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24-597: Amazonis may refer to: Amazonis Planitia , a plain on Mars Amazonis , lost Latin epic by Domitius Marsus Topics referred to by the same term [REDACTED] This disambiguation page lists articles associated with the title Amazonis . If an internal link led you here, you may wish to change the link to point directly to the intended article. Retrieved from " https://en.wikipedia.org/w/index.php?title=Amazonis&oldid=1171118527 " Category : Disambiguation pages Hidden categories: Short description

48-480: A "bright dusty volcanic desert crossed by many fresh-looking lava flows." Amazonis has become the primary focus of modern research efforts both because of its geological composition and because of its relative youth compared to other Martian regions, which are often hundreds of millions of years older. Hartman writes that the plain closely resembles Iceland's surface, with its "strange cobweb-like networks of ridges and crags [on both planets, divide] smoother areas into

72-431: A core of ice. Shadow measurements from HiRISE indicate the ridges are 4–5 meters high. Medusae Fossae Formation The total area of the formation is equal to 20% the size of the continental United States. It is divided into three subunits (members) that are all considered to be of Amazonian age, the youngest era in martian geological history. The formation straddles the highland - lowland boundary near

96-589: A group headed by Laura Kerber hypothesized that it could have been formed from ash from the volcanoes Apollinaris Mons , Arsia Mons , and possibly Pavonis Mons . An analysis of data from the Mars Odyssey Neutron Spectrometer revealed that the western lobe of the Medusae Fossae Formation contains some water. This means that this formation contains bulk water ice. During periods of high obliquity (tilt) water ice

120-402: A kilometer or so in length. Their height ranges from a meter to greater than 10 meters, while the width of the narrow ones is less than 10 meters. Comparisons of elemental composition suggest that the Medusae Fossae Formation has been a source of Mars' ubiquitous surface dust. In July 2018, researchers reported that it may be the largest single source of dust on the planet. The surface of

144-433: 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. Since the ridges occur in locations with clay, these formations could serve as

168-485: 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. When a fluid moves by a feature like a mound, it will become streamlined. Often flowing water makes the shape and later lava flows spread over the region. In the pictures below this has occurred. Many places on Mars show dark streaks on steep slopes , such as crater walls. It seems that

192-416: A pattern something like fragments of a broken plate." Both land masses' shapes have been formed by lava flows from volcanic eruptions, causing both surfaces to be covered by a thick layer of hardened lava. Findings from aerial footage of both Amazonis and Iceland have shown nearly identical terrain patterns, signifying the comparative ages of the two regions. The entire contemporary era on Mars has been named

216-571: A thin layer of dust is removed, the underlying surface appears dark. Much of the Martian surface is covered with dust. Dust storms are frequent, especially when the spring season begins in the southern hemisphere. At that time, Mars is 40% closer to the Sun. The orbit of Mars is much more elliptical than the Earth's. That is, the difference between the farthest point from the Sun and the closest point to

240-432: Is 1.765 ± 0.105 g/cm , similar to the density of terrestrial ignimbrites . This rules out significant amounts of ice in the bulk composition. In combination with the deposit's high content of sulfur and chlorine, it implies an explosive volcanic origin. The total volume of the deposit is 1.4 × 10 km ; such a large deposit might have been emplaced in periodic eruptions over an interval of 500 million years. In some places,

264-806: Is different from Wikidata All article disambiguation pages All disambiguation pages Amazonis Planitia Amazonis Planitia ( / ə ˈ m æ z ə n ɪ s p l ə ˈ n ɪ ʃ i ə / , Latin Amāzŏnis ) is one of the smoothest plains on Mars . It is located between the Tharsis and Elysium volcanic provinces, to the west of Olympus Mons , in the Amazonis and Memnonia quadrangles , centered at 24°48′N 196°00′E  /  24.8°N 196.0°E  / 24.8; 196.0 . The plain's topography exhibits extremely smooth features at several different lengths of scale. A large part of

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288-628: Is the fact that the area gives almost no radar return. The lower portion (member) of Medusae Fossae Formation contains many patterns and shapes that are thought to be the remains of streams. It is believed that streams formed valleys that were filled and became resistant to erosion by cementation of minerals or by the gathering of a coarse covering layer to form an inverted relief . These inverted stream beds are sometimes called sinuous ridges or raised curvilinear features. They have been divided into six classes: flat-crested, narrow-crested, round-crested, branching, non-branching, and multilevel. They may be

