Chondrite - Knowledge

1010: 1443:. (Type 1 and 2 chondrites are also unequilibrated.) Chondrites that remain in nearly pristine condition, with all components (chondrules, matrix, etc.) having nearly the same composition and mineralogy as when they accreted to the parent asteroid, are designated type 3.0. As petrologic type increases from type 3.1 through 3.9, profound mineralogical changes occur, starting in the dusty matrix, and then increasingly affecting the coarser-grained components like chondrules. Type 3.9 chondrites still look superficially unchanged because chondrules retain their original appearances, but all of the minerals have been affected, mostly due to 327: 1189:, and lacking metallic Fe. It is a matter of some controversy whether they once had chondrules and refractory inclusions that were later destroyed during formation of hydrous minerals, or they never had chondrules in the first place. CI chondrites are notable because their chemical compositions closely resemble that of the solar photosphere, neglecting the hydrogen and helium. Thus, they have the most "primitive" compositions of any meteorites and are often used as a standard for assessing the degree of chemical fractionation experienced by materials formed throughout the Solar System. 919: 1139: 995: 1312:

elements, and the fact that O/O ratios are anomalously high compared to Earth rocks. However, there are significant differences between R chondrites and ordinary chondrites: R chondrites have much more dusty matrix material (about 50% of the rock); they are much more oxidized, containing little metallic Fe–Ni; and their enrichments in O are higher than those of ordinary chondrites. Nearly all the metal they contain is oxidized or in the form of sulfides. They contain fewer chondrules than the E chondrites and appear to come from an asteroid's

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groups. Although CR chondrites are clearly similar in most ways to other chondrite groups, the origins of CH and CB chondrites are somewhat controversial. Some workers conclude that many of the chondrules and metal grains in these chondrites may have formed by impact processes after "normal" chondrules had already formed, and thus they may not be "true" chondrites.

498:. The various chondrite groups likely originated on separate asteroids or groups of related asteroids. Each chondrite group has a distinctive mixture of chondrules, refractory inclusions, matrix (dust), and other components and a characteristic grain size. Other ways of classifying chondrites include weathering and shock. 349: 1246:(subgroup a) chondrites are coarse grained, with large, often cm-sized chondrules and metal grains and almost no refractory inclusions. Chondrules have unusual textures compared to most other chondrites. As in CH chondrites, dusty material only occurs in discrete clasts, and there is no fine-grained matrix. CB 1416:

hydrous phases. This alteration took place at temperatures of 50 to 150 °C, so type 1 chondrites were warm, but not hot enough to experience thermal metamorphism. The members of the CI group, plus a few highly altered carbonaceous chondrites of other groups, are the only instances of type 1 chondrites.

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CH chondrites are remarkable for their very tiny chondrules, typically only about 0.02 mm (20 micrometres) in diameter. They have a small proportion of equally tiny refractory inclusions. Dusty material occurs as discrete clasts, rather than as a true matrix. CH chondrites are also distinguished

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Rumuruti (R) type chondrites are a very rare group, with only one documented fall out of almost 900 documented chondrite falls. They have a number of properties in common with ordinary chondrites, including similar types of chondrules, few refractory inclusions, similar chemical composition for most

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Three chondrites form what is known as the K (Kakangari type) grouplet: Kakangari, LEW 87232, and Lea Co. 002. They are characterized by large amounts of dusty matrix and oxygen isotope compositions similar to carbonaceous chondrites, highly reduced mineral compositions and high metal abundances (6%

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Chondrites can also be categorized according to their petrologic type, which is the degree to which they were thermally metamorphosed or aqueously altered (they are assigned a number between 1 and 7). The chondrules in a chondrite that is assigned a "3" have not been altered. Larger numbers indicate

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There are many groups of carbonaceous chondrites, but most of them are distinguished chemically by enrichments in refractory lithophile elements relative to Si and isotopically by unusually low ratios of O/O relative to O/O, when compared to Earth rocks. All groups of carbonaceous chondrites except

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was originally used to designate chondrites that lacked chondrules and contained large amounts of water and carbon. Current usage of type 1 is simply to indicate meteorites that have experienced extensive aqueous alteration, to the point that most of their olivine and pyroxene have been altered to

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and coarsened in grain size. By type 5, chondrules begin to become indistinct and matrix cannot be discerned. In type 6 chondrites, chondrules begin to integrate with what was once matrix, and small chondrules may no longer be recognizable. As metamorphism proceeds, many minerals coarsen and new,

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chondrites are those that have experienced extensive aqueous alteration, but still contain recognizable chondrules as well as primary, unaltered olivine and/or pyroxene. The fine-grained matrix is generally fully hydrated and minerals inside chondrules may show variable degrees of hydration. This

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Because chondrites accumulated from material that formed very early in the history of the Solar System, and because chondritic asteroids did not melt, they have very primitive compositions. "Primitive," in this sense, means that the abundances of most chemical elements do not differ greatly from

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of the sun, which in turn should be well-representative of the entire Solar System (note: to make such a comparison between a gaseous object like the sun and a rock like a chondrite, scientists choose one rock-forming element, such as silicon (Si), to use as a reference point, and then compare

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type), CB (Bencubbin type), and CH (high metal) carbonaceous chondrites are three groups that seem to be related by their chemical and oxygen isotopic compositions. All are rich in metallic Fe–Ni, with CH and especially CB chondrites having a higher proportion of metal than all other chondrite

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At some point during the formation of many chondrites, particles of metal became partially separated from particles of silicate minerals. As a result, chondrites coming from asteroids that did not accrete with their full complement of metal (e.g., L, LL, and EL chondrites) are depleted in all

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elements like Ca and Al became separated from less refractory elements like Mg and Si, and were not uniformly sampled by each asteroid. The parent bodies of many groups of carbonaceous chondrites contain over-sampled grains rich in refractory elements, whereas those of ordinary and enstatite

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type) chondrites are characterized by mm-sized chondrules and abundant refractory inclusions set in a dark matrix that comprises about half the rock. CV chondrites are noted for spectacular refractory inclusions, some of which reach centimetre sizes, and they are the only group to contain a

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type) chondrites are chemically and texturally similar to CV chondrites. However, they contain far fewer refractory inclusions than CV, they are much more oxidized rocks, and most of them have experienced considerable amounts of thermal metamorphism (compared to CV and all other groups of

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and a few million years after the asteroid formed the ice would have melted allowing the liquid water to react with and alter the olivines and pyroxenes. The formation of rivers and lakes on the asteroid is thought to have been unlikely if it was sufficiently porous to allow the water to

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Although all chondrite compositions can be considered primitive, there is variation among the different groups, as discussed above. CI chondrites seem to be nearly identical in composition to the sun for all but the gas-forming elements (e.g., hydrogen (H), carbon (C), nitrogen (N), and

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of particles of dust and grit present in the primitive Solar System which gave rise to asteroids over 4.54 billion years ago. These asteroid parent bodies of chondrites are (or were) small to medium-sized asteroids that were never part of any body large enough to undergo melting and

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Most, but not all, ordinary chondrites have experienced significant degrees of metamorphism, having reached temperatures well above 500 °C on the parent asteroids. They are divided into three groups, which have different amounts of metal and different amounts of total iron:

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an increase in thermal metamorphosis up to a maximum of 7, where the chondrules have been destroyed. Numbers lower than 3 are given to chondrites whose chondrules have been changed by the presence of water, down to 1, where the chondrules have been obliterated by this alteration.

