EL Melt Rock
(EL7 in MetBull 71; Primitive Used in past as synonym for Aubrites. Present definition from the Meteoritical Bulletin states that this rare class is an "enstatite-rich achondrite that has not yet been classified into a group". [Pilski et al., 2011])
(ELa7 in Weyrauch et al., 2018)
Found October 1989
21° 38′ N., 1° 16′ E. A single, relatively fresh (W0/1) stone weighing 421 g was found in the Algerian Sahara Desert. From initial chemical and petrologic analyses of Ilafegh 009, it was determined that the Work in progress. A solid natural object reaching a planet’s surface from interplanetary space. Solid portion of a meteoroid that survives its fall to Earth, or some other body. Meteorites are classified as stony meteorites, iron meteorites, and stony-iron meteorites. These groups are further divided according to their mineralogy and was a highly metamorphosed Type of meteorite high in the mineral enstatite and also referred to as E-chondrites. Although they contain substantial amounts of Fe, it is in the form of Ni-Fe metal or sulfide rather than as oxides in silicates. Their highly reduced nature indicates that they formed in an area of the consistent with a classification of EL6/7 (Otto, 1992). Subsequent analyses by Bischoff et al. (1992) and McCoy et al. (1995) verified its genetic relationship to the EL Chondrites are the most common meteorites accounting for ~84% of falls. Chondrites are comprised mostly of Fe- and Mg-bearing silicate minerals (found in both chondrules and fine grained matrix), reduced Fe/Ni metal (found in various states like large blebs, small grains and/or even chondrule rims), and various refractory inclusions (such group, and brought to light its unique igneous texture reflecting both Igneous rock composed of crystals that have grown and accumulated (often by gravitational settling) in a cooling magma chamber. and granoblastic characteristics, as well as its unusually large-sized A mineral that is composed of Mg-rich pyroxene, MgSiO3. It is the magnesium endmember of the pyroxene silicate mineral series - enstatite (MgSiO3) to ferrosilite (FeSiO3). crystals (up to 0.75 cm) that impart a lighter color to the whole rock than is typically apparent in E Chondrites are the most common meteorites accounting for ~84% of falls. Chondrites are comprised mostly of Fe- and Mg-bearing silicate minerals (found in both chondrules and fine grained matrix), reduced Fe/Ni metal (found in various states like large blebs, small grains and/or even chondrule rims), and various refractory inclusions (such. Ilafegh 009 is considered by some to be a total shock-melted rock from the EL chondrite The body from which a meteorite or meteoroid was derived prior to its ejection. Some parent bodies were destroyed early in the formation of our Solar System, while others like the asteroid 4-Vesta and Mars are still observable today..
|ENSTATITE CHONDRITE SUBGROUPS
Weyrauch et al., 2018
|Troilite||Cr <2 wt%||Cr >2 wt%||Cr <2 wt%||Cr >2 wt%|
|(Mn,Mg,Fe)S||Fe <20 wt%||Fe >20 wt%||Fe <20 wt%||Fe >20 wt%|
|Kamacite||Ni <6.5 wt%||Ni >6.5 wt%||Ni <6.5 wt%||Ni >6.5 wt%|
A few other E chondrites with intermediate mineralogy have also been identified, including LAP 031220 (EH4), QUE 94204 (EH7), Y-793225 (E-an), LEW 87223 (E-an), and PCA 91020 (possibly related to LEW 87223). Studies have determined that these meteorites were not derived from the EH or EL source through any Rocks that have recrystallized in a solid state due to changes in temperature, pressure, and chemical environment. processes, and some or all of them could represent separate E chondrite asteroids. The revised E chondrite classification scheme of Weyrauch et al. (2018) including selected examples from their 80-sample study can be found here. It was determined that Ilafegh 009 is a member of the ELa subgroup.It has been suggested that Ilafegh 009 crystallized from a superheated impact-induced melt (peak pressures >75 GPa), and then was rapidly cooled from peak temperatures of ~5000°C/m.y. (McCoy et al., 1992). The Ar–Ar age of Ilafegh 009 was calculated to be 4.43 b.y., while an older I–Xe age of ~4.565 b.y. indicates this chronometer was not reset (Bogard et al., 2010). This petrogenetic scenario is consistent with the appearance of unfractionated Element that readily forms cations and has metallic bonds; sometimes said to be similar to a cation in a cloud of electrons. The metals are one of the three groups of elements as distinguished by their ionization and bonding properties, along with the metalloids and nonmetals. A diagonal line drawn and sulfide, and the occurrence of magmatic inclusions within enstatite crystals. The large size of these crystals indicates that all of the original enstatite nuclei were eradicated in the superheated melt. At the same time, all of the trapped Noble gas represented by the atomic symbol Ar, that has Z = 18, and an atomic weight of 39.948. It is colorless, odorless, and very inert gas, comprising ~1 % of the Earth's atmosphere. and many other Chemical elements that condense (or volatilize) at relatively low temperatures. The opposite of volatile is refractory. Volatile elements can be divided into moderately volatile (Tc = 1230–640 K) and highly volatile (Tc < 640 K). The moderately volatile lithophile elements are: Mn, P, Na, B ,Rb, K, F, Zn. The moderately were degassed during this event. The Physical or chemical process or action that results in the formation of regularly-shaped, -sized, and -patterned solid forms known as crystals. sequence of the melt is believed to have been enstatite ⇒ plagioclase ⇒ Silicon dioxide, SiO2. ⇒ FeNi-metal/sulfides. The mineral sinoite has also been identified, which is associated with crystallization of an impact melt. Very fine-grained (few µm-sized), rounded, magmatic inclusions have been identified within the cores and rims of enstatites (Leroux et al., 1997). The inclusions consisting of plagioclase + metal + troilite are present in the cores, while those consisting of silica-rich glass (both K-rich and K-poor) are found in the enstatite rims as well as interstitially throughout the enstatite and plagioclase host grains—findings that are consistent with the proposed crystallization sequence. Besides these