Location: Western Sahara

Weight: 0.4 Ounces (Display)

Dimensions: 2.3 Inches Long, 1.5 Inches Wide, 0.6 Inches Thick (Display)

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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 igneous meteorites dominated by orthopyroxene, an iron- and magnesium-rich silicate mineral that gives these specimens their dark coloration and notably dense character. Minor components such as olivine, plagioclase feldspar, and small amounts of metallic phases may also be present, with proportions varying from specimen to specimen. These variations reflect differences in crystallization depth, cooling rate, and localized conditions within the parent body.

Most diogenites display a coarse crystalline texture, formed as molten material cooled slowly over extended periods. This gradual cooling allowed large mineral crystals to grow, distinguishing diogenites from fine-grained volcanic meteorites. Many examples exhibit a cumulate structure, indicating formation through the settling and accumulation of early-crystallizing minerals within magma chambers.

The origin of diogenites is closely tied to the internal evolution of asteroid 4 Vesta, a differentiated body that experienced significant melting early in solar system history. As basaltic magma cooled within Vesta, dense minerals such as orthopyroxene crystallized first and migrated downward, forming layered deposits beneath the surface. Later impact events excavated these deep-seated rocks and launched them into space, where a small fraction eventually reached Earth.

Because of their origin and mineralogy, diogenites offer important evidence for planetary differentiation, the process by which celestial bodies separate into distinct internal layers. They are part of the HED meteorite group, alongside eucrites and howardites—rocks that together represent different portions of Vesta’s crust and interior. Studying these meteorites helps scientists reconstruct the geological history of small planetary bodies and better understand the processes active during the early formation of the solar system.