Meteorite**NWA 13765, Eucrite**4.524 gram Slice W/Gorgeous matrix& fusion crust

Description

Hello up for sale is NWA 13765, classified as a Monomict eucrite. This beautiful slice weighs 4.524 grams, it has nice fresh black fusion crust on the edge.  A freshly cut window shows a fine-grained texture with white feldspar grains and light gray pyroxene grains. Electron microprobe analysis of a polished mount shows a mildly brecciated rock having clasts with variable grain size. This slice will comes with a COA card, Streaming meteorites & with a display case.  Thanks for your interest and take care.
Name: Northwest Africa 13765
This is an OFFICIAL meteorite name.
Abbreviation: NWA 13765
Observed fall: No
Year found: 2014
Country: Morocco
Mass: 82.1 g
Northwest Africa 13765 (NWA 13765)
Boujdour, Morocco
Find: 2014
Classification: HED achondrite (Eucrite)
History: Purchased by Douglas Chenin from a Moroccan meteorite dealer in 2014. Reportedly found the same year at Jrifia near Boujdour, Morocco.
Physical characteristics: This meteorite is a single stone covered in black shiny fusion crust. Numerous fine cracks are present on the surface, small chipped spots reveal light tan colored interior. A freshly cut window shows a fine-grained texture with white feldspar grains and light gray pyroxene grains.
Petrography: (C. Agee, UNM) Electron microprobe analysis of a polished mount shows a mildly brecciated rock having clasts with variable grain size. The finest grained clasts have plagioclase and pyroxene in size range 50-200 μm. Coarser grained clasts show elongate plagioclase up to 500 μm and equant pyroxene 100-400 μm. Very fine exsolution lamellae are present in both low-Ca pyroxene and augite. Chromite, Fe-metal, silica, and ilmenite are ubiquitous accessory minerals.
Geochemistry: (C. Agee, UNM) Low-Ca pyroxene Fs61.5±2.2Wo3.0±1.2, Fe/Mn=31±2, n=10; augite Fs27.3±0.5Wo43.5±0.6, Fe/Mn=31±2, n=10; plagioclase An88.9±0.8Ab10.5±0.7Or0.6±0.3, n=6. Compositionally uniform throughout with some grain size variation from clast to clast. Pyroxenes show nearly complete chemical compositional separation between low-Ca pyroxene and augite.
Classification: Monomict eucrite.
Specimens: 16.5 g on deposit at UNM, D. Chenin holds the main mass.
Data from:
MB110
Table 0
Line 0:
State/Prov/County:Boujdour
Origin or pseudonym:Jrifia
Place of purchase:Morocco
Date:2014
Mass (g):82.1
Pieces:1
Class:Eucrite
Shock stage:moderate
Weathering grade:low
Ferrosilite (mol%):61.5±2.2, 27.3±0.5
Wollastonite (mol%):3.0±1.2, 43.5±0.6
Classifier:C. Agee, UNM
Type spec mass (g):16.5
Type spec location:UNM
Main mass:D. Chenin
Comments:Submitted by C. Agee
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.