Chelyabinsk Meteorite, 2.182 grams
In the early morning hours of February 15, 2013, a brilliant streak of light illuminated the skies over the Russian city of Chelyabinsk. What initially appeared to be a celestial spectacle quickly turned into a terrifying event as a meteorite, traveling at an estimated speed of 42,900 miles per hour, exploded in the Earth’s atmosphere with a force nearly thirty times that of the Hiroshima atomic bomb.
The Chelyabinsk meteorite, weighing around 10,000 metric tons and measuring approximately 20 meters in diameter, originated from the asteroid belt between Mars and Jupiter. It entered Earth’s atmosphere at an angle of about 20 degrees, creating a blinding flash and a shockwave that shattered windows, damaged buildings, and injured over 1,500 people. The explosion generated a powerful airburst, releasing energy equivalent to approximately 440-500 kilotons of TNT.
Witnesses described a brilliant fireball streaking across the sky, leaving a long smoke trail in its wake. The sonic boom that followed shattered glass, causing injuries from flying debris. The event was captured by numerous dashboard cameras, security cameras, and smartphones, providing a wealth of footage that documented the meteorite’s dramatic entry and subsequent explosion.
The shockwave produced by the explosion caused widespread damage in Chelyabinsk and surrounding areas. Thousands of windows were shattered, and buildings suffered structural damage. Fortunately, no fatalities were reported, but the event served as a stark reminder of the potential danger posed by near-Earth objects.
Scientists quickly mobilized to study the Chelyabinsk meteorite, which had fragmented into countless smaller pieces upon explosion. Recovery efforts focused on collecting meteorite fragments scattered across the region. These fragments provided valuable insights into the meteorite’s composition and origin.
Analysis revealed that the Chelyabinsk meteorite was a type of stony meteorite known as a chondrite. Chondrites are among the most primitive objects in the solar system, containing minerals and compounds that have remained largely unchanged since the formation of the solar system over 4.6 billion years ago.
The Chelyabinsk meteorite’s impact highlighted the need for improved detection and tracking of near-Earth objects to mitigate the risk of future impacts. While events like the Chelyabinsk meteorite are rare, they serve as a reminder of the potential threat posed by asteroids and comets. In the years following the Chelyabinsk event, efforts to detect and track near-Earth objects have intensified. Ground-based observatories and space-based telescopes continuously scan the skies for potential threats, providing early warning of any objects on a collision course with Earth.
The Chelyabinsk meteorite remains a significant event in the study of planetary science and the ongoing efforts to understand and protect our planet from the hazards of space. Its dramatic entry into Earth’s atmosphere serves as a reminder of the dynamic and sometimes unpredictable nature of our cosmic neighborhood.
Stony Meteorites, which are the most abundant kind of meteorite, are divided into two groups: chondrites and achondrites. Chondrites are physically and chemically the most primitive meteorites in the solar system.
This great NWA Meteorite is from an unclassified find in 2005. Stonies are the most common of all meteorites and contain chondrules and iron flecks within. The Northwest Africa specimen has a nice fusion crust exterior. NWA meteorites are an affordable way to start of fine collection of extraterrestrial rocks.
Comprising approximately 95% of all 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.
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 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 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.
Prehistoric 101 (Learn about fossils, minerals, and meteorites)
What is a Meteorite? Nickel Iron
What is a Meteorite?
The Meteoritical Society Database
The Chelyabinsk Meteor: an Earth-shaking Cosmic Event
