Mount Egerton meteorite, Aubrite-an, Australia Prehistoric Online
Mount Egerton meteorite, Aubrite-an, Australia Prehistoric Online
Mount Egerton meteorite, Aubrite-an, Australia Prehistoric Online
Mount Egerton meteorite, Aubrite-an, Australia Prehistoric Online
Mount Egerton meteorite, Aubrite-an, Australia Prehistoric Online

Mount Egerton meteorite, Aubrite-an, Australia

Mount Egerton meteorite
Type: Aubrite-an
Find: 1941
TKW: 22kg
Country: Western Australia
Weight: 0.097g


SKU: or-stony-mtegerton

Availability: Only 1 left in stock

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Mount Egerton is renowned for yielding a rare type of meteorite known as Aubrites. These meteorites originate from a larger parent body, likely an asteroid, and are named after the Aubres meteorite, which fell in France in 1836. Mount Egerton, located in Victoria, Australia, has been a significant site for Aubrite-an meteorite discoveries.

Aubrites are primarily composed of minerals such as enstatite and olivine, making them chemically distinct from most other meteorite types. They often exhibit a coarse-grained texture, with angular crystals embedded in a fine-grained matrix. This unique composition suggests that Aubrites formed under extremely reducing conditions, likely in the early solar system.

The Mount Egerton Aubrites are of particular interest to scientists because of their pristine nature. They have undergone minimal alteration since their formation, providing valuable insights into the conditions present in the early solar system. By studying these meteorites, researchers can better understand processes such as planetary differentiation and the formation of asteroids.

One notable feature of Aubrites is the presence of metallic inclusions, predominantly composed of iron and nickel. These inclusions are thought to represent remnants of the parent body’s core, suggesting that Aubrites originated from a differentiated asteroid that underwent partial melting and segregation of its constituents.

The discovery of Aubrites at Mount Egerton dates back to the late 19th century, with numerous specimens being recovered from the region over the years. Meteorite hunters and researchers continue to explore the area in search of new specimens, adding to our understanding of these enigmatic objects.
Mount Egerton meteorite, Aubrite-an, Australia
Studying Aubrites also provides insights into the thermal and chemical history of the early solar system. By analyzing their isotopic compositions and mineralogy, scientists can infer the processes that occurred during their formation and subsequent evolution.

Stony Meteorites: Witness to Stellar Birth

Comprising approximately 95% of all meteorite falls, stony meteorites, as the name suggests, are primarily composed of silicate minerals. Within this group, there are further subdivisions based on mineral composition and texture, such as chondrites, achondrites, and carbonaceous chondrites.

Chondrites: Among the most common type of meteorites, chondrites are primitive remnants of the early solar system, dating back over 4.5 billion years. They contain small spherical structures called chondrules, which are believed to have formed in the protoplanetary disk around the young Sun. These chondrules are composed of minerals like olivine and pyroxene, encapsulating the conditions of the nascent solar system. The study of chondrites provides valuable information about the processes of planetary accretion and differentiation.

Mount Egerton meteorite, Aubrite-an, Australia

Achondrites: Unlike chondrites, achondrites lack chondrules and exhibit evidence of igneous processing, indicating that they originated from larger planetary bodies with internal differentiation. These meteorites often resemble terrestrial rocks, with mineral compositions similar to basalts and gabbros found on Earth. Achondrites are thought to originate from the crust or mantle of differentiated bodies such as asteroids or even Mars. By analyzing the mineralogy and isotopic signatures of achondrites, scientists gain insights into the geological history and differentiation processes of planetary bodies beyond Earth.

Carbonaceous Chondrites: Renowned for their high carbon content and volatile-rich composition, carbonaceous chondrites are among the most primitive meteorites, containing complex organic molecules and water-bearing minerals. These meteorites offer tantalizing clues about the conditions that prevailed in the early solar system, including the delivery of water and prebiotic molecules to Earth. Scientists believe that carbonaceous chondrites may have played a crucial role in seeding the primordial Earth with the necessary ingredients for life.

Iron Meteorites: Relics of Cosmic Cores

Comprising about 5% of meteorite falls, iron meteorites stand out for their high iron and nickel content, often accompanied by traces of other elements like cobalt and phosphorus. These meteorites are remnants of the cores of differentiated bodies such as asteroids or protoplanets, where intense heat and pressure led to the segregation of metallic alloys.

Octahedrites: Characterized by a distinctive crystalline structure known as a Widmanstätten pattern, octahedrites are the most common type of iron meteorites. This pattern forms as a result of slow cooling over millions of years within the core of a planetary body, allowing nickel-iron crystals to grow into elongated shapes. The presence of the Widmanstätten pattern serves as a signature of extraterrestrial origin and provides insights into the cooling rates and thermal histories of parent bodies.

Hexahedrites: Unlike octahedrites, hexahedrites exhibit a cubic crystal structure and are relatively rare compared to their octahedral counterparts. These meteorites likely formed under different cooling conditions within the cores of larger asteroids or protoplanets. The study of hexahedrites helps scientists understand the diversity of parent bodies in the early solar system and the processes that governed their differentiation.

Ataxites: Ataxites represent a minor subclass of iron meteorites characterized by their high nickel content and lack of a distinct crystalline structure. These meteorites likely originated from the outer regions of planetary cores, where nickel concentrations were higher. The study of ataxites provides valuable information about the chemical composition and thermal evolution of parent bodies, offering clues about the conditions prevailing in the early solar system.

Stony-Iron Meteorites: Bridging the Divide

Stony-iron meteorites, as the name implies, represent a hybrid of stony and iron compositions, with roughly equal proportions of silicate minerals and metallic alloys. These meteorites are thought to originate from the boundary regions between a differentiated body’s mantle and core, where material mixing occurred due to impacts or geological processes.

Pallasites: Gem embedded Nickel Iron:

Pallasites: Pallasites are one of the most visually striking meteorite types, characterized by their beautiful olivine crystals embedded in a metallic matrix. These meteorites likely formed at the interface between the core and mantle of differentiated bodies, where molten metal percolated through fractures and filled cavities within the silicate matrix. The study of pallasites provides insights into the dynamics of core-mantle interactions and the mixing of materials in the early solar system.

Mesosiderites: Mesosiderites are stony-iron meteorites composed of roughly equal parts of silicate minerals and metallic alloys. Unlike pallasites, which exhibit a distinct separation of metal and silicate phases, mesosiderites show evidence of intense brecciation and mixing, indicating violent processes within the parent body. These meteorites likely originated from the crust or mantle of large differentiated bodies, where impacts or tectonic activity led to the commingling of materials.

IAB Irons: IAB iron meteorites represent a transitional group between iron and stony-iron meteorites, exhibiting a mixture of metallic alloys and silicate inclusions. These meteorites often contain complex textures and mineral compositions, suggesting a heterogeneous parent body with a history of geological activity and differentiation. The study of IAB irons provides valuable insights into the processes of planetary formation and differentiation in the early solar system.

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Weight 5 oz
Dimensions 6 × 5 × 3 in
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