LL Chondrites

LL Chondrites form one of the three types of Ordinary Chondrites (being L, LL, & H). LL Chondrites the least abundant group of Ordinary Chondrites, accounting for about 10-11% of observed Ordinary-Chondrite falls and 8-9% of all meteorite falls.

LL Chondrites are a less common group of Ordinary Chondrite meteorites, characterised by their ‘low iron, low metal’ composition. Compared to H and L Chondrites, they contain the least amount of metallic iron, with most of their iron bound within silicate minerals. Formed over 4.5 billion years ago, LL Chondrites originated from primitive asteroid material that has undergone varying degrees of thermal metamorphism, preserving early solar system components alongside evidence of internal heating.

LL Chondrites typically display a lighter grey to brown interior with clearly visible chondrules when cut and polished. Due to their low metal content, they have a more uniform, less reflective appearance, with fewer metallic flecks than other Ordinary Chondrites. Their outer surface, when fresh, is covered by a dark fusion crust formed during atmospheric entry. In many cases, their well-defined chondrules make them especially attractive for study and display.

Studying LL Chondrites provides valuable insight into the range of compositions and conditions present in the early solar system. They are particularly important for understanding how variations in metal content influenced the evolution of asteroid parent bodies. For collectors, LL Chondrites are highly desirable due to their relative rarity within the Ordinary Chondrite groups and their clearly visible structures. Each specimen represents a distinctive example of primitive solar system material, offering both scientific value and visual appeal.