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 that is rich in iron and magnesium. The presence of this mineral gives diogenites their characteristic dark color and dense structure. In addition to orthopyroxene, diogenites may contain other minerals such as olivine, plagioclase, and various metallic phases. The specific mineralogical composition can vary among individual specimens, reflecting different cooling histories or parent body processes.
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.
The formation of diogenites is closely tied to the geological history of asteroid Vesta. These meteorites likely formed from differentiated basaltic magma, with heavier minerals like orthopyroxene crystallizing first and settling at the bottom of magma chambers. Subsequent impacts on Vesta ejected these rocks into space, eventually delivering them to Earth.
Studying diogenites provides key insights into planetary differentiation, revealing how celestial bodies develop layered structures, and helps scientists understand conditions in the early solar system.
Diogenites belong to the HED (Howardite-Eucrite-Diogenite) group. Howardites are mixtures of eucrite and diogenite material, while eucrites are basaltic rocks from Vesta with distinct mineral compositions. This classification allows researchers to trace the origins and evolutionary history of these meteorites and better understand similar bodies in the solar system.
