Carbonaceous chondrites are among the most scientifically important meteorites known. They are primitive stony meteorites that have undergone little to no melting since their formation in the early Solar System, preserving a direct record of its earliest materials and processes.
These meteorites are characterized by their high content of volatile elements, hydrated minerals, and organic compounds. Many carbonaceous chondrites contain water-bearing minerals, complex organic molecules, and, in some cases, amino acids, making them central to studies of the origin of water and prebiotic chemistry on Earth.
Carbonaceous chondrites are subdivided into several distinct groups (CI, CM, CO, CV, CK, CR, CH, CB), each reflecting differences in mineralogy, degree of aqueous alteration, and thermal history. Some groups, such as CI and CM chondrites, are extremely fine-grained and rich in phyllosilicates formed through interaction with liquid water on their parent bodies. Others, such as CV and CO chondrites, preserve refractory inclusions and chondrules that formed at high temperatures in the solar nebula.
Unlike most meteorites, carbonaceous chondrites often display unusual fusion crusts, sometimes brown, greenish, or unevenly developed, reflecting their low iron content and the presence of hydrated phases. Their interiors are typically dark, fragile, and heterogeneous, emphasizing their primitive nature.
Because of their rarity, fragility, and extraordinary scientific value, carbonaceous chondrites are highly sought after by researchers and advanced collectors alike. Each specimen provides a unique window into the chemical and mineralogical conditions that prevailed during the formation of planets.
