Hebes Mensa

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Hebes Mensa
Hebes Chasma based on day THEMIS.png
Hebes Chasma, seen on daytime IR THEMIS. Hebes Mensa is the feature in the center of the chasm.
Location Hebes Chasma (Valles Marineris)
Coprates quadrangle
Coordinates 1°01′S76°47′E / 1.02°S 76.78°E / -1.02; 76.78 [1]
Naming classical albedo feature [1]

Hebes Mensa is a large mensa that rises from the floor of Hebes Chasma, one of the chasmata of the Valles Marineris network on Mars. Some researchers have identified this mesa to be an interior layered deposit (ILD), similar to Ganges Mensa, and are named for alternating light-toned and dark-toned layers forming a stair-stepped stratigraphy. The faces of Hebes Mensa are sometimes fluted. [2] It is 7.5 kilometres (4.7 mi) tall and 120 by 43 kilometres (75 by 27 mi) wide. [3]

Contents

Observation history

Hebes Mensa was first named in 1982. [1]

Context

Hebes Mensa is located within the Hebes Chasma of Valles Marineris, within the Coprates quadrangle. To its east is Juventae Dorsa and the larger Lunae Planum, and to its south is Perrotin Crater and the main body of Valles Marineris (specifically Ophir Chasma). To its west are Tithoniae Fossae and Echus Chasma, the latter of which continues north of Hebes Mensa into the Lunae Palus quadrangle. Also to the north is Echus Fossae. As Hebes Mensa is part of Valles Marineris, many features which are common throughout Valles Marineris are common at Hebes Mesa. For example, many recurring slope linneae (dark, thin, seasonal features thought to be caused by modern running water) occur at Hebes Mensa. [4]

Formation theories

Many researchers have proposed a low-energy lacustrine depositional origin tied to continual groundwater feeding interspersed with occasional subaqueous volcanism. Others have contested this hypothesis, noting that Hebes Mensa is so tall that it actually stretches above the canyon walls of Hebes Chasma. Such researchers propose that Hebes Mensa is actually a tuya, modeled on ones observed in Russia's Azas Plateau and in northern Iceland, which are volcanic edifices that form due to the effects of subglacial volcanism. [5]

Another theory of the mensa’s origin ties it to the growth of its surrounding chasm; the chasm was filled by sediments, but then later grew, creating a valley between the original sediment fillings and the chasm walls. The sediments would have arrived there via either a pyroclastic (lava-related) or aeolian (wind-related) process. [6] It has also been suggested that Hebes Mensa is a salt dome. In this theory, 3 kilometres (1.9 mi) deep subsurface brine pools were heated up from below, causing the salt to separate from the water and displace the regolith above. This method of formation would also explain some aspects of Hebes Chasma formation as well. A terrestrial analogue would be Conrad and Thetis Deep at the Red Sea. [7]

Geology

Hebes Mensa's geology has been compared to Bishop Tuff, California. Bishop tuff.jpg
Hebes Mensa’s geology has been compared to Bishop Tuff, California.

Hebes Mensa is estimated to be the same age as other interior layered deposits in Mars, dating back to the Hesperian period of Mars’ history. [8] [9] [3] It can be split into at least three geological units, the Lower, Upper, and Late interior layered deposit units (ILDs). The Lower and Upper ILDs make up the bulk of the mensa, whereas the Late ILD is located in the valley between Hebes Mensa and the northern wall of the surrounding chasm. The Lower ILD underwent shallow folding. All layers are believed to have been shaped by past glacial activity, and ash falls are thought to have played an important role as well. [3]

