the northwestern floor of Slipher

## See also

- [List of craters on Mars](/source/List_of_craters_on_Mars)

## References

1. **[^](#cite_ref-1)** [International Astronomical Union](/source/International_Astronomical_Union) (IAU) Working Group for Planetary System Nomenclature (WGPSN). ["Slipher on Mars"](https://planetarynames.wr.usgs.gov/Feature/5600). *Gazetteer of Planetary Nomenclature*. US Geological Survey. Retrieved 2 February 2021.

1. ^ [***a***](#cite_ref-Malin,_M._2000_2-0) [***b***](#cite_ref-Malin,_M._2000_2-1) Malin, M., Edgett, K. 2000. Evidence for recent groundwater seepage and [surface runoff](/source/Surface_runoff) on Mars. Science 288, 2330–2335.

1. **[^](#cite_ref-3)** Malin, M., K. Edgett, L. Posiolova, S. McColley, E. Dobrea. 2006. Present-day impact cratering rate and contemporary gully activity on Mars. Science 314, 1573_1577.

1. **[^](#cite_ref-4)** Kolb, et al. 2010. Investigating gully flow emplacement mechanisms using apex slopes. Icarus 2008, 132-142.

1. **[^](#cite_ref-5)** McEwen, A. et al. 2007. A closer look at water-related geological activity on Mars. Science 317, 1706-1708.

1. **[^](#cite_ref-6)** Pelletier, J., et al. 2008. Recent bright gully deposits on Mars wet or dry flow? Geology 36, 211-214.

1. **[^](#cite_ref-7)** NASA/Jet Propulsion Laboratory. "NASA orbiter finds new gully channel on Mars." ScienceDaily. ScienceDaily, 22 March 2014. www.sciencedaily.com/releases/2014/03/140322094409.htm

1. **[^](#cite_ref-8)** ["NASA Spacecraft Observes Further Evidence of Dry Ice Gullies on Mars"](https://www.jpl.nasa.gov/news/news.php?release=2014-226). *[Jet Propulsion Laboratory](/source/Jet_Propulsion_Laboratory)*.

1. **[^](#cite_ref-9)** ["HiRISE | Activity in Martian Gullies (ESP_032078_1420)"](http://hirise.lpl.arizona.edu/ESP_032078_1420).

1. **[^](#cite_ref-10)** ["Gullies on Mars Carved by Dry Ice, Not Water"](http://www.space.com/26534-mars-gullies-dry-ice.html). *[Space.com](/source/Space.com)*. 16 July 2014.

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Adapted from the Wikipedia article [Slipher (Martian crater)](https://en.wikipedia.org/wiki/Slipher_(Martian_crater)) by Wikipedia contributors ([contributor history](https://en.wikipedia.org/wiki/Slipher_(Martian_crater)?action=history)). Available under [Creative Commons Attribution-ShareAlike 4.0 International](https://creativecommons.org/licenses/by-sa/4.0/). Changes may have been made.