Djoumine meteorite, Chondrite H5-6, Morocco Prehistoric Online
Djoumine meteorite, Chondrite H5-6, Morocco Prehistoric Online
Djoumine meteorite, Chondrite H5-6, Morocco Prehistoric Online
Djoumine meteorite, Chondrite H5-6, Morocco Prehistoric Online
Djoumine meteorite, Chondrite H5-6, Morocco Prehistoric Online

Djoumine meteorite, Chondrite H5-6, Morocco

Type: Chondrite H5-6
Find: Oct 31, 1999
TKW: 10kg
Country: Banzart, Tunisia
Weight: 0.119g

$25.95

SKU: or-stony-djoumine

Availability: Only 1 left in stock

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The Djoumine meteorite is a remarkable specimen that fell to Earth in Tunisia in 1999, specifically near the town of Djoumine. This meteorite, classified as an H5 ordinary chondrite, has captivated scientists and enthusiasts alike with its intriguing characteristics.

Belonging to the H5 group, the Djoumine meteorite is composed of abundant chondrules, small spherical grains formed during the early stages of the solar system’s evolution. These chondrules provide valuable insights into the conditions prevailing during the formation of our solar system over 4.5 billion years ago.

 

Studying the Djoumine meteorite offers scientists a window into the past, providing clues about the processes that shaped our solar system. By analyzing its mineralogy, isotopic composition, and organic content, researchers can unravel mysteries about the origins of celestial bodies and the building blocks of life.

The recovery and analysis of the Djoumine meteorite underscore the importance of meteorite studies in advancing our understanding of planetary science. These extraterrestrial specimens serve as tangible remnants of cosmic events, preserving invaluable information about the early history of our solar system.

Moreover, the Djoumine meteorite holds cultural significance, particularly for the local community near its landing site. Its discovery and subsequent study have sparked interest in astronomy and planetary science, inspiring curiosity and wonder among residents and visitors alike.

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.

Djoumine meteorite, Chondrite H5-6, Morocco

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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