The Lower ILD encompasses the materials at elevations from −3.7 to −1.4 kilometres (−2.30 to −0.87 mi), and the Upper ILD ranges from −1.4 to 3.8 kilometres (−0.87 to 2.36 mi). The Upper ILD has regions both light and dark in tone, although in general it is lighter than the Lower ILD. Yardangs are found in the Upper ILD. The Late ILD ranges over an area of 700 square kilometres (270 sq mi), and can be found in elevations ranging from −2.8 to −0.1 kilometres (−1.740 to −0.062 mi). It contains hummocks and polygons, which are not typically found in the other units. [3] The Late ILD only partially overlaps Hebes Mensa proper, although what remains is completely contained in Hebes Chasma. [10]

There have been at least 4 major landslides from the mesa. These past landslides have left scars, exposing the insides of the feature that are similar in composition to the outer layers. This lends confidence to deductions that have been made using outer layer geology. One such deduction is based on the presence of both mono- and poly-hydrated sulfates (with a transition between the two occurring between elevations 800 and 900 metres (2,600 and 3,000 ft)); their thorough presence implies that the mensa could have been saturated with water at the time of its formation. [3]

The central mound has a shallow slope of only 3°. The northern slopes have an average incline of 17°, whereas the southern slops are steeper, with an average incline of 27°. The northern side has undergone more erosion, and yardangs are more prevalent there. In the northeast, there are many wrinkle ridges, and to the west are many parallel faults. There are not many faults in the southern plateau. [10]

Related Research Articles

<span class="mw-page-title-main">Valles Marineris</span> Valleys on Mars

Valles Marineris is a system of canyons that runs along the Martian surface east of the Tharsis region. At more than 4,000 km (2,500 mi) long, 200 km (120 mi) wide and up to 7 km (23,000 ft) deep, Valles Marineris is the largest canyon of the Solar System.

Vallis or valles is the Latin word for valley. It is used in planetary geology to name landform features on other planets.

<span class="mw-page-title-main">Thermal Emission Imaging System</span> Camera aboard NASAs 2001 Mars Odyssey orbiter

The Thermal Emission Imaging System (THEMIS) is a camera on board the 2001 Mars Odyssey orbiter. It images Mars in the visible and infrared parts of the electromagnetic spectrum in order to determine the thermal properties of the surface and to refine the distribution of minerals on the surface of Mars as determined by the Thermal Emission Spectrometer (TES). Additionally, it helps scientists to understand how the mineralogy of Mars relates to its landforms, and it can be used to search for thermal hotspots in the Martian subsurface.

<span class="mw-page-title-main">Eos Chasma</span> Chasma on Mars

Eos Chasma is a chasma in the southern part of the Valles Marineris canyon system of the Coprates quadrangle and the Margaritifer Sinus quadrangles of the planet Mars.

In planetary nomenclature, a chasma is a deep, elongated, steep-sided depression. As of 2020, the IAU has named 122 such features in the Solar System, on Venus (63), Mars (25), Saturn's satellites Mimas (6), Tethys (2), Dione (8) and Rhea (5), Uranus's satellites Ariel (7), Titania (2) and Oberon (1) and Pluto's satellite Charon (3). An example is Eos Chasma on Mars.

<span class="mw-page-title-main">Juventae Chasma</span> Box canyon on Mars

Juventae Chasma is an enormous box canyon on Mars which opens to the north and forms the outflow channel Maja Valles. Juventae Chasma is located north of Valles Marineris in the Coprates quadrangle and cuts more than 5 km into the plains of Lunae Planum.

<span class="mw-page-title-main">Melas Chasma</span> Chasma on Mars

Melas Chasma is a canyon on Mars, the widest segment of the Valles Marineris canyon system, located east of Ius Chasma at 9.8°S, 283.6°E in Coprates quadrangle. It cuts through layered deposits that are thought to be sediments from an old lake that resulted from runoff of the valley networks to the west. Other theories include windblown sediment deposits and volcanic ash. Support for abundant, past water in Melas Chasma is the discovery by MRO of hydrated sulfates. In addition, sulfate and iron oxides were found by the same satellite. Although not chosen as one of the finalists, it was one of eight potential landing sites for the Mars 2020 rover, a mission with a focus on astrobiology.