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are by far the most common type of meteorite to fall to Earth: about 80% of all meteorites and over 90% of chondrites are ordinary chondrites. They contain abundant chondrules, sparse matrix (10–15% of the rock), few refractory inclusions, and variable amounts of Fe–Ni metal and

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Enstatite chondrites (also known as E-type chondrites) are a rare form of meteorite thought to comprise only about 2% of the chondrites that fall to Earth. Only about 200 E-Type chondrites are currently known. The majority of enstatite chondrites have either been recovered in

1166:. They are thought to have been formed the farthest from the sun of any of the chondrites as they have the highest proportion of volatile compounds. Another of their main characteristics is the presence of water or of minerals that have been altered by the presence of water. 1230:

CR chondrites have chondrules that are similar in size to those in ordinary chondrites (near 1 mm), few refractory inclusions, and matrix comprises nearly half the rock. Many CR chondrites have experienced extensive aqueous alteration, but some have mostly escaped this

318:, veining, localized melting, and formation of high-pressure minerals. The net result of these secondary thermal, aqueous, and shock processes is that only a few known chondrites preserve in pristine form the original dust, chondrules, and inclusions from which they formed. 1423:

alteration probably occurred at temperatures below 20 °C, and again, these meteorites are not thermally metamorphosed. Almost all CM and CR chondrites are petrologic type 2; with the exception of some ungrouped carbonaceous chondrites, no other chondrites are type 2.

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These meteorites either contain a proportion of water or minerals that have been altered by water. This suggests that the asteroid from which these meteorites originate must have contained water. At the beginning of the Solar System this would have been present as

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have high total iron and high metallic Fe (15–20% Fe–Ni metal by mass), and smaller chondrules than L and LL chondrites. They are formed of bronzite, olivine, pyroxene, plagioclase, metals and sulfides and ~42% of ordinary chondrite falls belong to this group

1659:(carbonaceous chondrites normally contain concentrations of 15 ppm or less). This could indicate that organic material is more abundant in the Solar System than was previously believed, and it reinforces the idea that the organic compounds present in the 1407:

The petrologic-type scheme originated by Van Schmus and Wood is really two separate schemes, one describing aqueous alteration (types 1–2) and one describing thermal metamorphism (types 3–6). The aqueous alteration part of the system works as follows:

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All groups of ordinary and enstatite chondrites, as well as R and CK chondrites, show the complete metamorphic range from type 3 to 6. CO chondrites comprise only type 3 members, although these span a range of petrologic types from 3.0 to 3.8.

1177:(Ivuna type) chondrites entirely lack chondrules and refractory inclusions; they are composed almost exclusively of fine-grained material that has experienced a high degree of aqueous alteration on the parent asteroid. CI chondrites are highly 1427:

The thermal metamorphism part of the scheme describes a continuous sequence of changes to mineralogy and texture that accompany increasing metamorphic temperatures. These chondrites show little evidence of the effects of aqueous alteration:

1404:, which appears as a number following the group name (e.g., an LL5 chondrite belongs to the LL group and has a petrologic type of 5). The current scheme for describing petrologic types was devised by Van Schmus and Wood in 1967. 298:

in their interiors. The source of the heat was most likely energy coming from the decay of short-lived radioisotopes (half-lives less than a few million years) that were present in the newly formed Solar System, especially

234:, which are believed to have formed more recently than chondrites. There are currently over 27,000 chondrites in the world's collections. The largest individual stone ever recovered, weighing 1770 kg, was part of the 307:, although heating may have been caused by impacts onto the asteroids as well. Many chondritic asteroids also contained significant amounts of water, possibly due to the accretion of ice along with rocky material. 1196:) and CM (Mighei type) chondrites are two related groups that contain very small chondrules, mostly 0.1 to 0.3 mm in diameter; refractory inclusions are quite abundant and have similar sizes to chondrules. 2517:

Aaron S. Burton; Jamie E. Elsila; Jason E. Hein; Daniel P. Glavin; Jason P. Dworkin (March 2013). "Extra-terrestrial amino acids identified in metal-rich CH and CB carbonaceous chondrites from Antarctica".

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Michael K. Weisberga; Martin Prinza; Robert N. Claytonb; Toshiko K. Mayedab; Monica M. Gradyc; Ian Franchid; Colin T. Pillingerd; Gregory W. Kallemeyne (1996). "The K (Kakangari) chondrite grouplet".

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distinctive type of large, once-molten inclusions. Chemically, CV chondrites have the highest abundances of refractory lithophile elements of any chondrite group. The CV group includes the remarkable

314:. In addition, all chondritic asteroids were affected by impact and shock processes due to collisions with other asteroids. These events caused a variety of effects, ranging from simple compaction to 1478:, although there is not consensus on whether this is necessary. Type 7 chondrites have experienced the highest temperatures possible, short of that required to produce melting. Should the onset of 192:

become the most common type of meteorite by arriving on a trajectory toward the planet's surface. Estimates for their contribution to the total meteorite population vary between 85.7% and 86.2%.

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have low total iron contents (including 7–11% Fe–Ni metal by mass). ~46% of ordinary chondrite falls belong to this group, which makes them the most common type of meteorite to fall on Earth.

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meteorite, which fell in Canada in 2000 and is intermediate between CI and CM chondrites; and Acfer 094, an extremely primitive chondrite that shares properties with both CM and CO groups.

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Although chondritic asteroids never became hot enough to melt based upon internal temperatures, many of them reached high enough temperatures that they experienced significant thermal

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meteorite shower of 1976. Chondrite falls range from single stones to extraordinary showers consisting of thousands of individual stones. An instance of the latter occurred in the

1605:) of hydrocarbons and ammonium carbonate in the presence of liquid water. In addition, the hydrocarbons could have formed deep within a planetoid by a process similar to the 1282:

Ungrouped carbonaceous chondrites: A number of chondrites are clearly members of the carbonaceous chondrite class, but do not fit into any of the groups. These include: the

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has been thoroughly studied; it fell in Australia close to the town that bears its name on 28 September 1969. It is a CM2 and it contains common amino acids such as

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Múñoz-Espadas, M.J.; Martínez-Frías, J.; Lunar, R. (2003). "Mineralogía, texturas y cosmoquímica de cóndrulos RP y PO en la condrita Reliegos L5 (León, España)".

