Hesperia Planum

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Hesperia Planum
Hesperia Topo Map.jpg
MOLA colorized relief map of Hesperia Planum region. Hesperia Planum has fewer impact craters than the surrounding Noachian highlands of Tyrrhena Terra and Terra Cimmeria. This indicates that the plain is younger than its more heavily cratered surroundings.
Feature typeLava plain
Location Mare Tyrrhenum quadrangle, Mars
Coordinates 21°25′S109°53′E / 21.417°S 109.883°E / -21.417; 109.883 [1]
Diameter~1 600 km [1]
EponymPoetic Hesperia

Hesperia Planum is a broad lava plain in the southern highlands of the planet Mars. The plain is notable for its moderate number of impact craters and abundant wrinkle ridges. It is also the location of the ancient volcano Tyrrhena Mons (Tyrrhena Patera). The Hesperian time period on Mars is named after Hesperia Planum. [2] [3]

Contents

MOLA map showing exact boundaries of it and other regions. Color indicates elevation. Wikiterracimmeriaboundaries.jpg
MOLA map showing exact boundaries of it and other regions. Color indicates elevation.

Name origin

Viking MDIM of Mare Tyrrhenum quadrangle. Hesperia is the intermediate-toned (dusky) region (left of center) lying between the darker regions Mare Tyrrhenum (left) and Mare Cimmerium (right). PIA00182-MC-22-MareTyrrhenumRegion-19980605.jpg
Viking MDIM of Mare Tyrrhenum quadrangle. Hesperia is the intermediate-toned (dusky) region (left of center) lying between the darker regions Mare Tyrrhenum (left) and Mare Cimmerium (right).

Most place names on Mars are derived from sources in the Bible or classical antiquity. [4] Hesperia is a Greco-Latin poetic term for "lands to the west," which to the ancient Greeks and Romans meant Italy, while Spain was referred as Hesperia Ultima. [5] [6] Planum (pl. plana) is Latin for plateau or high plain. It is a descriptor term used in planetary geology for a relatively smooth, elevated terrain on another planet or moon. [7]

The Hesperia region of Mars was named by Italian astronomer Giovanni Schiaparelli in 1877 for an intermediate-toned albedo feature centered at lat. 20°S, long. 240°W between two darker regions. [5] [8] Believing the dark areas were bodies of water, Schiaparelli interpreted Hesperia to be a floodplain or marsh bridging two adjacent seas, the Mare Tyrrhenum and Mare Cimmerium. [9] Although the existence of seas on Mars had been discounted by the early 20th century, [10] the true nature of the region remained obscure until the space age. In 1972, the Mariner 9 spacecraft showed that Hesperia was a cratered, wind-streaked plain. [11] The International Astronomical Union (IAU) formally named the area Hesperia Planum in 1973. [12] The dark areas flanking Hesperia Planum were found to be heavily cratered uplands. In 1979, the IAU designated the upland area to the west as Tyrrhena Terra and to the east as Terra Cimmeria. [13] (Terra is a Latin descriptor term meaning land or continent.)

Location and physical description

Closeup of the surface of northwestern Hesperia Planum, as seen by HiRISE camera on Mars Reconnaissance Orbiter (MRO). NW Hesperia PSP 010337 1650 RED.jpg
Closeup of the surface of northwestern Hesperia Planum, as seen by HiRISE camera on Mars Reconnaissance Orbiter (MRO).

Hesperia Planum is located along the broad northeastern rim of the giant Hellas impact basin [14] and is centered at lat. 22.3°S, long. 110°E in the Mare Tyrrhenum quadrangle (MC-22). A small part of this region in the south is found in the Hellas quadrangle. It has a maximum width of 1,700 km (1,100 mi) [12] and covers an area of about 2 million km2 (770,000 sq mi). [15]

At large scales (>100 m or 330 ft), Hesperia Planum appears smooth and level, [16] having a relatively uniform surface elevation of 1.2 km (0.75 mi) above Mars datum. [17] The plain's surface is 200–800 m (660–2,620 ft) lower in elevation than the surrounding uplands of Tyrrhena Terra and Terra Cimmeria and is slightly tilted to the south, with a mean regional slope of about 0.03°. [14] In high-resolution images (<19 m or 62 ft/pixel), the surface of Hesperia Planum is dominated by dust and fine-grained deposits. Few boulders or bedrock outcrops are visible. Abundant, shallow craters filled with smooth, flat-lying deposits are common. No vents or volcanic constructs are identifiable, although small (<10s meters wide) channels are present. [18]