<span class="mw-page-title-main">Hebes Chasma</span> Chasma on Mars

Hebes Chasma is an isolated chasma just north of the Valles Marineris canyon system of Mars. It is centered at 1 degree southern latitude and 76 degrees western longitude, just between the Martian equator and the Valles Marineris system, just east of the Tharsis region.

<span class="mw-page-title-main">Echus Chasma</span> Chasma on Mars

Echus Chasma is a chasma in the Lunae Planum high plateau north of the Valles Marineris canyon system of Mars. It is in the Coprates quadrangle. Clay has been found within it, meaning that water once sat there for a time. It may have been one of the many lakes that have been advanced for the Martian past.

<span class="mw-page-title-main">Coprates quadrangle</span> Map of Mars

The Coprates quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Coprates quadrangle is also referred to as MC-18. The Coprates quadrangle contains parts of many of the old classical regions of Mars: Sinai Planum, Solis Planum, Thaumasia Planum, Lunae Planum, Noachis Terra, and Xanthe Terra.

<span class="mw-page-title-main">Eos Chaos</span> Chaos on Mars

Eos Chaos is a rough, collapsed area in the Coprates quadrangle on Mars at 16.8° south latitude and 46.9° west longitude. It is about 490 km long and was named after the Greek name of Aurora, an albedo feature.

<span class="mw-page-title-main">Capri Mensa</span> Mensa on Mars

Capri Mensa is a mesa in the Coprates quadrangle of Mars at 14° south latitude and 47.4° west longitude. It is about 275 km long and was named after a classical albedo feature name.

<span class="mw-page-title-main">Ophir Chasma</span> Canyon on Mars

Ophir Chasma is a canyon in the Coprates quadrangle of Mars at 4° south latitude and 72.5° west longitude. It is about 317 km long and was named after Ophir, a land mentioned in the Bible. In the Bible it was the land which King Solomon sent an expedition that returned with gold. It is a classical albedo feature name.

<span class="mw-page-title-main">Ius Chasma</span> Canyon on Mars

Ius Chasma is a large canyon in the Coprates quadrangle of Mars at 7° south latitude and 85.8° west longitude. It is about 938 km long and was named after a classical albedo feature name.

Tithonium Chasma is a large canyon in the Coprates quadrangle of Mars at 4.6° south latitude and 84.7° west longitude. It is about 810 km long and was named after a classical albedo feature.

<span class="mw-page-title-main">Coprates Chasma</span> Chasma on Mars

Coprates Chasma is a huge canyon in the Coprates quadrangle of Mars, located at 13.4° south latitude and 61.4° west longitude, part of the Valles Marineris canyon system. It is 966 km (600 mi) long and was named after a classical albedo feature name. It was named from the classical Greek name for the Dez River in Persia.

<span class="mw-page-title-main">Ganges Mensa</span> Mensa in the Coprates quadrangle of Mars

Ganges Mensa is a mesa and an interior layered deposit in Ganges Chasma, one of the peripheral valleys of Valles Marineris on Mars. The mesa rises up to 4 kilometres (13,000 ft) from the floor of Ganges Chasma, nearly to the same elevation as the surrounding plateaux of Lunae Planum. Like Hebes Mensa, the mesa is completely separated from the surrounding canyon walls and has sustained significant erosion that has caused it to retreat in areal extent.

To date, interplanetary spacecraft have provided abundant evidence of water on Mars, dating back to the Mariner 9 mission, which arrived at Mars in 1971. This article provides a mission by mission breakdown of the discoveries they have made. For a more comprehensive description of evidence for water on Mars today, and the history of water on that planet, see Water on Mars.

