The Chondrites are undifferentiated meteorites that have not been modified due to melting or differentiation of the parent body. They are formed when various types of dust, water ice, small mineral grains, chondrules and chondrule fragments present in the early solar system accreted to form primitive asteroids. They are the most common type of meteorite that falls to Earth with estimates for the proportion of the total fall that they represent varying between 85.7% and 86.2%, with most of those chondrites being equilibrated ordinary chondrites, often referred to as simply ordinary chondrites (OC) or equilibrated chondrites (EC). The Ordinary Chondrites come in three types (LL, L, and H) depending on the iron content of their olivine and pyroxene. Each of these three types are then given petrological grades between 3 and 7 depending on how equilibrated they are, with 3 being the least equilibrated and 7 being the most equilibrated. There are several less common types of chondrites including; Carbonaceous Chondrites (C), Enstatite Chondrites (E), Rumuruti-like Chondrites (R), and Kakangari-like Chondrites (K). The study of the ordinary chondrites and the other types of chondrites provides important clues for understanding the origin and age of the Solar System, the synthesis of organic compounds, the origin of life, and how Earth got its water. One of the key characteristics of the chondrites is the presence of chondrules, which are complex spherical mineral grains, often glassy and having gone through multiple rapid heating events. Chondrules typically constitute between 20% and 80% of a chondrite by volume.

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