Geology

Hesperia Planum is generally interpreted to be composed of flood lavas, [19] although layered volcaniclastic or lacustrine (lake-bed) sediments cannot be ruled out. [18] The lavas appear to partly fill a large, irregular topographic depression that existed in Noachian times. The rims of pre-existing impact craters are still visible in places, indicating that the lava deposits are 250–500 m in thickness. The volume of lavas within Hesperia Planum is comparable to that found in large igneous provinces on Earth, such as the Columbia River Basalt Group. [14]

Impact cratering and age

Viking orbiter view of wrinkle ridges in Hesperia Planum. North is at upper left. Image is about 107 km (66 mi) across. Viking 418S39 Hesperia.jpg
Viking orbiter view of wrinkle ridges in Hesperia Planum. North is at upper left. Image is about 107 km (66 mi) across.

The moderate amount of cratering on Hesperia Planum indicates that the plain has an intermediate age in Martian history. In planetary geology, the number density of impact craters is a measure of the relative age of a planetary surface. Heavily cratered surfaces are old, and sparsely cratered surfaces are young. Hesperia Planum is the type locality for the Hesperian System and time period. The lavas making up Hesperia Planum define the base of the Hesperian System. [21] They erupted at the beginning of the Hesperian Period around 3700 million years ago. [22] (Mars itself, along with the other planets, formed about 4500 million years ago.) Hesperian lavas are younger than the rocks in the heavily cratered Noachian terrains but older than rocks formed during the more recent Amazonian Period. (See Geology of Mars.)

Wrinkle ridges

Wrinkle ridges are long, linear topographic highs with a distinctive morphology that consists of a low, broad arch topped by a narrow crenulated ridge (pictured left). They are common features on the Moon where they occur exclusively within lava flow plains (the lunar maria). [23] Their occurrence on Mars is thought to reflect a similar volcanic association. Thus, areas on Mars with abundant wrinkle ridges are interpreted as plains formed by very fluid basaltic lava (flood basalts). The ridges themselves are believed to be the surface expression of thrust faults formed after the lava flows were emplaced. [24] [25] They are not volcanic features, but secondary, tectonic structures that form in dense, competent rocks (such as layered basalts) that have undergone compressional stress. Hesperian-aged "ridged plains" like Hesperia Planum cover about 30% of the Martian surface. [19]

Tyrrhenus Mons

THEMIS daytime IR mosaic image of Tyrrhenus Mons. This ancient, eroded volcano was nicknamed the Dandelion when first seen in Mariner 9 images. Tyrrhena Mons.jpg
THEMIS daytime IR mosaic image of Tyrrhenus Mons. This ancient, eroded volcano was nicknamed the Dandelion when first seen in Mariner 9 images.

Tyrrhenus Mons (Tyrrhena Patera) is an eroded, low-lying volcano in the western part of Hesperia Planum. It is one of the oldest large central-vent volcanoes on the planet [27] and a member of a class of volcanoes called highland paterae, which erupted mainly in the Late Noachian and Early Hesperian. [28] Tyrrhenus Mons stands only 1.5 km above the surrounding plains. At its center lies a 40 km diameter depression, or caldera, from which radiate numerous flat-floored valleys and ridges that suggest the volcano has been highly eroded. The low relief of Tyrrhenus Mons combined with its degraded state indicate the volcano consists largely of friable and easily eroded material such as volcanic ash. The ash was likely derived from the interaction of magma with groundwater or ice. [29]