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Carbonaceous chondrites contain more than 600 organic compounds that were synthesized in distinct places and at distinct times. These organic compounds include:

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As a result, many chondrites contain hydrous minerals, such as clays, that formed when the water interacted with the rock on the asteroid in a process known as

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Two meteorites that were collected in Antarctica in 1992 and 1995 were found to be abundant in amino acids, which are present at concentrations of 180 and 249

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rocks known, with most of their iron taking the form of metal or sulfide rather than as an oxide. This suggests that they were formed in an area that lacked

1049:(FeS). Their chondrules are generally in the range of 0.5 to 1 mm in diameter. Ordinary chondrites are distinguished chemically by their depletions in 1439:

chondrites because minerals such as olivine and pyroxene show a wide range of compositions, reflecting formation under a wide variety of conditions in the

467:, and their origin continues to be the object of some debate. The scientific community generally accepts that these spheres were formed by the action of a 1210:

CO chondrites have only about 30% matrix and have experienced very little aqueous alteration. Most have experienced small degrees of thermal metamorphism.

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Boss, A.P.; Durisen, R.H. (2005). "Chondrule-forming Shock Fronts in the Solar Nebula: A Possible Unified Scenario for Planet and Chondrite Formation".

389:, millimetre-sized spherical objects that originated as freely floating, molten or partially molten droplets in space; most chondrules are rich in the 1242:

CB chondrites occur in two types, both of which are similar to CH chondrites in that they are very depleted in volatile elements and rich in metal. CB

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chondrites, in which the compositions of most minerals have become quite homogeneous due to high temperatures. By type 4, the matrix has thoroughly

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CM chondrites are composed of about 70% fine-grained material (matrix), and most have experienced extensive aqueous alteration. The much studied

463:, which predate the formation of our solar system and originated elsewhere in the galaxy. The chondrules have distinct texture, composition and 2717: 1275:

CL (Loongana type) chondrites are largely chondrules and CAIs, correspondingly low in matrix and volatiles, with trace elements resembling CR.

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elements, whereas those that accreted too much metal (e.g., CH, CB, and EH chondrites) are enriched in these elements compared to the sun.

2803: 2138: 872: 428: 2690: 2495: 1158:(also known as C-type chondrites) make up less than 5% of the chondrites that fall on Earth. They are characterized by the presence of 1747:

The E stands for Enstatite, H indicates a high metallic iron content of approximately 30%, and L low. The number refers to alteration.

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The first fraction appears to originate from interstellar space and the compounds belonging to the other fractions derive from a

1380:. In general, the level of depletion corresponds to the degree of volatility, where the most volatile elements are most depleted. 223:

or partially molten droplets of distinct minerals. Chondrules typically constitute between 20% and 80% of a chondrite by volume.

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have low total iron and low metal contents (3–5% Fe–Ni metal by mass of which 2% is metallic Fe and they also contain bronzite,

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fall in Mexico in 1969, which became one of the most widely distributed and, certainly, the best-studied meteorite in history.

455:. The remainder of chondrites consists of fine-grained (micrometre-sized or smaller) dust, which may either be present as the 2801:

Hyman Hartman; Michael A. Sweeney; Michael A. Kropp; John S. Lewis (1993). "Carbonaceous chondrites and the origin of life".

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of the rock or may form rims or mantles around individual chondrules and refractory inclusions. Embedded in this dust are

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Small to medium asteroids that were never part of a body large enough to undergo melting and planetary differentiation.

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generated a shock wave with a velocity of more than 10 km/s, which resulted in the formation of the chondrules.

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ratios. Thus, the atomic ratio of Mg/Si measured in the sun (1.07) is identical to that measured in CI chondrites).

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Their study provides important clues for understanding the origin and age of the Solar System, the synthesis of

1590:, chloroform soluble hydrocarbons and a fraction that is soluble in methanol (which includes the amino acids). 1393:

chemical, mineralogical, and isotopic characteristics (above). The degree to which it has been affected by the

1060:, relative to Si, and isotopically by their unusually high O/O ratios relative to O/O compared to Earth rocks. 93: 81: 57: 2955: 271:, matching ages for other chronometers. Another indication of their age is the fact that the abundance of non- 239: 3790: 2253:

Van Schmus, W. R.; Wood, J. A. (1967). "A chemical-petrologic classification for the chondritic meteorites".

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that passed through the Solar System, although there is little agreement as to the cause of this shock wave.

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Except for the High Iron, all the other carbonaceous chondrites are named after a characteristic meteorite.

945: 2930: 1787:"2.2 La composición de la Tierra: el modelo condrítico in Planetología. Universidad Complutense de Madrid" 3795: 3694: 3518: 1606: 1462: 474:

An article published in 2005 proposed that the gravitational instability of the gaseous disk that formed

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This is a unique meteorite that has been suggested to be the only known sample of the D asteroid family.

1597:. It has been proposed that the amino acids were synthesized close to the surface of a planetoid by the 1250:(subgroup b) chondrites contain much smaller (mm-sized) chondrules and do contain refractory inclusions. 447:), which are among the oldest objects to form in the Solar System, particles rich in metallic Fe-Ni and 3800: 3643: 3633: 3422: 3417: 3118: 1362: 1053: 17: 2659: 1009: 3701: 3127: 3055: 2786:

Jordi Llorca i Piqué (2004). "Moléculas orgánicas en el sistema solar: ¿dónde y cómo encontrarlas?".

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It is thought possible that a proportion of the water present on the Earth comes from the impact of

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processes of thermal metamorphism and aqueous alteration on the parent asteroid is indicated by its

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Jörn Müller; Harald Lesch (2003). "Woher kommt das Wasser der Erde? – Urgaswolke oder Meteoriten".

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Norton, O.R. and Chitwood, L.A. Field Guide to Meteors and Meteorites, Springer-Verlag, London 2008

1844:"Meteorites for the Sahara: Find locations, shock classification, degree of weathering and pairing" 1678: 255: 3663: 3412: 2288:

Clayton, R. N.; Mayeda, T. K. (1989), "Oxygen Isotope Classification of Carbonaceous Chondrites",

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Meteorite articles, including discussions of chondrites in Planetary Science Research Discoveries

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Andrew M. Davis; Lawrence Grossman; R. Ganapathy (1977). "Yes, Kakangari is a unique chondrite".

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Grevesse and Sauval (2005) in Encyclopedia of Astronomy & Astrophysics, IOP Publishing, Ltd.

