Cebrenia quadrangle

Image of the Cebrenia Quadrangle (MC-7). The northwest contains relatively smooth plains; the southeast contains Hecates Tholus (one of three Elysium shield volcanoes) and Phlegra Montes (a ridge system).

The Cebrenia quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The quadrangle is located in the northeastern portion of Mars’ eastern hemisphere and covers 120° to 180° east longitude (180° to 240° west longitude) and 30° to 65° north latitude. The quadrangle uses a Lambert conformal conic projection at a nominal scale of 1:5,000,000 (1:5M). The Cebrenia quadrangle is also referred to as MC-7 (Mars Chart-7).^[1] It includes part of Utopia Planitia and Arcadia Planitia. The southern and northern borders of the Cebrenia quadrangle are approximately 3,065 km (1,905 mi) and 1,500 km (930 mi) wide, respectively. The north to south distance is about 2,050 km (1,270 mi) (slightly less than the length of Greenland).^[2] The quadrangle covers an approximate area of 4.9 million square km, or a little over 3% of Mars’ surface area.^[3]

Origin of name

Cebrenia is a telescopic albedo feature centered on 50° N and 150° E on Mars. The feature is named after Cebrenia, a country near ancient Troy. The name was approved by the International Astronomical Union (IAU) in 1958.^[4]

Physiography and geology

The quadrangle's prominent features are the large craters Mie and Stokes, a volcano, Hecates Tholus, and a group of mountains, Phlegra Montes. This area is a flat, smooth plain for the most part, so the relatively large craters Mie and Stokes really stand out. The Galaxias Region has an area of chaos, where the ground seems to have collapsed.

Viking II (part of Viking program) landed near Mie on September 3, 1976. Its landing coordinates were 48° N and 226° W.^[5]

Results from Viking II mission

What it would look like walking around the landing site

The sky would be a light pink. The dirt would also appear pink. The surface would be uneven; the soil would be formed into troughs. Large rocks would be spread about. Most of the rocks are similar in size. Many of the rocks would have small holes or bubbles on their surfaces caused by gas escaping after the rocks came to the surface. Some boulders would show erosion due to the wind. Many rocks would appear to be perched, as if wind removed much of the soil at their bases.^[6][7] In the winter snow or frost would cover most of the ground. There would be many small sand dunes that are still active. The wind speed would typically be 7 meters per second (16 miles per hour). There would be a hard crust on the top of the soil similar to a deposit, called caliche which is common in the U.S. Southwest. Such crusts are formed by solutions of minerals moving up through soil and evaporating at the surface.^[8] Scientists, in a September, 2009 article in the journal Science, have asserted that if Viking II only dug four (4) inches deeper, it would have reached a layer of almost pure ice.^[9][10][11]

Analysis of soil

Image from Mars taken by Viking 2

The soil resembled those produced from the weathering of basaltic lavas. The tested soil contained abundant silicon and iron, along with significant amounts of magnesium, aluminum, sulfur, calcium, and titanium. Trace elements, strontium and yttrium, were detected. The amount of potassium was 5 times lower than the average for the Earth's crust. Some chemicals in the soil contained sulfur and chlorine that were like typical compounds remaining after the evaporation of sea water. Sulfur was more concentrated in the crust on top of the soil then in the bulk soil beneath. The sulfur may be present as sulfates of sodium, magnesium, calcium, or iron. A sulfide of iron is also possible.^[12] The Spirit Rover and the Opportunity Rover both found sulfates on Mars.^[13] The Opportunity Rover (landed in 2004 with advanced instruments) found magnesium sulfate and calcium sulfate at Meridiani Planum.^[14] Using results from the chemical measurements, mineral models suggest that the soil could be a mixture of about 90% iron-rich clay, about 10% magnesium sulfate (kieserite?), about 5% carbonate (calcite), and about 5% iron oxides (hematite, magnetite, goethite?). These minerals are typical weathering products of mafic igneous rocks.^[15][16][17] Studies with magnets aboard the landers indicated that the soil is between 3 and 7 percent magnetic materials by weight. The magnetic chemicals could be magnetite and maghemite. These could come from the weathering of basalt rock.^[18][19] Experiments carried out by the Mars Spirit Rover (landed in 2004) indicated that magnetite could explain the magnetic nature of the dust and soil on Mars. Magnetite was found in the soil and that the most magnetic part of the soil was dark. Magnetite is very dark.^[20]

Search for life

Viking did three experiments to look for life. The results were surprising and interesting. Most scientists now believe that the data were due to inorganic chemical reactions of the soil, although a few scientists still believe the results were due to living reactions. No organic chemicals were found in the soil. However, dry areas of Antarctica do not have detectable organic compounds either, but they have organisms living in the rocks.^[21] Mars has almost no ozone layer, like the Earth, so UV light sterilizes the surface and produces highly reactive chemicals such as peroxides that would oxidize any organic chemicals.^[7] The Phoenix Lander discovered the chemical perchlorate in the Martian Soil. Perchlorate is a strong oxidant so it may have destroyed any organic matter on the surface.^[22] If it is widespread on Mars, carbon-based life would be difficult at the soil surface.

