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 type of meteorite classified within the group of achondrites, which are stony meteorites that have undergone differentiation and crystallization processes similar to those that occur in planetary bodies. Specifically, diogenites are believed to originate from the asteroid 4 Vesta, one of the largest bodies in the asteroid belt. This classification is part of a broader understanding of meteorites and their origins, which provides insights into the early solar system's formation and evolution.
Diogenites are primarily composed of orthopyroxene, a mineral rich in iron and magnesium, which gives these meteorites their characteristic dark color and dense structure. In addition to orthopyroxene, diogenites may contain olivine, plagioclase, and various metallic phases. The specific mineralogical composition can vary between specimens, reflecting differences in cooling histories or parent body processes.
The texture of diogenites is typically coarse-grained, resulting from slow cooling rates during formation. This slow cooling allows larger crystals to develop compared to other meteorites. Some diogenites exhibit a cumulate texture, indicating they formed from the accumulation of crystals settling out of molten magma.
Diogenites are closely linked to the geological history of asteroid 4 Vesta. They are thought to have formed from differentiated basaltic magma on Vesta’s surface. As the magma cooled, heavier minerals like orthopyroxene crystallized first and settled to the bottom of magma chambers. Subsequent impacts on Vesta likely excavated these materials and ejected them into space, where they eventually landed on Earth as meteorites.
The study of diogenites provides valuable insights into planetary differentiation processes, showing how celestial bodies separate into layers based on density, and helping scientists understand the conditions in the early solar system.
Diogenites belong to the HED (Howardite–Eucrite–Diogenite) group of meteorites. This group also includes howardites, which are mixtures of eucrite and diogenite material, and eucrites, which are basaltic rocks from Vesta with different mineral compositions. This classification helps researchers trace the origins and evolutionary history of these meteorites and provides context for understanding similar bodies throughout our solar system.