1582:, etc. These compounds can be divided into three main groups: a fraction that is not soluble in 3149: 1688: 1236: 1155: 1145: 1129: 1113: 415:

Shiny Ni/Fe metal is prominently displayed in this ordinary chondrite found in Northwest Africa

326: 272: 3601: 3571: 3378: 3373: 3292: 2967: 1609:. These conditions could be analogous to the events that caused the origin of life on Earth. 918: 494:

on the basis of their mineralogy, bulk chemical composition, and oxygen isotope compositions

2800: 2531: 2491: 1976: 3611: 3508: 3490: 3244: 2871: 2812: 2625: 2580: 2527: 2516: 2353: 2323: 2297: 2262: 2216: 2029: 1972: 1855: 1708: 1483: 1458: 1436: 304: 264: 2977: 8: 3513: 3185: 2991: 2107: 1814: 1786: 1633: 1617: 1547: 1204: 1057: 934: 926: 332: 3089: 2875: 2816: 2629: 2584: 2357: 2327: 2301: 2266: 2220: 2081: 2041: 2033: 1859: 1138: 3606: 3458: 3203: 2895: 2860:"Evidence for extraterrestrial amino-acids and hydrocarbons in the Murchison meteorite" 2855: 2854:

Kvenvolden, Keith A.; Lawless, James; Pering, Katherine; Peterson, Etta; Flores, Jose;

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by their low iron and nickel content. Non-metallic meteorites that lack chondrules are

32: 2693:. Meteorite Museum. University of New Mexico. Institute of Meteoritics. Archived from 2637: 2433: 2274: 1350:(Ar) etc.). Other chondrite groups deviate from the solar composition (i.e., they are 3764: 3732: 3405: 3365: 3072: 2887: 2828: 2768: 2366: 2341: 2147: 1992: 1927: 1873: 1579: 1261: 1256: 746: 452: 2557: 2236: 1368:

In a similar manner, although the exact process is not very well understood, highly

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Some workers have extended the Van Schmus and Wood metamorphic scheme to include a

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A synthesis of the various classification schemes is provided in the table below.

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to 10% by volume) that are most like enstatite chondrites, and concentrations of

1186: 460: 448: 103: 86: 2172:(in Spanish). Translated by Sara Benedicta Oyola. 18 March 2005 . Archived from 3436: 3345: 3262: 3084: 3067: 3040: 1703: 715: 235: 227: 2135: 1303:

Many of their other characteristics are similar to the O, E and C chondrites.

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The use of the term non-metallic does not imply the total absence of metals.

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Wlotzka, F. (July 1993), "A Weathering Scale for the Ordinary Chondrites",

1893:"Pistas químicas apuntan a un origen de polvo para los planetas terrestres" 1718: 1594: 1454: 1440: 1435:

chondrites show low degrees of metamorphism. They are often referred to as

1174: 1089: 300: 295: 189: 181: 180:. They are formed when various types of dust and small grains in the early 2891: 2384: 1376:

No chondrites except the CI group formed with a full, solar complement of

1207:, which fell in Australia in 1969, is the best-known member of this group. 3670: 3566: 3550: 3545: 3252: 3213: 3208: 3094: 3018: 2211: 1539: 1505: 1326: 1096:

and olivine). Only 1 in 10 ordinary chondrite falls belong to this group.

1083: 1068: 898: 421: 363: 200: 177: 39: 3585: 3257: 3235: 2824: 2539: 1683: 1598: 1583: 1575: 1531: 1369: 1297: 1163: 1093: 1050: 1015: 941: 464: 440: 385:

Prominent among the components present in chondrites are the enigmatic

348: 276: 231: 3112: 3759: 3621: 3590: 3503: 3325: 3315: 3282: 3272: 3050: 3026: 3014: 2883: 2592: 2108:"NWA 10499; Meteoritical Bulletin Database. The Meteoritical Society" 2082:"Grassland; Meteoritical Bulletin Database. The Meteoritical Society" 1693: 1673: 1649: 1602: 1444: 1399: 1335: 1182: 1024: 949: 759: 719: 386: 370: 354: 268: 208: 165: 72: 2056:"Bjurböle; Meteoritical Bulletin Database. The Meteoritical Society" 3727: 3395: 3277: 2228: 1713: 1587: 1555: 1479: 1467: 1313: 1123: 1046: 778: 398: 390: 340: 185: 2340:

Stöffler, Dieter; Keil, Klaus; Edward R.D, Scott (December 1991).

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of 1912, in which an estimated 14,000 stones grounded in northern

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Meteorites.tv. Meteorites for Science, Education & Collectors

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Wood, J.A. (1988). "Chondritic Meteorites and the Solar Nebula".

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II Curso de Ciencias Planetarias de la Universidad de Salamanca

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Calvin J. Hamilton (Translated from English by Antonio Bello).

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lithophile elements that are most like ordinary chondrites.

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the CH group are named for a characteristic type specimen:

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El sistema solar: Nuestro pequeño rincón en la vía láctea

1500: 335:: particles of dust and grit collide and accrete forming 280: 71:

A specimen of the NWA 869 chondrite (type L4–6), showing

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those that are measured by spectroscopic methods in the

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Abstracts of the Lunar and Planetary Science Conference

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elements in chondrites is similar to that found in the

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and carbonaceous chondrites with the Earth's surface.

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chondrites have been increasingly altered by thermal

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Chondrites are divided into about 15 distinct groups

188:. Some such bodies that are captured in the planet's 140: 134: 2785: 1447:

of elements between grains of different composition.