Bright part is water ice that has been exposed by impact. The ice was identified using CRISM on the MRO.

Research, published in the Journal of Geophysical Research in September 2010, proposed that organic compounds were actually present in the soil analyzed by both Viking 1 and 2. NASA's Phoenix lander in 2008 detected perchlorate which can break down organic compounds. The study's authors found that perchlorate will destroy organics when heated and will produce chloromethane and dichloromethane, the identical chlorine compounds discovered by both Viking landers when they performed the same tests on Mars. Because perchlorate would have broken down any Martian organics, the question of whether or not Viking found life is still wide open.^[23]

Ice exposed in new craters

Impressive research, reported in the journal Science in September 2009,^[24] has showed that some new craters on Mars show exposed, pure, water ice. After a time, the ice disappears, evaporating into the atmosphere. The ice is only a few feet deep. The ice was confirmed with the Compact Imaging Spectrometer (CRISM)] on board the Mars Reconnaissance Orbiter (MRO). The ice was found in a total of 5 locations. Three of the locations are in the Cebrenia quadrangle. These locations are 55°34′N 150°37′E / 55.57°N 150.62°E / 55.57; 150.62, 43°17′N 176°54′E / 43.28°N 176.9°E / 43.28; 176.9 and 45°00′N 164°30′E / 45°N 164.5°E / 45; 164.5.^[9][10][11] This discovery proves that future colonists on Mars will be able to obtain water from a wide variety of locations. The ice can be dug up, melted, then taken apart to provide fresh oxygen and hydrogen for rocket fuel. Hydrogen is the powerful fuel used by the space shuttle main engines

Other craters

Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits.^[25] Sometimes craters will display layers. Since the collision that produces a crater is like a powerful explosion, rocks from deep underground are tossed onto the surface. Hence, craters can show us what lies deep under the surface.

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  Kufra Crater Floor, as seen by HiRISE Pits are thought to be caused by escaping water.
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  Fenagh Crater Ejecta, as seen by HiRISE.
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  Chincoteague Crater, as seen by HiRISE.
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  Close-up of Chincoteague Crater, as seen by HiRISE.
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  Group of secondary craters, as seen by HiRISE under HiWish program.
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  Layers in wall of crater, as seen by HiRISE under HiWish program.
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  Mie Crater, as seen by CTX camera (on Mars Reconnaissance Orbiter). Viking II landed near Mie Crater in 1976.
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  Western side of Adams Crater (Martian Crater), as seen by CTX camera (on Mars Reconnaissance Orbiter).
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  Western side of Tyndall (Martian crater), as seen by CTX camera (on Mars Reconnaissance Orbiter).

Hecates Tholus

Recent research leads scientists to believe that Hecates Tholus erupted explosively about 350 million years ago, which is a not that long ago for Mars. The eruptions created depressions on the flanks of the volcano. And just five million years ago, glacial deposits formed inside these depressions.^[26] Some valleys on Hecates show a parallel drainage pattern.^[25]

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  Hecates Tholus, as seen by Mars Global Surveyor.
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  Hecates Tholus topography.
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  Hecates Tholus Ridges, as seen by HiRISE. Ridges are to the west-northwest of Hecates Tholus. The deepest ridge was measured to be about 50 meters high.^[27]
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  Buvinda Vallis, as seen by THEMIS. Buvinda Vallis is associated with Hecates Tholus; it lies just east of Hecates Tholus.
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  Lava channels on flank of Hecates Tholus, as seen by HiRISE under HiWish program. A crater has been partially covered over by lava flows. This crater will be enlarged in the next image.
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  Enlarged view of lava filling a crater, as seen by HiRISE under HiWish program.
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  Crater on edge of lava flow on Hecates Tholus, as seen by HiRISE under HiWish program. Lava seems to have formed tail shape on the lee side of obstacles like crater rims.

