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Contents:
  1. Space-rock hunting
  2. Primary menu
  3. IRON METEORITES
  4. Feature: A castaway from ancient Mars | Science | AAAS
  5. References

The name designated by the Meteoritical Society is used by scientists, catalogers, and most collectors.

Space-rock hunting

Most meteoroids disintegrate when entering the Earth's atmosphere. Usually, five to ten a year are observed to fall and are subsequently recovered and made known to scientists. Instead, they typically arrive at the surface at their terminal velocity and, at most, create a small pit. Large meteoroids may strike the earth with a significant fraction of their escape velocity second cosmic velocity , leaving behind a hypervelocity impact crater. The kind of crater will depend on the size, composition, degree of fragmentation, and incoming angle of the impactor.

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The force of such collisions has the potential to cause widespread destruction. Examples of craters caused by iron meteoroids include Barringer Meteor Crater , Odessa Meteor Crater , Wabar craters , and Wolfe Creek crater ; iron meteorites are found in association with all of these craters. In contrast, even relatively large stony or icy bodies like small comets or asteroids , up to millions of tons, are disrupted in the atmosphere, and do not make impact craters.

Very large stony objects, hundreds of meters in diameter or more, weighing tens of millions of tons or more, can reach the surface and cause large craters but are very rare.

IRON METEORITES

Such events are generally so energetic that the impactor is completely destroyed, leaving no meteorites. The very first example of a stony meteorite found in association with a large impact crater, the Morokweng crater in South Africa, was reported in May Several phenomena are well documented during witnessed meteorite falls too small to produce hypervelocity craters. Various colors have been reported, including yellow, green, and red. Flashes and bursts of light can occur as the object breaks up.

Feature: A castaway from ancient Mars | Science | AAAS

Explosions, detonations, and rumblings are often heard during meteorite falls, which can be caused by sonic booms as well as shock waves resulting from major fragmentation events. These sounds can be heard over wide areas, with a radius of a hundred or more kilometers. Whistling and hissing sounds are also sometimes heard but are poorly understood. Following the passage of the fireball, it is not unusual for a dust trail to linger in the atmosphere for several minutes. As meteoroids are heated during atmospheric entry , their surfaces melt and experience ablation.

They can be sculpted into various shapes during this process, sometimes resulting in shallow thumbprint-like indentations on their surfaces called regmaglypts. If the meteoroid maintains a fixed orientation for some time, without tumbling, it may develop a conical "nose cone" or "heat shield" shape. As it decelerates, eventually the molten surface layer solidifies into a thin fusion crust, which on most meteorites is black on some achondrites , the fusion crust may be very light-colored. On stony meteorites, the heat-affected zone is at most a few mm deep; in iron meteorites, which are more thermally conductive, the structure of the metal may be affected by heat up to 1 centimetre 0.

Reports vary; some meteorites are reported to be "burning hot to the touch" upon landing, while others are alleged to have been cold enough to condense water and form a frost. Meteoroids that experience disruption in the atmosphere may fall as meteorite showers, which can range from only a few up to thousands of separate individuals.

References

The area over which a meteorite shower falls is known as its strewn field. Strewn fields are commonly elliptical in shape, with the major axis parallel to the direction of flight. In most cases, the largest meteorites in a shower are found farthest down-range in the strewn field. Most meteorites are stony meteorites, classed as chondrites and achondrites. Modern classification of meteorites is complex. The review paper of Krot et al.


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These particles, or chondrules , are composed mostly of silicate minerals that appear to have been melted while they were free-floating objects in space. Certain types of chondrites also contain small amounts of organic matter , including amino acids , and presolar grains. Chondrites are typically about 4.

thisislamu.com/dipaw-de-comida-ejemplo.php Like comets , chondritic asteroids are some of the oldest and most primitive materials in the solar system. Chondrites are often considered to be "the building blocks of the planets".


