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The Margaritifer Sinus quadrangle is one of a series of 30 quadrangle maps of Mars used by the United States Geological Survey (USGS) Astrogeology Research Program. The Margaritifer Sinus quadrangle is also referred to as MC-19 (Mars Chart-19).[1]
The Margaritifer Sinus quadrangle covers the area from 0° to 45° west longitude and 0° to 30° south latitude on Mars. This quadrangle shows many signs of past water with evidence of lakes, deltas, ancient rivers, inverted channels, and chaos regions that released water.[2] Margaritifer Sinus contains some of the longest lake-chain systems on Mars, perhaps because of a wetter climate, more groundwater, or some of each factor. The Samara/Himera lake-chain system is about 1800 km long; the Parara/Loire valley network and lake-chain system is about 1100 km long.[3] A low area between Parana Valles and Loire Vallis is believed to have once held a lake.[4][5] The 154 km diameter Holden Crater also once held a lake.[6] Near Holden Crater is a graben, called Erythraea Fossa, that once held a chain of three lakes.[7]
This region of Mars is famous because the Opportunity Rover landed there on January 25, 2004 at 1.94°S and 354.47°E (5.53° W).
Map of Margaritifer Sinus quadrangle with major features labeled.
Opportunity Rover as seen by HiRISE on January 29, 2009. Opportunity is on its way to Endeavour Crater, 17 km away at this point (2.1° S and 354.5° E).
Location of Opportunity Rover on surface of Mars.
Mars Global Surveyor orbiter's photograph of landing site showing "hole in one."
Opportunity Rover found that the soil at Meridiani Planum was very similar to the soil at Gusev crater and Ares Vallis; however in many places at Meridiani the soil was covered with round, hard, gray spherules that were named "blueberries."[8] These blueberries were found to be composed almost entirely of the mineral hematite. It was decided that the spectra signal spotted from orbit by Mars Odyssey was produced by these spherules. After further study it was decided that the blueberries were concretions formed in the ground by water.[9] Over time, these concretions weathered from what was overlying rock, and then became concentrated on the surface as a lag deposit. The concentration of spherules in bedrock could have produced the observed blueberry covering from the weathering of as little as one meter of rock.[10][11] Most of the soil consisted of olivine basalt sands that did not come from the local rocks. The sand may have been transported from somewhere else.[12]
Drawing showing how "blueberries" came to cover much of surface in Meridiani Planum.
A Mössbauer spectrum was made of the dust that gathered on Opportunity’s capture magnet. The results suggested that the magnetic component of the dust was titanomagnetite, rather than just plain magnetite, as was once thought. A small amount of olivine was also detected which was interpreted as indicating a long arid period on the planet. On the other hand, a small amount of hematite that was present meant that there may have been liquid water for a short time in the early history of the planet.[13] Because the Rock Abrasion Tool (RAT) found it easy to grind into the bedrocks, it is thought that the rocks are much softer than the rocks at Gusev crater.
Few rocks were visible on the surface where Opportunity landed, but bedrock that was exposed in craters was examined by the suit of instruments on the Rover.[14] Bedrock rocks were found to be sedimentary rocks with a high concentration of sulfur in the form of calcium and magnesium sulfates. Some of the sulfates that may be present in bedrocks are kieserite, sulfate anhydrate, bassanite, hexahydrite, epsomite, and gypsum. Salts, such as halite, bischofite, antarcticite, bloedite, vanthoffite, or gluberite may also be present.[15][16]
The rocks contained the sulfates had a light tone compared to isolated rocks and rocks examined by landers/rovers at other locations on Mars. The spectra of these light toned rocks, containing hydrated sulfates, were similar to spectra taken by the Thermal Emission Spectrometer on board the Mars Global Surveyor. The same spectrum is found over a large area, so it is believed that water once appeared over a wide region, not just in the area explored by Opportunity Rover.[17]
The Alpha Particle X-ray Spectrometer (APXS) found rather high levels of phosphorus in the rocks. Similar high levels were found by other rovers at Ares Vallis and Gusev Crater, so it has been hypothesized that the mantle of Mars may be phosphorus-rich.[18] The minerals in the rocks could have originated by acid weathering of basalt. Because the solubility of phosphorus is related to the solubility of uranium, thorium, and rare earth elements, they are all also expected to be enriched in rocks.[19]
When Opportunity Rover traveled to the rim of Endeavour crater, it soon found a white vein that was later identified as being pure gypsum.[20][21] It was formed when water carrying gypsum in solution deposited the mineral in a crack in the rock. A picture of this vein, called "Homestake" formation, is shown below.
Examination of Meridiani rocks found strong evidence for past water. The mineral called jarosite which only forms in water was found in all bedrocks. This discovery proved that water once existed in Meridiani Planum[22] In addition, some rocks showed small laminations (layers) with shapes that are only made by gently flowing water.[23] The first such laminations were found in a rock called "The Dells." Geologists would say that the cross-stratification showed festoon geometry from transport in subaqueous ripples.[16] A picture of cross-stratification, also called cross-bedding, is shown on the left.