219:, grain), which are round grains formed in space as 152: 146: 143: 1917: 131: 2925:Сarnegie Institution for Science (13 March 2008). 207:. One of their characteristics is the presence of 3777: 1482:the meteorite would probably be classified as a 959:E-type chondrites are among the most chemically 1508:towards its interior, as occurs in terrestrial 864:Phyllosilicates, Magnetite, Ca-Mg-Fe carbonates 3013: 2927:"Meteorites a Rich Source for Primordial Soup" 2252: 1841: 27:Class of stony meteorites made of round grains 2999: 2287: 2248: 2246: 2021:Annual Review of Earth and Planetary Sciences 795:Olivine, Pyroxene, metals, Ca minerals and Al 2858:; Kaplan, Isaac R.; Moore, Carleton (1970). 2483: 1810: 1808: 517:Distinguishing features/Chondrule character 2956:Natural History Museum, meteorite catalogue 2804:Origins of Life and Evolution of Biospheres 2457:"metal, iron, & nickel in meteorites 1" 2342:"Shock metamorphism of ordinary chondrites" 1961:"Pb isotopic age of the Allende chondrules" 1663:could have had an extraterrestrial origin. 481: 3006: 2992: 2847: 2716:Drake, Michael J.; Righter, Kevin (2001). 2243: 2017: 1958: 1648:as well as other less common ones such as 1107: 65: 3198: 2547: 2414: 2412: 2410: 2365: 2210: 1867: 1805: 1389:A chondrite's group is determined by its 3225: 2918: 2131: 2129: 1611: 1526: 1181:, brecciated rocks, containing abundant 917: 357:in chondrite from the Bjurböle meteorite 267:gives an estimated age of 4,566.6 ± 1.0 2973:The British and Irish Meteorite Society 2379: 2377: 2313: 1290: 944:or have been collected by the American 913: 14: 3778: 2779: 2564: 2490:The Internet Encyclopedia of Science. 2407: 1959:Amelin, Yuri; Krot, Alexander (2007). 1306: 978: 956:), from which they derive their name. 948:. They tend to be high in the mineral 168:that has not been modified, by either 2987: 2906:from the original on 12 November 2021 2794: 2709: 2126: 1884: 1823:from the original on 25 February 2021 1601:(dissociation of molecules caused by 249: 226:Chondrites can be distinguished from 2718:"Where did Earth's water come from?" 2683: 2644: 2607: 2498:from the original on 8 February 2006 2374: 2188: 2114:from the original on 21 January 2016 2088:from the original on 13 January 2021 2062:from the original on 23 January 2021 1940:from the original on 13 January 2023 1920:"Nuestra historia en los meteoritos" 1493: 2520:Meteoritics & Planetary Science 2454: 2428:New England Meteoritical Services. 2421: 2166:"¿Cocinó Júpiter a los meteoritos?" 2158: 2042:10.1146/annurev.ea.16.050188.000413 2011: 1999:from the original on 16 August 2020 1965:Meteoritics & Planetary Science 1926:. Universitat Jaume I. p. 75. 1911: 1384: 24: 2465:Washington University in St. Louis 1985:10.1111/j.1945-5100.2007.tb00559.x 1899:from the original on 3 August 2008 1869:10.1111/j.1945-5100.1995.tb01219.x 1373:chondrites were deficient in them. 1056:elements, such as Ca, Al, Ti, and 380: 25: 3812: 2949: 2395:from the original on 9 March 2021 1890: 1842:Bischoff, A.; Geiger, T. (1995). 1793:from the original on 15 June 2009 1522: 369:Chondrules in chondrite from the 31:For trace fossil ichnogenus, see 1137: 1122: 1100:An example of this group is the 1023: 1008: 993: 420: 408: 362: 347: 325: 127: 2744: 2674: 2617:Geochimica et Cosmochimica Acta 2510: 2448: 2346:Geochimica et Cosmochimica Acta 2333: 2307: 2281: 2255:Geochimica et Cosmochimica Acta 2100: 2074: 1759: 1750: 1741: 1132:CV3 that fell in Mexico in 1969 2048: 1952: 1835: 1779: 1732: 1319: 254:Chondrites were formed by the 13: 1: 2638:10.1016/S0016-7037(96)00233-5 2275:10.1016/S0016-7037(67)80030-9 1772: 1466:metamorphic minerals such as 1356:) in highly systematic ways: 203:and the presence of water on 2367:10.1016/0016-7037(91)90078-J 1918:Jordi, Llorca Pique (2004). 946:National Weather Association 427:Chondrule in Chondrite from 7: 1666: 837:Chondrules and CAIs, metals 809:Olivine, Ca minerals and Al 184:accreted to form primitive 10: 3817: 3644:extraterrestrial materials 1817:"Meteoroides y Meteoritos" 1111: 982: 932: 777:Phyllosilicates, Olivine, 703: 569: 29: 3720: 3679: 3584: 3559: 3533: 3489: 3435: 3364: 3336: 3291: 3243: 3234: 3140: 3103: 3025: 2980:from Meteorites Australia 2691:"Asteroid Geology: Water" 2198:The Astrophysical Journal 1272:carbonaceous chondrites). 1235:by extreme depletions in 1076:Meteorite fall statistics 851:Pyroxene, metals, Olivine 660: 617: 574: 527: 524: 490:Meteorites classification 451:, and isolated grains of 261:planetary differentiation 112: 102: 92: 80: 64: 55: 50: 2652:"R Group (Rumurutiites)" 2492:"carbonaceous chondrite" 1725: 1679:Meteorite classification 1486:instead of a chondrite. 482:Chondrite classification 439:Chondrites also contain 38:Not to be confused with 3423:Meteorites on Mars list 3418:Martian meteorites list 2640:. 0016-7037, 4253–4263. 2532:2013M&PS...48..390B 1977:2007M&PS...42.1043F 1699:Glossary of meteoritics 1607:Fischer–Tropsch process 1156:Carbonaceous chondrites 1108:Carbonaceous chondrites 705:Carbonaceous chondrites 431:LL3 Primitive Chondrite 2765:10.1002/ciuz.200300282 2753:Chemie in unserer Zeit 1689:Carbonaceous chondrite 1629: 1535: 1277:Triple oxygen position 1146:Carbonaceous chondrite 1130:Carbonaceous chondrite 1114:Carbonaceous chondrite 967:, probably within the 930: 443:inclusions (including 3572:Nonmagmatic meteorite 2961:12 March 2008 at the 2603:. 