Dunes

Interactive Mars map

Interactive image map of the global topography of Mars. Hover your mouse over the image to see the names of over 60 prominent geographic features, and click to link to them. Coloring of the base map indicates relative elevations, based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor. Whites and browns indicate the highest elevations (+12 to +8 km); followed by pinks and reds (+8 to +3 km); yellow is 0 km; greens and blues are lower elevations (down to -8 km). Axes are latitude and longitude; Polar regions are noted. (See also: Mars Rovers map and Mars Memorial map) (view * discuss) Mars Map.JPGCydonia MensaeGale craterHolden craterJezero craterLomonosov craterLyot craterMalea PlanumMaraldi craterMareotis TempeMie craterMilankovič craterSisyphi Planum
Interactive icon.svg Interactive image map of the global topography of Mars. Hover your mouse over the image to see the names of over 60 prominent geographic features, and click to link to them. Coloring of the base map indicates relative elevations, based on data from the Mars Orbiter Laser Altimeter on NASA's Mars Global Surveyor . Whites and browns indicate the highest elevations (+12 to +8 km); followed by pinks and reds (+8 to +3 km); yellow is 0 km; greens and blues are lower elevations (down to −8 km). Axes are latitude and longitude; Polar regions are noted.

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<span class="mw-page-title-main">Icaria Planum</span> Planum on Mars

Icaria Planum is a region on Mars in the Thaumasia quadrangle. It is located roughly south-southwest of the Tharsis Rise. Icaria Planum is named after the island of Ikaria, where, according to Greek mythology, Icarus fell and died in the sea.

Linear ridge networks are found in various places on Mars in and around craters. These features have also been called "polygonal ridge networks", "boxwork ridges", and "reticulate ridges". Ridges often appear as mostly straight segments that intersect in a lattice-like manner. They are hundreds of meters long, tens of meters high, and several meters wide. It is thought that impacts created fractures in the surface, these fractures later acted as channels for fluids. Fluids cemented the structures. With the passage of time, surrounding material was eroded away, thereby leaving hard ridges behind. It is reasonable to think that on Mars impacts broke the ground with cracks since faults are often formed in impact craters on Earth. One could guess that these ridge networks were dikes, but dikes would go more or less in the same direction, as compared to these ridges that have a large variety of orientations. Since the ridges occur in locations with clay, these formations could serve as a marker for clay which requires water for its formation. Water here could have supported past life in these locations. Clay may also preserve fossils or other traces of past life.

<span class="mw-page-title-main">Thaumasia Planum</span> Planum on Mars

The Thaumasia Planum of Mars lies south of Melas Chasmata and Coprates Chasmata. It is in the Coprates quadrangle. Its center is located at 21.66 S and 294.78 E. It was named after a classical albedo feature. The name was approved in 2006. Some forms on its surface are evidence of a flow of lava or water the Melas Chasma. Many wrinkle ridges and grabens are visible. One set of grabens, called Nia Fossae, seem to follow the curve of Melas Chasmata which lies just to the north. Some researchers have discovered dikes in this region. For the study, Thermal Emission Imaging System (THEMIS) daytime infrared images, THEMIS nighttime infrared images, CTX images, and HiRISE images were used. These dikes contain magnesium-rich olivine which indicates a primitive magma composition. Dikes occur when magma follows cracks and faults under the ground. Sometimes erosion reveals them. The presence of pit craters, narrow grabens, linear troughs, and ovoid troughs are also evidence of dikes. These dikes that lie close to and parallel to Valles Marineris, the great canyon system, are evidence that extensional stress aided the formation of Valles Marineris. They may be part of a system of dikes that came from the same magma source that fed the whole area. That source may have been a “plume” of molted rock that rose from the Martian mantle.

The Thaumasia Plateau is a vast sloping volcanic plain in the western hemisphere of Mars, and is the most extensive component of the Tharsis Rise by area. Syria Planum, Solis Planum, Sinai Planum, and Thaumasia Planum are the constituent sectors of the plateau, which sits between 8 km and 4 km above the surrounding southern highlands. It is bounded by vestigial basement terrains that predate the formation of Tharsis. This area has been proposed to be a drainage basin that sourced the floodwaters forming the outflow channels surrounding Chryse Planitia.