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  • Most achondrites are also ancient rocks, and are thought to represent crustal material of differentiated planetesimals. One large family of achondrites the HED meteorites may have originated on the parent body of the Vesta Family , although this claim is disputed. Two small groups of achondrites are special, as they are younger and do not appear to come from the asteroid belt.

    One of these groups comes from the Moon, and includes rocks similar to those brought back to Earth by Apollo and Luna programs. The other group is almost certainly from Mars and constitutes the only materials from other planets ever recovered by humans. Most iron meteorites are thought to come from the cores of planetesimals that were once molten. As with the Earth, the denser metal separated from silicate material and sank toward the center of the planetesimal, forming its core.

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    After the planetesimal solidified, it broke up in a collision with another planetesimal. This would be explained by a recovery bias; laypeople are more likely to notice and recover solid masses of metal than most other meteorite types. The abundance of iron meteorites relative to total Antarctic finds is 0. They are a mixture of iron-nickel metal and silicate minerals. One type, called pallasites , is thought to have originated in the boundary zone above the core regions where iron meteorites originated. The other major type of stony-iron meteorites is the mesosiderites. Tektites from Greek tektos , molten are not themselves meteorites, but are rather natural glass objects up to a few centimeters in size that were formed—according to most scientists—by the impacts of large meteorites on Earth's surface.

    A few researchers have favored tektites originating from the Moon as volcanic ejecta, but this theory has lost much of its support over the last few decades. In March , NASA scientists reported that, for the first time, complex organic compounds found in DNA and RNA , including uracil , cytosine and thymine , have been formed in the laboratory under outer space conditions, using starting chemicals, such as pyrimidine , found in meteorites.

    Pyrimidine and polycyclic aromatic hydrocarbons PAHs may have been formed in red giants or in interstellar dust and gas clouds, according to the scientists. In January , researchers found that 4. Most meteorite falls are recovered on the basis of eyewitness accounts of the fireball or the impact of the object on the ground, or both. Therefore, despite the fact that meteorites fall with virtually equal probability everywhere on Earth, verified meteorite falls tend to be concentrated in areas with high human population densities such as Europe, Japan, and northern India.

    A small number of meteorite falls have been observed with automated cameras and recovered following calculation of the impact point. The images were used both to determine the location of the stones on the ground and, more significantly, to calculate for the first time an accurate orbit for a recovered meteorite.

    Following the Pribram fall, other nations established automated observing programs aimed at studying infalling meteorites. This program also observed a meteorite fall, the Lost City chondrite, allowing its recovery and a calculation of its orbit. It too recovered a single meteorite, Innisfree , in Until the twentieth century, only a few hundred meteorite finds had ever been discovered.

    To this day, few stony meteorites are reported each year that can be considered to be "accidental" finds. The reason there are now more than 30, meteorite finds in the world's collections started with the discovery by Harvey H.

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    Nininger that meteorites are much more common on the surface of the Earth than was previously thought. Nininger's strategy was to search for meteorites in the Great Plains of the United States, where the land was largely cultivated and the soil contained few rocks. Between the late s and the s, he traveled across the region, educating local people about what meteorites looked like and what to do if they thought they had found one, for example, in the course of clearing a field.

    The result was the discovery of over new meteorites, mostly stony types. In the late s, Roosevelt County, New Mexico in the Great Plains was found to be a particularly good place to find meteorites. After the discovery of a few meteorites in , a public awareness campaign resulted in the finding of nearly new specimens in the next few years, with many being by a single person, Ivan Wilson.

    In total, nearly meteorites were found in the region since In the area of the finds, the ground was originally covered by a shallow, loose soil sitting atop a hardpan layer. During the dustbowl era, the loose soil was blown off, leaving any rocks and meteorites that were present stranded on the exposed surface. A few meteorites were found in Antarctica between and In , the 10th Japanese Antarctic Research Expedition found nine meteorites on a blue ice field near the Yamato Mountains. With this discovery, came the realization that movement of ice sheets might act to concentrate meteorites in certain areas.

    This team recovered nearly meteorites.