inclusions, undeveloped orthoenstatite nuclei are present within enstatite host grains. It is considered that following solidification, the Ilafegh 009 lithology was impact-shocked to stage S4, as indicated by undulatory In astronomy, the dimming of starlight as it passes through the interstellar medium. Dust scatters some of the light, causing the total intensity of the light to diminish. It is important to take this effect into account when measuring the apparent brightness of stars. The dark bands running across portions, moderate mosaicism, and planar fractures in the Orthorhombic, low-Ca pyroxene common in chondrites. Its compositional range runs from all Mg-rich enstatite, MgSiO3 to Fe-rich ferrosilite, FeSiO3. These end-members form an almost complete solid solution where Mg2+ substitutes for Fe2+ up to about 90 mol. % and Ca substitutes no more than ~5 mol. % (higher Ca2+ contents occur grains. In addition, microscopic striations are present in some A class of silicate (SiO3) minerals that form a solid solution between iron and magnesium and can contain up to 50% calcium. Pyroxenes are important rock forming minerals and critical to understanding igneous processes. For more detailed information, please read the Pyroxene Group article found in the Meteoritics & Classification category. lamellae that were formed by the intergrowth of orthoenstatite and clinoenstatite phases resulting from shock (McCoy et al., 1995). In contrast to Ilafegh 009, the impact-melt derived EL chondrite Happy Canyon did not experience temperatures to the same high degree, as concluded from the presence in Happy Canyon of a fine-grained lithology, considered to result from crystallization sustained by pre-existing enstatite nuclei. Happy Canyon was also cooled more rapidly due to the incorporation of cold clastic material, which eventually solidified to form a Work in Progress ... A rock that is a mechanical mixture of different minerals and/or rock fragments (clasts). A breccia may also be distinguished by the origin of its clasts: (monomict breccia: monogenetic or monolithologic, and polymict breccia: polygenetic or polylithologic). The proportions of these fragments within the unbrecciated material. In addition, Happy Canyon experienced less severe post-solidification shock than Ilafegh 009. Nevertheless, Pilski et al. (2011) propose that Ilafegh 009 may more properly be classified with Zakłodzie, and perhaps Happy Canyon, QUE 94204, and Y-8404, as a primitive enstatite An achondrite is a type of stony meteorite whose precursor was of chondritic origin and experienced metamorphic and igneous processes. They have a planetary or differentiated asteroidal origin where the chondritic parent body reached a sufficient size that through heating due to radioactive decay of 26Al (aluminum isotope) and gravitational representing the residue from the rapid An igneous process whereby rocks melt and the resulting magma is comprised of the remaining partially melted rock (sometimes called restite) and a liquid whose composition differs from the original rock. Partial melting occurs because nearly all rocks are made up of different minerals, each of which has a different melting of an enstatite chondrite parent body. In their advanced microscopic analyses of Ilafegh 009, Boesenberg et al. (2014) proposed a slightly different two-stage petrogenetic history. The first stage in their scenario involves formation as a melt rock, after which it would resemble the other fine-grained, granular-textured EL chondrites such as Zakłodzie and Happy Canyon. They invoke a subsequent heating event that resulted in the re-orientation and sintering (and/or Ostwald ripening) of these small enstatite grains into a coarse-grained, crystallographically-contiguous texture. The O-isotopes for Ilafegh 009 plot with the E chondrites and Aubrites are named for the Aubres meteorite that fell in 1836 near Nyons, France. They are an evolved achondrite that is Ca-poor and composed mainly of enstatite (En100) and diopside (En50Wo50) with minor amounts of olivine (Fa0) and traces of plagioclase (An2-8). They contain large white crystals of enstatite as. Interestingly, I–Xe radiochronometry demonstrates that Ilafegh 009, Happy Canyon, and the anomalous Aubrites are named for the Aubres meteorite that fell in 1836 near Nyons, France. They are an evolved achondrite that is Ca-poor and composed mainly of enstatite (En100) and diopside (En50Wo50) with minor amounts of olivine (Fa0) and traces of plagioclase (An2-8). They contain large white crystals of enstatite as Shallowater all share similar closure times for radiogenic xenon in the iodine host enstatite phase at ~4.565 b.y. ago. This suggests that each meteorite experienced essentially concurrent episodes of an I–Xe clock-resetting, impact-melting event in a common formation region (Kehm et al., 1993). The younger K–Ar age calculated for Ilafegh 009 of 4.34–4.44 b.y. may represent subsequent thermal resetting by impact, while the K–Ar age of 4.53 b.y. calculated for both Happy Canyon and Shallowater may reflect the actual closure of this particular chronometric Definable part of the universe that can be open, closed, or isolated. An open system exchanges both matter and energy with its surroundings. A closed system can only exchange energy with its surroundings; it has walls through which heat can pass. An isolated system cannot exchange energy or matter with during metamorphic cooling following Accumulation of smaller objects into progressively larger bodies in the solar nebula leading to the eventual formation of asteroids, planetesimals and planets. The earliest accretion of the smallest particles was due to Van der Waals and electromagnetic forces. Further accretion continued by relatively low-velocity collisions of smaller bodies in the. The specimen shown above is a 1.55 g partial slice of Ilafegh 009, which highlights the metallic component of this meteorite. It was originally part of a 25.5 g partial slice in the collection of JNMC–Zurich (see photo below). The middle portion shown is being utilized for further Thin slice or rock, usually 30 µm thick. Thin sections are used to study rocks with a petrographic microscope. studies.
Photo courtesy of JNMC–Zurich