Box-shaped holes in some rocks were caused by sulfates forming large crystals, and then when the crystals later dissolved, holes, called vugs, were left behind.[23] The concentration of the element bromine in rocks was highly variable probably because it is very soluble. Water may have concentrated it in places before it evaporated. Another mechanism for concentrating highly-soluble bromine compounds is frost deposition at night that would form very thin films of water that would concentrate bromine in certain spots.[8]
One rock, "Bounce Rock," found sitting on the sandy plains was found to be ejecta from an impact crater. Its chemistry was different than the bedrocks. Containing mostly pyroxene and plagioclase and no olivine, it closely resembled a part, Lithology B, of the shergottite meteorite EETA 79001, a meteorite known to have come from Mars. Bounce rock received its name by being near an airbag bounce mark.[10]
Opportunity Rover found meteorites just sitting on the plains. The first one analyzed with Opportunity’s instruments was called "Heatshield Rock," as it was found near where Opportunity’s headshield landed. Examination with the Miniature Thermal Emission Spectrometer (Mini-TES), Mossbauer spectrometer, and APXS lead researchers to, classify it as an IAB meteorite. The APXS determined it was composed of 93% iron and 7% nickel. The cobble named "Fig Tree Barberton" is thought to be a stony or stony-iron meteorite (mesosiderite silicate),[24][25] while "Allan Hills," and "Zhong Shan" may be iron meteorites.
Heat Shield Rock was the first meteorite ever identified on another planet.
Heat shield, with Heat Shield Rock just above and to the left in the background.
Observations at the site have led scientists to believe that the area was flooded with water a number of times and was subjected to evaporation and desiccation.[10] In the process sulfates were deposited. After sulfates cemented the sediments, hematite concretions grew by precipitation from groundwater. Some sulfates formed into large crystals which later dissolved to leave vugs. Several lines of evidence point toward an arid climate in the past billion years or so, but a climate supporting water, at least for a time, in the distant past.[26]
Vallis (plural valles) is the Latin word for valley. It is used in planetary geology for the naming of valley landform features on other planets.
Vallis was used for old river valleys that were discovered on Mars, when probes were first sent to Mars. The Viking Orbiters caused a revolution in our ideas about water on Mars; huge river valleys were found in many areas. Space craft cameras showed that floods of water broke through dams, carved deep valleys, eroded grooves into bedrock, and traveled thousands of kilometers.[27][28][29]
Parana Valles, as seen by HiRISE. Scale bar is 1000 meters long.
Ladon Valles, as seen by HiRISE. Click on image to see dark and light-toned layers.
Ravi Vallis, as seen by Viking Orbiter. Ravi Vallis was probably formed when catastrophic floods came out of the ground to the right (chaotic terrain). Image located in Margaritifer Sinus quadrangle.
Tear-drop shaped islands caused by flood waters from Maja Vallis, as seen by Viking Orbiter. Image is located in Oxia Palus quadrangle.
The long channel Nirgal Vallis is showed where it connects to Uzboi Vallis. The crater Luki is 21 km in diameter. Picture taken by THEMIS.
Nirgal Vallis, as seen by THEMIS.
Nirgal Vallis Close-up, as seen by THEMIS
The Viking Orbiters discovered much about water on Mars. Branched streams, studied by the Orbiters in the southern hemisphere, suggested that rain once fell.[27][28][29]
The branched channels seen by Viking from orbit strongly suggested that it rained on Mars in the past. Image is located in Margaritifer Sinus quadrangle
Aureum Chaos is a major canyon system and collapsed area. It is probably a major source of water for large outflow channels.
Large outflow channels on Mars are believed to be caused by catastrophic discharges of ground water. Many of the channels begin in chaotic terrain, where the ground has apparently collapsed. In the collapsed section, blocks of undisturbed material be seen. The OMEGA experiment on Mars Express discovered clay minerals (phyllosilicates) in a variety of places in Aureum Chaos. Clay minerals need water to form, so the area may once have contained large amounts of water.[30] Scientists are interested in determining what parts of Mars contained water because evidence of past or present life may be found there.
Huge canyons in Aureum Chaos. Gullies are rare at this latitude. Picture taken by THEMIS.
On April 1, 2010, NASA released the first images under the HiWish program, with the public suggesting places for HiRISE to photograph. One of the eight locations was Aureum Chaos.[31] The first image below gives a wide view of the area. The next two images are from the HiRISE image.[32]
THEMIS image of wide view of following HiRISE images. Black box shows approximate location of HiRISE images. This image is just a part of the vast area known as Aureum Chaos. Click on image to see more details.
Aureum Chaos, as seen by HiRISE, under the HiWish program.
Close up view of previous image, as seen by HiRISE under HiWish program. Small round dots are boulders.
