Description: Hello, up for sale is NWA 14403, Eucrite Monomict Achondrite (HED). This individual weighs 5.085 grams, it has a gorgeous look. This meteorite is a fragmental breccia of basaltic eucrite with subophitic texture with ~60% pyroxene and ~35% plagioclase. Pyroxenes show exsolution lamellae and have a compositional continuum between low-Ca pyroxene and augite. Accessory phases are silica, ilmenite, troilite, chromite, and zircon. Thirty similar appearing fusion crusted individuals. Brecciated texture is visible on the exterior with dark and light colored clasts. This meteorite comes with a COA card and display case. Thanks for your interest and take care. Monomict Eucrite meteorites are a type of achondritic stony meteorite that primarily consists of the mineral pyroxene. They belong to a specific class of meteorites known as the HED (Howardite, Eucrite, Diogenite) meteorites, which are thought to originate from the asteroid Vesta. Eucrites are primarily composed of pyroxene and plagioclase feldspar, with trace amounts of other minerals such as olivine and quartz. They are typically basaltic in composition and show evidence of volcanic or magmatic origin. Monomict Eucrites are classified as monomict breccias, meaning that they consist of a single lithology (in this case, Eucrite) with similar mineral composition throughout. Studying monomict Eucrite meteorites can provide valuable insights into the geology and history of Vesta, the parent body from which they originated. Researchers analyze these meteorites to understand the processes that shaped Vesta's crust and interior, as well as the conditions that existed in the early solar system. Name:Northwest Africa 14403 This is an OFFICIAL meteorite name. Abbreviation:NWA 14403 Observed fall:No Year found:2021 Country:(Northwest Africa) Mass:3 kg Northwest Africa 14403(NWA 14403) (Northwest Africa) Purchased: 2021 Classification: HED achondrite (Eucrite, monomict) History: Purchased by Matthew Stream from Ali Hnini and Mostafa Hnini in June 2021. Physical characteristics: Thirty similar appearing fusion crusted individuals. Brecciated texture is visible on the exterior with dark and light colored clasts. Petrography: (C. Agee and A. Ross,UNM) Reflected light microscopy and electron microprobe imaging shows that this meteorite is a fragmental breccia of basaltic eucrite with subophitic texture with ~60% pyroxene and ~35% plagioclase. Pyroxenes show exsolution lamellae and have a compositional continuum between low-Ca pyroxene and augite. Accessory phases are silica, ilmenite, troilite, chromite, and zircon. Geochemistry: (A. Ross,UNM) Pyroxene Fs50.914.2Wo19.216.0, Fe/Mn=321, n=12; plagioclase An87.31.9, n=6. Classification: Achondrite (monomict eucrite) Specimens: 26.11 g on deposit atUNM, Matthew Stream holds the main mass. Data from: MB110 Table 0 Line 0: Place of purchase:Morocco Date:P 2021 Mass (g):3000 Pieces:30 Class:Eucrite-mmict Shock stage:high Weathering grade:low Ferrosilite (mol%):50.914.2Wollastonite (mol%):19.216.0 Classifier:C. Agee, UNM Type spec mass (g):26.11 Type spec location:UNM Main mass:Matthew Stream Comments:Field name MST-8; submitted by C. Agee, UNM 4 Vesta is the second most massive body in the main asteroid belt, accounting for almost nine percent of the total mass of all asteroids. Only dwarf planet Ceres is more massive in that region of rocky debris between Mars and Jupiter. NASAs Dawn spacecraft circled Vesta from July 16, 2011 until Sept. 5, 2012, when it departed and began its journey to dwarf planet Ceres. The giant asteroid is almost spherical, and so is nearly classified a dwarf planet. Unlike most known asteroids, Vesta has separated into crust, mantle and core (a characteristic known as being differentiated), much like Earth. Understanding why this is so was one of the objectives of the Dawn mission. The answer turned out to be that Vesta formed early, within 1 to 2 million years of the birth of the solar system. Short-lived radioactive material that was incorporated into bodies that formed during this epoch heated them to the point wherein cases like Vestathe objects melted, allowing the denser materials to sink to the asteroid's core and the lower density materials to rise. Vesta has one of the largest brightness ranges observed on any rocky body in our solar system. The bright materials appear to be native rocks, while the dark material is believed to have been deposited by other asteroids crashing into Vesta. Scientists on the Dawn team estimate that about 300 dark asteroids with diameters ranging from one to 10 km (0.6 to six miles) hit Vesta during the last 3.5 billion years. This would have been enough to wrap the Vesta in a blanket of material about three to seven feet (one to two meters) thick. An extensive system of troughs encircles Vesta's equatorial region. The largest, named Divalia Fossa, is bigger than the Grand Canyon. Vesta appears to be the source of the Howardite, Eucrite and Diogenite groups of meteorites that have been found on Earth. They help scientists understand the "Lunar Cataclysm," when a repositioning of the gas-giant planets billions of years ago destabilized the orbits of asteroids in the early asteroid belt and triggered a solar-system-wide bombardment. They also provide clues to Vesta's geochemical evolution, a story that was tested and enhanced by the information Dawn provided about the asteroid's surface and interior. Vesta is believed to have lost about one percent of its mass less than a billion years ago in a massive collision responsible for the Rheasilvia crater, which is about 310 miles (500 kilometers) widesome 95 percent of the asteroid's mean diameter. The Vesta family of asteroids is probably debris from this collision. Another huge crater is Veneneia, which is about 250 miles (400 km) in diameter.
Price: 60 USD
Location: Riverside, California
End Time: 2024-11-13T06:26:42.000Z
Shipping Cost: 9 USD
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