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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 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 linked to the geological history of Vesta. It is hypothesized that these meteorites formed from differentiated basaltic magma on Vesta's surface. As Vesta cooled, heavier minerals like orthopyroxene crystallized first and settled towards the bottom of magma chambers. Over time, impacts on Vesta could have excavated these materials and ejected them into space, where they eventually fell to Earth as meteorites.

The study of diogenites provides valuable information about planetary differentiation processes—how celestial bodies separate into layers based on density—and helps scientists understand the conditions present in the early solar system.

Diogenites are categorized within a broader classification scheme for meteorites based on their mineralogy and chemical composition. They fall under the HED (Howardite-Eucrite-Diogenite) group, which includes two other types: howardites and eucrites. Howardites are mixtures of eucrite and diogenite material; eucrites are basaltic rocks that also originate from Vesta but have different mineral compositions compared to diogenites.

This classification aids researchers in tracing back the origins and evolutionary history of these celestial materials while providing context for understanding similar bodies throughout our solar system.