0028-0836, 230–232. 2385:"Types of Meteorites" 2170:Astrobiology Magazine 1620:is on display at the 1615: 1530: 1162:compounds, including 921: 754:Olivines rich in Fe, 525:Enstatite chondrites 113:Total known specimens 3791:Chondrite meteorites 3639:Ca–Al-rich inclusion 2461:meteorites.wustl.edu 2389:The Meteorite Market 1709:Stony-iron meteorite 1652:and pseudo-leucine. 1484:primitive achondrite 1291:Kakangari chondrites 1279:near the CV-CK area. 914:Enstatite chondrites 897:Olivine, Pyroxenes, 2876:1970Natur.228..923K 2856:Ponnamperuma, Cyril 2817:1993OLEB...23..221H 2697:on 15 December 2012 2630:1996GeCoA..60.4253W 2585:1977Natur.265..230D 2436:on 21 February 2009 2358:1991GeCoA..55.3845S 2328:1993Metic..28Q.460W 2302:1989LPI....20..169C 2267:1967GeCoA..31..747V 2221:2005ApJ...621L.137B 2044:. 0084-6597, 53–72. 2034:1988AREPS..16...53W 1860:1995Metic..30..113B 1634:Murchison meteorite 1618:Murchison meteorite 1307:Rumuruti chondrites 1205:Murchison meteorite 1042:Ordinary chondrites 1018:Chondrite L6 – 1868 979:Ordinary chondrites 935:Enstatite chondrite 927:enstatite chondrite 571:Ordinary chondrites 520:Letter designation 333:Protoplanetary disk 3796:Meteorite minerals 2825:10.1007/BF01581900 2732:on 5 November 2018 2722:GSA Annual Meeting 2540:10.1111/maps.12063 1971:(7/8): 1043–1463. 1630: 1536: 1032:Ordinary chondrite 1001:Ordinary chondrite 985:Ordinary chondrite 931: 312:aqueous alteration 250:Origin and history 82:Compositional type 33:Chondrites (genus) 3801:Planetary geology 3773: 3772: 3765:Near-Earth object 3733:Atmospheric entry 3580: 3579: 3529: 3528: 3431: 3430: 2870:(5275): 923–926. 2624:(21): 4253–4263. 2579:(5591): 230–232. 2352:(12): 3845–3867. 1580:nitrogenous bases 1534:general structure 1494:Presence of water 1451:Types 4, 5, and 6 1378:volatile elements 911: 910: 735:Phyllosilicates, 453:silicate minerals 197:organic compounds 120: 119: 16:(Redirected from 3808: 3598:Characteristics 3374:Basaltic Breccia 3241: 3240: 3138: 3137: 3110: 3109: 3008: 3001: 2994: 2985: 2984: 2978:Chondrite images 2943: 2942: 2940: 2938: 2929:. Archived from 2922: 2916: 2915: 2913: 2911: 2884:10.1038/228923a0 2851: 2845: 2844: 2798: 2792: 2791: 2783: 2777: 2776: 2748: 2742: 2741: 2739: 2737: 2728:. Archived from 2713: 2707: 2706: 2704: 2702: 2687: 2681: 2678: 2672: 2671: 2669: 2667: 2662:on 18 April 2013 2658:. Archived from 2648: 2642: 2641: 2611: 2605: 2604: 2593:10.1038/265230a0 2568: 2562: 2561: 2551: 2549:2060/20130014351 2514: 2508: 2507: 2505: 2503: 2487: 2481: 2480: 2478: 2476: 2467:. Archived from 2455:Korotev, Randy. 2452: 2446: 2445: 2443: 2441: 2432:. Archived from 2425: 2419: 2416: 2405: 2404: 2402: 2400: 2381: 2372: 2371: 2369: 2337: 2331: 2330: 2311: 2305: 2304: 2285: 2279: 2278: 2250: 2241: 2240: 2214: 2212:astro-ph/0501592 2205:(2): L137–L140. 2192: 2186: 2185: 2183: 2181: 2176:on 19 April 2007 2162: 2156: 2155: 2133: 2124: 2123: 2121: 2119: 2104: 2098: 2097: 2095: 2093: 2078: 2072: 2071: 2069: 2067: 2052: 2046: 2045: 2015: 2009: 2008: 2006: 2004: 1956: 1950: 1949: 1947: 1945: 1915: 1909: 1908: 1906: 1904: 1888: 1882: 1881: 1871: 1839: 1833: 1832: 1830: 1828: 1812: 1803: 1802: 1800: 1798: 1783: 1766: 1763: 1757: 1754: 1748: 1745: 1739: 1736: 1572:phosphonic acids 1544:carboxylic acids 1385:Petrologic types 1187:sulfate minerals 1141: 1126: 1027: 1012: 997: 823:Pyroxene, metals 508: 507: 445:Ca–Al inclusions 424: 412: 366: 351: 329: 160:is a stony (non- 159: 158: 155: 154: 151: 148: 145: 142: 139: 136: 133: 75:and metal flakes 69: 48: 47: 43: 36: 21: 3816: 3815: 3811: 3810: 3809: 3807: 3806: 3805: 3786:Meteorite types 3776: 3775: 3774: 3769: 3716: 3675: 3588: 3576: 3555: 3525: 3485: 3427: 3401:Orthopyroxenite 3360: 3332: 3287: 3230: 3130: 3122: 3099: 3021: 3012: 2963:Wayback Machine 2952: 2947: 2946: 2936: 2934: 2933:on 29 July 2020 2923: 2919: 2909: 2907: 2852: 2848: 2799: 2795: 2784: 2780: 2749: 2745: 2735: 2733: 2714: 2710: 2700: 2698: 2689: 2688: 2684: 2679: 2675: 2665: 2663: 2650: 2649: 2645: 2612: 2608: 2569: 2565: 2515: 2511: 2501: 2499: 2488: 2484: 2474: 2472: 2453: 2449: 2439: 2437: 2426: 2422: 2417: 2408: 2398: 2396: 2383: 2382: 2375: 2338: 2334: 2312: 2308: 2286: 2282: 2251: 2244: 2193: 2189: 2179: 2177: 2164: 2163: 2159: 2134: 2127: 2117: 2115: 2106: 2105: 2101: 2091: 2089: 2080: 2079: 2075: 2065: 2063: 2054: 2053: 2049: 2016: 2012: 2002: 2000: 1957: 1953: 1943: 1941: 1934: 1916: 1912: 1902: 1900: 1889: 1885: 1840: 1836: 1826: 1824: 1813: 1806: 1796: 1794: 1785: 1784: 1780: 1775: 1770: 1769: 1764: 1760: 1755: 1751: 1746: 1742: 1737: 1733: 1728: 1723: 1669: 1661:primordial soup 1525: 1496: 1387: 1322: 1309: 1293: 1249: 1245: 1224: 1153: 1152: 1151: 1150: 1149: 1142: 1134: 1133: 1127: 1116: 1110: 1039: 1038: 1037: 1036: 1035: 1028: 1020: 1019: 1013: 1005: 1004: 998: 987: 981: 955: 937: 916: 716:Phyllosilicates 484: 461:presolar grains 438: 436: 435: 434: 433: 432: 425: 417: 416: 413: 383: 381:Characteristics 378: 377: 376: 375: 374: 367: 359: 358: 352: 344: 343: 330: 263:. Dating using 252: 228:iron meteorites 174:differentiation 130: 126: 104:Petrologic type 76: 44: 37: 30: 28: 23: 22: 15: 12: 11: 5: 3814: 3804: 3803: 3798: 3793: 3788: 3771: 3770: 3768: 3767: 3762: 3757: 3756: 3755: 3745: 3740: 3735: 3730: 3721: 3718: 3717: 3715: 3714: 3709: 3704: 3699: 3698: 3697: 3692: 3686:Meteorites by 3683: 3681: 3677: 3676: 3674: 3673: 3668: 3667: 3666: 3661: 3653: 3652: 3651: 3646: 