Several sites in the Margaritifer Sinus quadrangle have been proposed as areas to send NASA's next major Mars rover, the Mars Science Laboratory. Both Holden Crater and Eberswalde Crater made the cut to be among the top four.[33] Miyamoto Crater was in the top 7 sites chosen. Holden Crater is believed to have once been a lake. Actually, it is now believed that it held two lakes.[34] The first was longer lived and was formed from drainage within the crater and precipitation. The last lake began when water damed up in Uzboi Vallis broke through a divide, then rapidly drained into Holden Crater. Because there are rocks meters in diameter on the crater floor, it is thought it was a powerful flood when water flowed into the crater.[6]
West Rim of Holden Crater, as seen by THEMIS. Click on image to see more details.
Close-up of Channels on Rim of Holden Crater, as seen by THEMIS. Click on image to see more details.
Eberswalde Crater contains a delta.[35] There is a great deal of evidence that Miyamoto Crater once contained rivers and lakes. Many minerals, such as clays, chlorides, sulfates, and iron oxides, have been discovered there.[36] These minerals are often formed in water. A picture below shows an inverted channel in Miyamoto Crater. Inverted channels formed from accumulated sediments that were cemented by minerals. These channels eroded into the surface, then the whole area was covered over with sediments. When the sediments were later eroded away, the place where the river channel existed remained because the hardened material that was deposited in the channel was resistant to erosion.[37] Iani Chaos, pictured below, was among the top 33 landing sites. Deposits of hematite and gypsum have been found there.[38] Those minerals are usually formed in connection with water.
Iani Chaos, as seen by THEMIS. Sand from eroding mesas is covering brighter floor material. Click on image to see relationship of Iani Chaos to other local features.
Landing zone in Iani Chaos, as seen by THEMIS.
The aim of the Mars Science Laboratory is to search for signs of ancient life. It is hoped that a later mission could then return samples from sites that the Mars Science Laboratory identified as probably containing remains of life. To safely bring the craft down, a 12 mile wide, smooth, flat circle is needed. Geologists hope to examine places where water once ponded.[38] They would like to examine sediment layers.
Some places on Mars show inverted relief. In these locations, a stream bed may be a raised feature, instead of a valley. The inverted former stream channels may be caused by the deposition of large rocks or due to cementation. In either case erosion would erode the surrounding land and leave the old channel as a raised ridge because the ridege will be more resistant to erosion. An image below, taken with HiRISE of Miyamoto Crater shows a ridge that is an old channel that has become inverted.[39]
Inverted Channel in Miyamoto Crater, as seen by HiRISE. The scale bar is 500 meters long.
CTX context image for next image that was taken with HiRISE. Note long ridge going across image is probably an old stream. Box indicates area for HiRISE image.
Example of inverted terrain in Parana Valles region, as seen by HiRISE under the HiWish program.
Researchers have found a number of examples of deltas that formed in Martian lakes. Finding deltas is a major sign that Mars once had a lot of water. Deltas often require deep water over a long period of time to form. Also, the water level needs to be stable to keep sediment from washing away. Deltas have been found over a wide geographical range. Below, are pictures of a few.[40]
Delta in Margaritifer Sinus quadrangle as seen by THEMIS.
Probable delta in Eberswalde Crater that lies to the NE of Holden Crater, as seen by Mars Global Surveyor. Image in Margaritifer Sinus quadrangle.
Impact craters generally have a rim with ejecta around them, in contrast volcanic craters usually do not have a rim or ejecta deposits. As craters get larger (greater than 10 km in diameter) they usually have a central peak.[41] The peak is caused by a rebound of the crater floor following the impact.[27] Sometimes craters will display layers. Craters can show us what lies deep under the surface.
In December 2011, Opportunity Rover discovered a vein of gypsum sticking out of the soil along the rim of
Bedrock in Luki Crater, enhanced HiRISE color image. The central region of the crater consists of uplifted ancient bedrock with a variety of rock types, indicated by the range of colors. Image is about 1 km. wide.
Butte in Arsinoes Chaos with some light-toned layers, as seen by HiRISE under HiWish program.
Layered butte, as seen by HiRISE under HiWish program.
Beer Crater eroded west wall, as seen by CTX.
Alga Crater, as seen by HiRISE. Click on image to see the relationship between Alga Crater and the larger Chekalin Crater.
Timbuktu Crater, located on the edge of Capri Chasma. Image taken with THEMIS.
[42]
Solar System, Mars Reconnaissance Orbiter, Oxygen, Mercury (planet), Moon
Mars, Mars Reconnaissance Orbiter, Gale (crater), Mars Pathfinder, Viking program
Mars, Mars Science Laboratory, Mars Reconnaissance Orbiter, Themis, Mare Boreum quadrangle
Mars, Diacria quadrangle, Arcadia quadrangle, Mare Acidalium quadrangle, Ismenius Lacus quadrangle
Mars, Mars Reconnaissance Orbiter, Mare Boreum quadrangle, Arcadia quadrangle, Mare Acidalium quadrangle
Mars, Phoenicis Lacus quadrangle, Margaritifer Sinus quadrangle, Mare Boreum quadrangle, Diacria quadrangle
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Mars, Mare Boreum quadrangle, Diacria quadrangle, Arcadia quadrangle, Mare Acidalium quadrangle
Mars, Digital object identifier, Mare Boreum quadrangle, Diacria quadrangle, Arcadia quadrangle