Volcano-ice interactions

Large amounts of water ice are believed to be present under the surface of Mars. Some channels lie near volcanic areas. When hot subsurface molten rock comes close to this ice, large amounts of liquid water and mud may be formed. Hrad Vallis in the Cebrenia quadrangle is close to Elysium Mons, a large volcano, which may have supplied water to create the channel. Hrad Vallis is pictured below.^[28]

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  Hrad Vallis may have been formed when the large Elysium Mons volcanic complex melted ground ice, as seen by THEMIS.
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  Streamlined islands in Hrad Vallis, as seen by HiRISE.

Galaxias region

The ground in Galaxias seems to have collapsed. Such land forms on Mars are called "Chaos terrain." Galaxias Chaos is different from many other chaotic regions. It does not have associated outflow channels, and it does not display a great elevation difference between it and the surrounding land area, as most of the other chaos regions. Research by Pedersen and Head, published in 2010, suggests that Galaxias Chaos is the site of a volcanic flow that buried an ice-rich layer, called the Vastitas Borealis Formation (VBF). It is generally believed that the VBF is a residue from water-rich materials deposited by large floods.^[29][30] The VBF may have been of varied thickness and may have contained varied amounts of ice. In the thin atmosphere of Mars, this layer would have slowly disappeared by sublimation (changing from a solid directly to a gas). Since some areas would have sublimated more than others, the upper lava cap would not be supported evenly and would crack. Cracks/troughs may have begun from sublimation and shrinkage along the edges of the lava cap. Stress from the undermining of the cap edge would have made cracks in the cap. Places with cracks would undergo more sublimation, then the cracks would widen and form the blocky terrain characteristic of regions of chaos. The sublimation process may have been aided by heat (geothermal flux) from magma movements. There are volcanoes, namely Elysium Montes and Hecates Tholus, nearby which most likely are surrounded by dikes, which would have heated the ground. Also, a warmer period in the past would have increased the amount of water sublimating from the ground.^[31]

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  This series of drawings shows a model for the formation of Martian chaos, as proposed by Pedersen and Head 2011^[32] Amount of sublimation is exaggerated to improve understanding. Click on image to see more details.
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  Galaxius Mons, as seen by HiRISE. The black line was a section that was not imaged. There are many more details visible on the original image.
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  Galaxias Fossae Trough, as seen by HiRISE.
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  Galaxias Chaos as seen by CTX. The scene in the next image is a part of this picture.
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  Galaxias Chaos as seen by HiRISE.

Evidence of Glaciers

Glaciers, loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past.^[25][33] Lobate convex features on the surface known as viscous flow features and lobate debris aprons, which show the characteristics of non-Newtonian flow, are now almost unanimously regarded as true glaciers.^{[33][34][35][36][37][38][39][40][41]} However, a variety of other features on the surface have also been interpreted as directly linked to flowing ice, such as fretted terrain,^[33][42] lineated valley fill,^[38][40] concentric crater fill,^[34][43] and arcuate ridges.^[41] A variety of surface textures seen in imagery of the midlatitudes and polar regions are also thought to be linked to sublimation of glacial ice.^[43][44]

,

The pictures below show features that are probably associated with glaciers.

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  Elephant Foot Glacier in the Earth's Arctic, as seen by Landsat 8. This picture shows several glaciers that have the same shape as many features on Mars that are believed to also be glaciers.
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  Material moving down slope in Phlegra Montes, as seen by HiRISE. Movement is probably aided by water/ice.
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  Lobate debris apron in Phlegra Montes, as seen by HiRISE. The debris apron is probably mostly ice with a thin covering of rock debris, so it could be a source of water for future Martian colonists. Scale bar is 500 meters long.
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  Wide view of a cliff and remains of a glacier, as seen by HiRISE under HiWish program.
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  Close-up of a cliff showing possible faults, as seen by HiRISE under HiWish program; note the rock that seems to be split by the fault. Some boulders are sitting in round holes because their ability to gather and hold heat may have melted ground ice.
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  Close-up of grooves left by a glacier, as seen by HiRISE under HiWish program. The presence of grooves suggest that it was a wet-based glacier. Moisture under the glacier may have helped Martian organisms to survive.
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  Close-up of surface, as seen by HiRISE under HiWish program

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  Lineated valley fill, as seen by HiRISE under HiWish program
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  Close view of lineated valley fill and mantle, as seen by HiRISE under HiWish program
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  Flow being constricted, as seen by HiRISE under HiWish program
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  Latitude dependent mantle, as seen by HiRISE under HiWish program

