Meteorite**NWA 15000, Eucrite Polymict**14.077 gram Endcut with glossy crust

Description

Hello up for sale is one of my newest classifications NWA 15000, Eucrite Polymict Achondrite (HED). This fragment endcut weighs 14.077 grams, it has a gorgeous look with nice glossy black fusion crust and a nicely polished face. Petrography:  Breccia composed of a variety of lithic eucrite clasts plus related crystalline debris and minor diogenitic orthopyroxene (<10 vol.%) within a fine grained matrix. Textures of lithic clasts include fine intergranular, subophitic, diabasic, gabbroic and very fine-grained equigranular (or granulitic). Minerals are low-Ca pyroxene, unexsolved pigeonite (some compositionally zoned), calcic plagioclase, subcalcic augite, augite, silica polymorph, chromite, ilmenite and troilite, plus rare fayalite and Fe metal. This meteorite comes with a COA card, thanks for your interest and take care.
THIS IS A GORGEOUS FUSION CRUSTED EUCRITE ACHONDRITE
ENDCUT
,
PIECE OF ARTWORK!!
Name: Northwest Africa 15000
This is an OFFICIAL meteorite name.
Abbreviation: NWA 15000
Observed fall: No
Year found: 2021
Country: (Northwest Africa)
Mass: 1700 g
Northwest Africa 15000 (NWA 15000)
(Northwest Africa)
Purchased: 2021
Classification: HED achondrite (Eucrite, polymict)
History: Purchased by Craig Zlimen in 2021 from an Algerian dealer.
Petrography: (A. Irving, UWS and J. Boesenberg, BrownU) Breccia composed of a variety of lithic eucrite clasts plus related crystalline debris and minor diogenitic orthopyroxene (<10 vol.%) within a fine grained matrix. Textures of lithic clasts include fine intergranular, subophitic, diabasic, gabbroic and very fine-grained equigranular (or granulitic). Minerals are low-Ca pyroxene, unexsolved pigeonite (some compositionally zoned), calcic plagioclase, subcalcic augite, augite, silica polymorph, chromite, ilmenite and troilite, plus rare fayalite and Fe metal.
Geochemistry: Diogenitic orthopyroxene (Fs20.0-22.0Wo0.9-2.6, FeO/MnO = 27-38, N = 3; Fs27.8-36.9Wo3.2-5.7, FeO/MnO = 27-40, N = 4), low-Ca pyroxene (Fs43.7-55.8Wo1.5-5.2, FeO/MnO = 30-33, N = 8), pigeonite (Fs52.1Wo10.1; Fs43.9Wo17.1; FeO/MnO = 30-32; N = 2), subcalcic augite (Fs39.2Wo22.9, FeO/MnO = 30), augite (Fs26.0Wo40.5, FeO/MnO = 29), plagioclase (An80.2-92.9Or1.1-0.2, N = 5).
Classification: Eucrite (polymict breccia).
Specimens: 24.7 g including one polished thin section at UWB; remainder with Mr. C. Zlimen.
Data from:
MB111
Table 0
Line 0:
Place of purchase: Algeria
Date: P 2021
Mass (g): 1700
Pieces: 1
Class: Eucrite-pmict
Shock stage: low
Weathering grade: low
Ferrosilite (mol%): 20.0-22.0; 47.9-55.8; 27.8-36.9; 26.0
Wollastonite (mol%): 0.9-2.6; 1.5-5.1; 3.2-5.7; 40.5
Classifier: A. Irving, UWS, and J. Boesenberg, BrownU
Type spec mass (g): 24.7
Type spec location: UWB
Main mass: C. Zlimen
Comments: Work name ZLI067; submitted by A. Irving
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. NASA’s 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 where—in cases like Vesta—the 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) wide—some 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.