Stony meteorites

Choose from more than 900 stony meteorites from locations around the world – from affordable chondrites to rare lunar, Martian and other achondritic meteorites. Each product includes its exact weight, origin and photographs. Unless random selection is specified, you will always receive the exact specimen shown.

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What are stony meteorites?

Stony meteorites are the most abundant group of meteorites. They consist mainly of silicate minerals such as olivine, pyroxenes and plagioclase. They may also contain smaller amounts of iron-nickel metal and other mineral components.

According to the structure and history of their parent bodies, stony meteorites are divided into two main groups: chondrites and achondrites.

Chondrites and chondrules

Chondrites are very ancient meteorites that have generally not undergone extensive melting or differentiation since their formation. They therefore preserve information about the earliest history of the Solar System and are approximately 4.5 billion years old.

A characteristic feature of many chondrites is the presence of chondrules – small spherical structures composed mainly of silicate minerals. They formed through the rapid cooling of molten droplets of material before the planets were created.

Main groups of chondrites

Ordinary chondrites (H, L and LL)
The most common group of meteorites. The individual types differ mainly in their total iron content and the amount of iron-nickel metal.

• H chondrites – higher iron and metal content
• L chondrites – lower iron content
• LL chondrites – low iron and metal content

Carbonaceous chondrites (CI, CM, CO, CV, CR, CH and CB)
Rare and scientifically important meteorites. Some contain organic compounds, hydrated minerals and material preserved from the early Solar System.

Enstatite chondrites (EH and EL)
Meteorites rich in the mineral enstatite that formed under conditions with very little available oxygen.

Achondrites

Achondrites are stony meteorites that generally do not contain chondrules. They originate from parent bodies that underwent heating, melting and differentiation. Their structure may therefore resemble that of terrestrial igneous rocks.

HED meteorites

HED meteorites include howardites, eucrites and diogenites. Based on their mineralogical and chemical composition, they most likely originate from the asteroid Vesta.

• Howardites – mixtures of material similar to eucrites and diogenites
• Eucrites – rocks formed mainly from basaltic lava
• Diogenites – intrusive rocks rich mainly in pyroxenes

Martian meteorites

Martian meteorites were ejected from the surface of Mars by large impacts and later fell to Earth. They include mainly shergottites, nakhlites and chassignites.

Their origin was determined by comparing their chemical and isotopic composition with data obtained during the exploration of Mars.

Lunar meteorites

Lunar meteorites originate from the surface of the Moon. They were ejected into space by the impact of another object, and some of this material later fell to Earth.

They may represent lunar basalts, rocks from the lunar highlands or mixtures of different rocks known as breccias.

Other achondrites

Other achondrites include aubrites, ureilites and angrites. The individual groups differ considerably in their chemical and mineralogical composition and originate from various bodies within the Solar System.

How to choose a stony meteorite

Affordable ordinary chondrites are particularly suitable for beginning collectors. Cut and polished specimens make it easier to observe the internal structure, chondrules and metallic particles.

Rarer achondrites, lunar meteorites and Martian meteorites are suitable for advanced collectors or as an exceptional gift. When choosing a specimen, we recommend considering its classification, locality, weight, type of preparation and the history of its find or fall.