Channels

There is enormous evidence that water once flowed in river valleys on Mars.^{[45] [46]} Images of curved channels have been seen in images from Mars spacecraft dating back to the early seventies with the Mariner 9 orbiter. ^{[47] [48] [49] [50]} Indeed, a study published in June 2017, calculated that the volume of water needed to carve all the channels on Mars was even larger than the proposed ocean that the planet may have had. Water was probably recycled many times from the ocean to rainfall around Mars.^{[51] [52]}

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  Streamlined form along channel, as seen by HiRISE under HiWish program
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  Context for next image of layers along Hrad Vallis, as seen by CTX. Photo labeled with layers, streamlined forms, and arrow indicating direction water flowed.
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  Layers exposed along Hrad Vallis, as seen by HiRISE under HiWish program

Pedestal craters

A pedestal crater is a crater with its ejecta sitting above the surrounding terrain and thereby forming a raised platform (like a pedestal). They form when an impact crater ejects material which forms an erosion-resistant layer, thus causing the immediate area to erode more slowly than the rest of the region. Some pedestals have been accurately measured to be hundreds of meters above the surrounding area. This means that hundreds of meters of material were eroded away. The result is that both the crater and its ejecta blanket stand above the surroundings. Pedestal craters were first observed during the Mariner missions.^{[53][54][55][56]}

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  Pedestal crater, as seen by HiRISE under HiWish program

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  Pedestal crater, as seen by HiRISE under HiWish program
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  Close view of ejecta of pedestal crater, as seen by HiRISE under HiWish program Arrow shows one of example of a boulder sitting in a pit. This image will be enlarged to better show this in the next two images.
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  Closer view of ejecta, as seen by HiRISE under HiWish program Note: Arrows show examples of boulders sitting in pits.
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  Close view of ejecta, as seen by HiRISE under HiWish program Note: Arrows show examples of boulders sitting in pits.

Additional Images in Cebrenia quadrangle

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  Map of Cebrenia. Viking II landed near Mie crater. The volcano Hecates probably has glaciers on its slopes.
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  Apsus Vallis, as seen by THEMIS. Apsus is near the Elysium volcanic system; it may have been partially formed by the action of lava.
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  Hephaestus Fossae Two Views, as seen by HiRISE. Picture on right lies to the top (north) of other picture. Fossa (geology) often form by material moving into an underground void.
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  Close up view of mantle, as seen by HiRISE under the HiWish program. Mantle may be composed of ice and dust that fell from the sky during past climatic conditions.
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  Ridge and surface features near rim of Adams crater, as seen by HiRISE under HiWish program
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  Layered mesa in crater, as seen by HiRISE under HiWish program.
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  Cones, as seen by HiRISE under HiWish program.
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  Crater ejecta, as seen by HiRISE under HiWish program
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  Close view of crater ejecta, as seen by HiRISE under HiWish program Note this is an enlargement of the previous image.

Other Mars quadrangles

0°N 180°W / 0°N 180°W / 0; -180

0°N 0°W / 0°N -0°E / 0; -0

90°N 0°W / 90°N -0°E / 90; -0

MC-01

Mare Boreum

MC-02

Diacria

MC-03

Arcadia

MC-04

Mare Acidalium

MC-05

Ismenius Lacus

MC-06

Casius

MC-07

Cebrenia

MC-08

Amazonis

MC-09

Tharsis

MC-10

Lunae Palus

MC-11

Oxia Palus

MC-12

Arabia

MC-13

Syrtis Major

MC-14

Amenthes

MC-15

Elysium

MC-16

Memnonia

MC-17

Phoenicis

MC-18

Coprates

MC-19

Margaritifer

MC-20

Sabaeus

MC-21

Iapygia

MC-22

Tyrrhenum

MC-23

Aeolis

MC-24

Phaethontis

MC-25

Thaumasia

MC-26

Argyre

MC-27

Noachis

MC-28

Hellas

MC-29

Eridania

MC-30

Mare Australe

The thirty cartographic quadrangles of Mars, defined by the United States Geological Survey.^[57][60] The quadrangles are numbered with the prefix "MC" for "Mars Chart."^[61] Click on a quadrangle name link and you will be taken to the corresponding article. North is at the top; 0°N 180°W / 0°N 180°W / 0; -180 is at the far left on the equator. The map images were taken by the Mars Global Surveyor.

[]

Interactive Mars map

Interactive imagemap of the global topography of Mars. Hover your mouse to see the names of over 25 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. Reds and pinks are higher elevation (+3 km to +8 km); yellow is 0 km; greens and blues are lower elevation (down to −8 km). Whites (>+12 km) and browns (>+8 km) are the highest elevations. Axes are latitude and longitude; Poles are not shown.

(See also: Mars Rovers map) (view • discuss)

See also

References

External links

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