<span class="mw-page-title-main">Lakes on Mars</span> Overview of the presence of lakes on Mars

In summer 1965, the first close-up images from Mars showed a cratered desert with no signs of water. However, over the decades, as more parts of the planet were imaged with better cameras on more sophisticated satellites, Mars showed evidence of past river valleys, lakes and present ice in glaciers and in the ground. It was discovered that the climate of Mars displays huge changes over geologic time because its axis is not stabilized by a large moon, as Earth's is. Also, some researchers maintain that surface liquid water could have existed for periods of time due to geothermal effects, chemical composition or asteroid impacts. This article describes some of the places that could have held large lakes.

<span class="mw-page-title-main">Louros Valles</span> Martian valleys

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References

  1. 1 2 3 "Gazetteer of Planetary Nomenclature: Hebes Mensa". United States Geological Survey. 2006. Retrieved 11 November 2018.
  2. ↑ Beyer, RA; McEwen, AS (2005). "Constraints on the Origin of Fine Layers in Ganges Mensa and Hebes Mensa, Mars" (PDF). Abstracts of the Lunar and Planetary Science Conference (1070): 1070. Bibcode:2005LPI....36.1070B . Retrieved 12 November 2018.
  3. 1 2 3 4 5 6 Schmidt, Gene; Fueten, Frank; Stesky, Robert; Flahaut, Jessica; Hauber, Ernst (2018). "Geology of Hebes Chasma, Mars: 1. Structure, Stratigraphy, and Mineralogy of the Interior Layered Deposits". Journal of Geophysical Research: Planets. 123 (11): 2893–2919. Bibcode:2018JGRE..123.2893S. doi: 10.1029/2018JE005658 . ISSN   2169-9100.
  4. ↑ Stillman, David E.; Michaels, Timothy I.; Grimm, Robert E. (2017-03-15). "Characteristics of the numerous and widespread recurring slope lineae (RSL) in Valles Marineris, Mars". Icarus. 285: 195–210. Bibcode:2017Icar..285..195S. doi:10.1016/j.icarus.2016.10.025. ISSN   0019-1035.
  5. ↑ Komatsu, G.; Ori, G.G.; Ciarcelluti, P.; Litasov, Y.D. (2004). "Interior layered deposits of Valles Marineris, Mars: analogous subice volcanism related to Baikal Rifting, Southern Siberia". Planetary and Space Science. 52 (1–3): 167–187. Bibcode:2004P&SS...52..167K. doi:10.1016/j.pss.2003.08.003.
  6. ↑ "1982LPSC...12.1459P Page 1459". adsabs.harvard.edu. Bibcode:1982LPSC...12.1459P . Retrieved 2021-06-22.
  7. ↑ Hovland, M; Rueslatten, H; Johnsen, H.K.; Fichler, C.; Schreiber, B.C. (2011). "Hydrothermal evaporites – on Earth and on Mars". International Association of Sedimentologists (IAS). Annual meeting, Alghero, Sardinia, Book of Abstracts.
  8. ↑ Head, J. W.; Greeley, R.; Golombek, M. P.; Hartmann, W. K.; Hauber, E.; Jaumann, R.; Masson, P.; Neukum, G.; Nyquist, L. E.; Carr, M. H. (2001). "Geological Processes and Evolution". In Kallenbach, Reinald; Geiss, Johannes; Hartmann, William K. (eds.). Chronology and Evolution of Mars. Space Sciences Series of ISSI. Vol. 12. Dordrecht: Springer Netherlands. pp. 263–292. doi:10.1007/978-94-017-1035-0_9. ISBN   978-94-017-1035-0.
  9. ↑ Schultz, Richard A. (June 1998). "Multiple-process origin of Valles Marineris basins and troughs, Mars". Planetary and Space Science. 46 (6–7): 827–834. Bibcode:1998P&SS...46..827S. doi:10.1016/S0032-0633(98)00030-0. ISSN   0032-0633.
  10. 1 2 "GEOLOGY OF HEBES CHASMA, VALLES MARINERIS, MARS" (PDF). Master's Project for Faculty of Earth Sciences, Brock University St. Catharines, Ontario. 2015.
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