3641: 3631: 3630: 3629: 3624: 3616: 3615: 3614: 3609: 3604: 3595: 3593: 3582: 3581: 3578: 3577: 3575: 3574: 3569: 3563: 3561: 3560:Obsolete terms 3557: 3556: 3554: 3553: 3548: 3543: 3537: 3535: 3531: 3530: 3527: 3526: 3524: 3523: 3522: 3521: 3516: 3511: 3501: 3495: 3493: 3487: 3486: 3484: 3483: 3478: 3475: 3472: 3469: 3466: 3461: 3456: 3453: 3450: 3445: 3441: 3439: 3433: 3432: 3429: 3428: 3426: 3425: 3420: 3415: 3410: 3409: 3408: 3398: 3393: 3388: 3383: 3382: 3381: 3370: 3368: 3362: 3361: 3359: 3358: 3353: 3348: 3346:Impact breccia 3342: 3340: 3334: 3333: 3331: 3330: 3329: 3328: 3323: 3318: 3308: 3303: 3297: 3295: 3289: 3288: 3286: 3285: 3280: 3275: 3270: 3265: 3260: 3255: 3249: 3247: 3238: 3232: 3231: 3229: 3228: 3223: 3222: 3221: 3216: 3211: 3201: 3196: 3195: 3194: 3191: 3183: 3182: 3181: 3178: 3175: 3172: 3169: 3166: 3163: 3158: 3155: 3146: 3144: 3135: 3107: 3105:Classification 3101: 3100: 3098: 3097: 3092: 3087: 3085:Micrometeorite 3082: 3077: 3076: 3075: 3065: 3064: 3063: 3058: 3053: 3048: 3038: 3032: 3030: 3023: 3022: 3011: 3010: 3003: 2996: 2988: 2982: 2981: 2975: 2970: 2965: 2951: 2950:External links 2948: 2945: 2944: 2917: 2846: 2811:(4): 221–227. 2793: 2778: 2759:(4): 242–246. 2743: 2708: 2682: 2673: 2643: 2606: 2563: 2526:(3): 390–402. 2509: 2482: 2471:on 2 July 2019 2447: 2420: 2406: 2373: 2332: 2306: 2280: 2261:(5): 747–765. 2242: 2229:10.1086/429160 2187: 2157: 2142:(in Spanish). 2125: 2099: 2073: 2047: 2010: 1951: 1933:978-8480214667 1932: 1910: 1895:(in Spanish). 1883: 1854:(1): 113–122. 1834: 1819:(in Spanish). 1804: 1777: 1776: 1774: 1771: 1768: 1767: 1758: 1749: 1740: 1730: 1729: 1727: 1724: 1722: 1721: 1716: 1711: 1706: 1704:Iron meteorite 1701: 1696: 1691: 1686: 1681: 1676: 1670: 1668: 1665: 1568:sulfonic acids 1524: 1523:Origin of life 1521: 1495: 1492: 1472: 1471: 1463:recrystallized 1448: 1437:unequilibrated 1425: 1424: 1417: 1386: 1383: 1382: 1381: 1374: 1366: 1321: 1318: 1308: 1305: 1292: 1289: 1288: 1287: 1280: 1273: 1265: 1253: 1252: 1251: 1247: 1243: 1240: 1232: 1222: 1221: 1213: 1212: 1211: 1208: 1198: 1197: 1190: 1143: 1136: 1135: 1128: 1121: 1120: 1119: 1118: 1117: 1112:Main article: 1109: 1106: 1098: 1097: 1087: 1081: 1029: 1022: 1021: 1014: 1007: 1006: 999: 992: 991: 990: 989: 988: 983:Main article: 980: 977: 953: 933:Main article: 915: 912: 909: 908: 905: 895: 892: 886: 885: 882: 879: 876: 869: 868: 865: 862: 856: 855: 852: 849: 842: 841: 838: 835: 828: 827: 824: 821: 814: 813: 810: 807: 800: 799: 796: 793: 786: 785: 782: 775: 766: 765: 762: 752: 743: 742: 739: 733: 726: 725: 722: 713: 707: 701: 700: 697: 693: 692: 689: 685: 684: 681: 677: 676: 673: 669: 668: 665: 662: 658: 657: 654: 650: 649: 646: 642: 641: 638: 634: 633: 630: 626: 625: 622: 619: 615: 614: 611: 607: 606: 603: 599: 598: 595: 591: 590: 587: 583: 582: 579: 576: 573: 567: 566: 563: 559: 558: 555: 551: 550: 547: 543: 542: 539: 535: 534: 531: 528: 526: 522: 521: 518: 515: 512: 483: 480: 426: 419: 418: 414: 407: 406: 405: 404: 403: 382: 379: 368: 361: 360: 353: 346: 345: 331: 324: 323: 322: 321: 320: 251: 248: 201:origin of life 118: 117: 114: 110: 109: 106: 100: 99: 96: 90: 89: 84: 78: 77: 70: 62: 61: 53: 52: 26: 9: 6: 4: 3: 2: 3813: 3802: 3799: 3797: 3794: 3792: 3789: 3787: 3784: 3783: 3781: 3766: 3763: 3761: 3758: 3754: 3751: 3750: 3749: 3746: 3744: 3741: 3739: 3736: 3734: 3731: 3729: 3726: 3723: 3722: 3719: 3713: 3712:Organizations 3710: 3708: 3705: 3703: 3700: 3696: 3693: 3691: 3690:find location 3688: 3687: 3685: 3684: 3682: 3678: 3672: 3669: 3665: 3664:Widmanstätten 3662: 3660: 3659:Neumann lines 3657: 3656: 3654: 3650: 3649:meteoric iron 3647: 3645: 3642: 3640: 3637: 3636: 3635: 3632: 3628: 3625: 3623: 3620: 3619: 3617: 3613: 3610: 3608: 3605: 3603: 3600: 3599: 3597: 3596: 3594: 3592: 3587: 3583: 3573: 3570: 3568: 3565: 3564: 3562: 3558: 3552: 3549: 3547: 3544: 3542: 3539: 3538: 3536: 3532: 3520: 3517: 3515: 3514:Eagle Station 3512: 3510: 3507: 3506: 3505: 3502: 3500: 3497: 3496: 3494: 3492: 3488: 3482: 3479: 3476: 3473: 3470: 3467: 3465: 3462: 3460: 3457: 3454: 3451: 3449: 3446: 3443: 3442: 3440: 3438: 3434: 3424: 3421: 3419: 3416: 3414: 3411: 3407: 3404: 3403: 3402: 3399: 3397: 3394: 3392: 3389: 3387: 3384: 3380: 3377: 3376: 3375: 3372: 3371: 3369: 3367: 3363: 3357: 3354: 3352: 3349: 3347: 3344: 3343: 3341: 3339: 3335: 3327: 3324: 3322: 3319: 3317: 3314: 3313: 3312: 3309: 3307: 3304: 3302: 3299: 3298: 3296: 3294: 3290: 3284: 3281: 3279: 3276: 3274: 3271: 3269: 3266: 3264: 3261: 3259: 3256: 3254: 3251: 3250: 3248: 3246: 3242: 3239: 3237: 3233: 3227: 3224: 3220: 3217: 3215: 3212: 3210: 3207: 3206: 3205: 3202: 3200: 3197: 3192: 3189: 3188: 3187: 3184: 3179: 3176: 3173: 3170: 3167: 3164: 3162: 3159: 3156: 3153: 3152: 3151: 3148: 3147: 3145: 3143: 3139: 3136: 3134: 3129: 3125: 3120: 3116: 3111: 3108: 3106: 3102: 3096: 3093: 3091: 3088: 3086: 3083: 3081: 3078: 3074: 3071: 3070: 3069: 3066: 3062: 3059: 3057: 3054: 3052: 3049: 3047: 3044: 3043: 3042: 3039: 3037: 3034: 3033: 3031: 3028: 3024: 3020: 3016: 3009: 3004: 3002: 2997: 2995: 2990: 2989: 2986: 2979: 2976: 2974: 2971: 2969: 2966: 2964: 2960: 2957: 2954: 2953: 2932: 2928: 2921: 2905: 2901: 2897: 2893: 2889: 2885: 2881: 2877: 2873: 2869: 2865: 2861: 2857: 2850: 2842: 2838: 2834: 2830: 2826: 2822: 2818: 2814: 2810: 2806: 2805: 2797: 2790:(in Spanish). 2789: 2782: 2774: 2770: 2766: 2762: 2758: 2755:(in German). 