312-485: The Amazonian Epoch because researchers originally (and incorrectly) thought Amazonis Planitia to be representative of all Martian plains. Instead, over the past two decades, researchers have realized that the area's youth and extremely smooth surface actually distinguish the area from its neighbors. It is even possible that the area possessed distinctive characteristics when all of Mars was under water. Although

336-737: The Medusae Fossae Formation lies in Amazonis Planitia. Its name derives from one of the classical albedo features observed by early astronomers, which was in turn named after the Amazons , a mythical race of warrior women. Only approximately 100 million years old, these plains provide some of the fewest sedimentary layers impeding viewing of the Martian terrain, and closely resemble the composition of Earth's Iceland . Formed by free-flowing lava across great plains, Amazonis has been described by William Hartmann as

360-418: The Tharsis and Elysium volcanic areas, and extends across five quadrangles: Amazonis , Tharsis , Memnonia , Elysium , and Aeolis . The origin of the formation is unknown, but many theories have been presented over the years. In 2020, a group of researchers headed by Peter Mouginis-Mark has hypothesized that the formation could have been formed from pumice rafts from the volcano Olympus Mons . In 2012,

384-440: The Sun is very great for Mars, but only slight for the Earth. Also, every few years, the entire planet is engulfed in a global dust storm. When NASA's Mariner 9 craft arrived there, nothing could be seen through the dust storm. Other global dust storms have also been observed, since that time. Brain terrain is common in many places on Mars. It is formed when ice sublimates along cracks. The ridges of brain terrain may contain

408-519: The atmosphere covering everything. We know a lot about this dust because the solar panels of Mars rovers get covered with dust. The power of the Rovers has been saved many times by the wind, in the form of dust devils that have cleared the panels and boosted the power. So we know that dust falls from the atmosphere frequently. It is most generally accepted that the streaks represent avalanches of dust. Streaks appear in areas covered with dust. When

432-532: The equator of Mars. The surface of the formation has been eroded by the wind into a series of linear ridges called yardangs. These ridges generally point in direction of the prevailing winds that carved them and demonstrate the erosive power of Martian winds. The easily eroded nature of the Medusae Fossae Formation suggests that it is composed of weakly cemented particles, Linear ridge networks are found in various places on Mars in and around craters. Ridges often appear as mostly straight segments that intersect in

456-460: The formation appears as a smooth and gently undulating surface, while in others it is wind-sculpted into ridges and grooves. Radar imaging has suggested that the region may contain either extremely porous rock (for example volcanic ash) or deep layers of glacier-like ice deposits amounting to about the same quantity as is stored in Mars' south polar cap. Further evidence for a fine-grained composition

480-547: The formation has been eroded by the wind into a series of linear ridges called yardangs . These ridges generally point in direction of the prevailing winds that carved them, and demonstrate the erosive power of Martian winds. The easily eroded nature of the Medusae Fossae Formation suggests that it is composed of weakly cemented particles, and was most likely formed by the deposition of wind-blown dust or volcanic ash . Yardangs are parts of rock that have been sand blasted into long, skinny ridges by bouncing sand particles blowing in

504-418: The full implications of Amazonis's youth have not yet been determined, the nature of the area (i.e. lack of sedimentary rock) has at least provided researchers evidence that the areas are the most likely to provide future discoveries, and as such, has been proposed as a future site for most NASA landings. The Medusae Fossae Formation is a soft, easily eroded deposit that extends for nearly 1,000 km along

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528-471: The wind. Layers are seen in parts of the formation. A resistant caprock on the top of yardangs has been observed in Viking, Mars Global Surveyor , and HiRISE photos. Images from spacecraft show that they have different degrees of hardness probably because of significant variations in the physical properties, composition, particle size, and/or cementation . Very few impact craters are visible throughout

552-437: The youngest streaks are dark and they become lighter with age. Often they begin as a small narrow spot then widen and extend downhill for hundreds of meters. Several ideas have been advanced to explain the streaks. Some involve water , or even the growth of organisms . The streaks appear in areas covered with dust. Much of the Martian surface is covered with dust because at more or less regular intervals dust settles out of

576-519: Was stable on the surface. By means of a re-analysis of data from Mars Express ' MARSIS radar, Thomas Watters found evidence about the existence of large underground water deposits in Medusae Fossae up to 3.7 km thick and covered by hundreds of meters of dust. Combining several gravity models of Mars with the MOLA topographic dataset allowed calculation of the density of the deposit; the value

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