Tatahouine Diogenite Stony Meteorite Achondrites Specimen Fell June 24, 1931 Display
Location: Tunisia
Weight: 0.4 Ounces (Display)
Dimensions: 2.3 Inches Long, 1.5 Inches Wide, 0.6 Inches Thick (Display)
Comes with a Free Display Case.
The item pictured is the one you will receive.
Tatahouine Diogenite is a meteorite classified as an achondrite, a type of stony meteorite that has undergone differentiation and crystallization processes similar to those occurring in planetary bodies. Diogenites are specifically believed to originate from asteroid 4 Vesta, one of the largest objects in the asteroid belt. Studying these meteorites helps scientists understand the formation and early evolution of the solar system.
Diogenites are primarily composed of orthopyroxene, a mineral rich in iron and magnesium, which gives them their characteristic dark color and dense structure. They may also contain other minerals such as olivine, plagioclase, and various metallic phases. Variations in mineral composition among individual specimens reflect differences in cooling histories and processes on their parent body.
The texture of diogenites is typically coarse-grained due to slow cooling rates during their formation. This slow cooling allows for the growth of larger crystals compared to other types of meteorites. Some diogenites exhibit a cumulate texture, indicating that they formed from the accumulation of crystals settling out from a molten state.
Tatahouine Diogenite is an achondrite meteorite believed to originate from asteroid 4 Vesta, one of the largest bodies in the asteroid belt. Diogenites formed from differentiated basaltic magma on Vesta’s surface. As the asteroid cooled, heavier minerals like orthopyroxene crystallized first and settled toward the bottom of magma chambers. Subsequent impacts on Vesta excavated these rocks, sending fragments into space that eventually reached Earth.
Diogenites are primarily composed of orthopyroxene, giving them a dark color and dense structure. They may also contain olivine, plagioclase, and metallic phases. Many specimens exhibit a coarse-grained texture, reflecting slow cooling and crystal growth, while some show a cumulate texture, indicating the accumulation of early-formed crystals in magma.
These meteorites provide crucial insight into planetary differentiation, revealing how celestial bodies separate into layers based on density, and offering a window into the conditions of the early solar system.
Diogenites belong to the HED (Howardite-Eucrite-Diogenite) meteorite group, alongside eucrites, which are basaltic rocks from Vesta with different mineral compositions, and howardites, which are mixtures of eucrite and diogenite material. This classification allows researchers to trace the origins and evolutionary history of these meteorites and better understand the formation of other bodies in our solar system.