2754: 2747: 2731: 2727: 2723: 2719: 2712: 2696: 2692: 2686: 2677: 2661: 2657: 2653: 2647: 2639: 2635: 2631: 2627: 2623: 2619: 2618: 2610: 2602: 2598: 2594: 2590: 2586: 2582: 2578: 2574: 2567: 2559: 2555: 2550: 2545: 2541: 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1635: 1627: 1623: 1619: 1614: 1610: 1608: 1604: 1600: 1596: 1591: 1589: 1585: 1581: 1577: 1573: 1569: 1565: 1561: 1557: 1553: 1549: 1545: 1541: 1533: 1529: 1520: 1518: 1513: 1511: 1507: 1502: 1491: 1487: 1485: 1481: 1480:melting occur 1477: 1469: 1464: 1460: 1456: 1452: 1449: 1446: 1442: 1438: 1434: 1431: 1430: 1429: 1421: 1418: 1414: 1411: 1410: 1409: 1405: 1403: 1401: 1396: 1392: 1379: 1375: 1371: 1367: 1364: 1359: 1358: 1357: 1355: 1354: 1349: 1345: 1341: 1337: 1331: 1328: 1317: 1315: 1304: 1301: 1299: 1285: 1281: 1278: 1274: 1270: 1266: 1263: 1258: 1254: 1241: 1238: 1233: 1229: 1228: 1227: 1226: 1225: 1218: 1214: 1209: 1206: 1202: 1201: 1200: 1199: 1195: 1191: 1188: 1184: 1180: 1176: 1173: 1172: 1171: 1167: 1165: 1161: 1157: 1147: 1140: 1131: 1125: 1115: 1105: 1103: 1095: 1091: 1090:LL chondrites 1088: 1085: 1082: 1079: 1077: 1070: 1067: 1066: 1065: 1061: 1059: 1055: 1052: 1048: 1043: 1033: 1026: 1017: 1011: 1002: 996: 986: 976: 974: 970: 966: 962: 957: 951: 947: 943: 936: 928: 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These are 1455:metamorphism 1450: 1441:solar nebula 1432: 1426: 1419: 1412: 1406: 1398: 1394: 1390: 1388: 1353:fractionated 1351: 1332: 1323: 1310: 1302: 1294: 1223: 1168: 1154: 1099: 1084:L chondrites 1073: 1062: 1040: 958: 938: 923: 890:Rumurutiites 845: 831: 817: 803: 789: 770: 747: 729: 709: 504: 500: 495: 487: 485: 473: 437: 384: 311: 309: 296:metamorphism 293: 253: 225: 216: 194: 190:gravity well 182:Solar System 123: 121: 45: 3671:CI1 fossils 3567:Amphoterite 3551:Octahedrite 3546:Hexahedrite 3253:Acapulcoite 3180:C ungrouped 3095:Parent body 3019:meteoritics 2430:"Meteorlab" 2316:Meteoritics 1848:Meteoritics 1622:Smithsonian 1576:amino acids 1363:siderophile 1336:noble gases 1327:photosphere 1320:Composition 1284:Tagish Lake 1194:Ornans type 1164:amino acids 1104:meteorite. 1069:H chondrite 1058:rare earths 899:Plagioclase 860:Tagish Lake 496:(see below) 316:brecciation 232:achondrites 178:parent body 116:Over 27,000 94:Parent body 40:Chondrodite 3780:Categories 3612:weathering 3586:Mineralogy 3534:Structural 3509:Main group 3491:Stony-iron 3293:Asteroidal 3258:Brachinite 3236:Achondrite 3056:statistics 3015:Meteorites 2322:(3): 460, 1944:30 October 1773:References 1684:Achondrite 1599:radiolysis 1584:chloroform 1532:Amino acid 1400:petrologic 1370:refractory 1298:refractory 1144:NWA 13887 1094:oligoclase 1054:lithophile 1051:refractory 1016:Phnom Penh 942:Antarctica 798:CO3–CO3.7 764:CV2–CV3.3 688:Indistinct 667:LL3–LL3,9 645:Indistinct 602:Indistinct 554:Indistinct 469:shock wave 465:mineralogy 441:refractory 387:chondrules 355:Chondrules 283:and other 277:atmosphere 211:(from the 209:chondrules 73:chondrules 18:Chondritic 3760:Meteoroid 3725:See also: 3655:Patterns 3622:chondrule 3591:petrology 3504:Pallasite 3396:Nakhlites 3326:Howardite 3316:Diogenite 3283:Winonaite 3273:Lodranite 3245:Primitive 3199:Kakangari 3186:Enstatite 3142:Chondrite 3051:impactite 3027:Meteorite 2833:0169-6149 2773:0009-2851 2152:0213-683X 2146:: 35–38. 2139:Geogaceta 2028:: 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1314:regolith 1269:Karoonda 1257:Vigarano 1237:volatile 1231:process. 1179:oxidized 1047:troilite 903:Sulfides 848:igh Iron 820:encubbin 781:, metals 779:Pyroxene 741:CM1–CM2 672:Distinct 664:Abundant 629:Distinct 624:L3–L3,9 621:Abundant 586:Distinct 581:H3–H3,9 578:Abundant 538:Distinct 530:Abundant 514:Subtype 449:sulfides 399:pyroxene 391:silicate 273:volatile 217:chondros 215:χόνδρος 162:metallic 3618:Grains 3541:Ataxite 3366:Martian 3321:Eucrite 3306:Aubrite 3301:Angrite 3090:Notable 3080:Largest 3073:hunting 2900:4147981 2892:5482102 2872:Bibcode 2841:2045303 2813:Bibcode 2626:Bibcode 2601:4295051 2581:Bibcode 2528:Bibcode 2354:Bibcode 2324:Bibcode 2298:Bibcode 2296:: 169, 2263:Bibcode 2217:Bibcode 2092:6 March 2066:6 March 2030:Bibcode 2003:13 July 1973:Bibcode 1891:Axxón. 1856:Bibcode 1642:alanine 1638:glycine 1552:ketones 1391:primary 1262:Allende 1217:Renazzo 1102:NWA 869 973:Mercury 961:reduced 834:oongana 806:aroonda 750:igarano 737:Olivine 476:Jupiter 395:olivine 337:planets 287:in our 279:of the 244:Arizona 176:of the 170:melting 3753:shower 3748:Meteor 3702:Awards 3391:Kaidun 3046:bolide 2898: 2890: 2864:Nature 2839: 2831: 2771: 2599: 2573:Nature 2556: 2475:1 July 2235: 2150: 1991: 1930: 1903:11 May 1876: 1797:19 May 1564:amides 1560:amines 1517:comets 1476:type 7 1433:Type 3 1420:Type 2 1413:Type 1 1346:(Ne), 1342:(He), 1340:helium 1160:carbon 965:oxygen 952:(MgSiO 894: 881: 878: 773:enazzo 696:Melted 653:Melted 610:Melted 562:Melted 457:matrix 373:meteor 289:galaxy 221:molten 199:, the 3738:Comet 3680:Lists 3602:shock 3468:IIIAB 3338:Lunar 3268:IIICD 3128:group 3119:class 2896:S2CID 2837:S2CID 2597:S2CID 2554:S2CID 2233:S2CID 2207:arXiv 1989:S2CID 1726:Notes 1470:form. 1348:argon 1074:(see 969:orbit 929:(EH5) 875:-type 792:rnans 732:ighei 511:Type 488:(see 285:stars 265:Pb/Pb 236:Jilin 205:Earth 87:Stony 3695:type 3589:and 3474:IIIF 3471:IIIE 3448:IIAB 3437:Iron 3356:List 3131:and 3124:clan 3115:type 3068:Find 3041:Fall 3017:and 2939:2009 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