References

  1. 1 2 "Hesperia Planum". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program. (Center Latitude: -21.42°, Center Longitude: 109.89°)
  2. ↑ Scott, D.H.; Carr, M.H. (1978). Geologic Map of Mars. U.S. Geological Survey Miscellaneous Investigations Series Map I-1083.
  3. ↑ Morton, 2002, p. 117.
  4. ↑ Hartmann, 2003, p. 12.
  5. 1 2 "Hesperia". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  6. ↑ Simpson, D.P. (1968). Cassell's New Latin Dictionary; Funk & Wagnalls: New York, p. 275.
  7. ↑ USGS Gazetteer of Planetary Nomenclature. http://planetarynames.wr.usgs.gov/DescriptorTerms.
  8. ↑ Hartmann, 2003, p. 199.
  9. ↑ Sheehan, 1996, p. 223.
  10. ↑ Moore, P. (1954). The Planet Mars in Realities of Space Travel: Selected Papers of the British Interplanetary Society, L.J. Carter, Ed.; McGraw-Hill: New York, p. 320.
  11. ↑ Sagan, C. et al. (1972). Variable Features on Mars: Preliminary Mariner 9 Television Results. Icarus,17, 346–372.
  12. 1 2 "Hesperia Planum". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  13. ↑ "Terra, terrae". USGS Gazetteer of Planetary Nomenclature.
  14. 1 2 3 Ivanov, M. A.; Korteniemi, J.; Kostama, V.-P.; Aittola, M.; Raitala, J.; Glamoclija, M.; Marinangeli, L.; Neukum, G. (2005), "Major Episodes of the Hydrologic History in the Region of Hesperia Planum", Mars. J. Geophys. Res.,110, E12S21, doi : 10.1029/2005JE002420.
  15. ↑ Gregg, T. K. P.; Crown, D. A. (2005). What is Hesperia Planum, Mars? An Examination of Multiple Working Hypotheses. (PDF) 36th Lunar and Planetary Science Conference, Abstract #1962.
  16. ↑ Greeley, R. (1994). Planetary Landscapes, 2nd ed.; Chapman & Hall: New York, p. 162. ISBN   0-412-05181-8.
  17. ↑ Kostama, V.-P.; Ivanov, M. A.; Korteniemi, J.; Aittola, M.; Raitala, J.; Glamoclija, M.; Marinangeli, L.; Neukum, G.; and the HRSC Co-Investigator Team. (2005). Major Episodes of the Hydrologic History of Hesperia Planum, Mars. (PDF) 36th Lunar and Planetary Science Conference, Abstract #1659.
  18. 1 2 Gregg, T. K. P.; de Silva, S. (2009). Tyrrhena Patera and Hesperia Planum, Mars: New Insights (and Old Interpretations) from High-Resolution Imagery. 40th Lunar and Planetary Science Conference, Abstract #1700. http://www.lpi.usra.edu/meetings/lpsc2009/pdf/1700.pdf.
  19. 1 2 Greeley, R.; Spudis, P. (1981). Volcanism on Mars. Rev. Geophys. Space Phys., 19(1), 13–41.
  20. ↑ Boyce, 2008, p. 89.
  21. ↑ Tanaka, K.L. (1986). The Stratigraphy of Mars. J. Geophys. Res., Seventeenth Lunar and Planetary Science Conference Part 1, 91(B13), E139–E158.
  22. ↑ Werner, S.C. (2009). The Global Martian Volcanic Evolutionary History. Icarus,201, 44–68.
  23. ↑ Carr, 2006, p. 89.
  24. ↑ Golombek, M.P.; Anderson, F.S.; Zuber, M.T. (2001). Martian Wrinkle Ridge Topography: Evidence for Subsurface Faults from MOLA. J. Geophys. Res.,106(El0), 23,811–23,821.
  25. ↑ Montési, L. G. J.; Zuber, M.T. (2003). Clues to the Lithospheric Structure of Mars from Wrinkle Ridge Sets and Localization Instability. J. Geophys. Res.,108(E6), 5048, doi : 10.1029/2002JE001974.
  26. ↑ Morton, 2002, p. 103.
  27. ↑ Greeley, R.; Crown, D.A. (1990). Volcanic Geology of Tyrrhena Patera, Mars. J. Geophys. Res.,95(B5), 7133–7149.
  28. ↑ Crown, D. A.; Berman, D. C.; Gregg, T. K. P. (2007). Geologic Diversity and Chronology of Hesperia Planum, Mars. 38th Lunar and Planetary Science Conference, Abstract #1169. http://www.lpi.usra.edu/meetings/lpsc2007/pdf/1169.pdf.
  29. ↑ Carr, 2006, pp. 69, 74, Fig. 3.33.
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