Meteorite**Jikharra 001, Eucrite-Melt Breccia**120.10 gram Big Slice, NEW FIND!

Description

Hello up for sale is Jikharra 001 classified as a Eucrite-melt breccia. This massive slice weighs 120.10 grams, perfect polish to one side, remnants of fusion crust and vesicles, composed of several cm-sized lithic clasts set in abundant recrystallized shock melt. Lithic clasts consist of calcic plagioclase and aggregates of fine-grained, 30-70 µm sized pigeonite crystals displaying patchy compositional zoning. The melt matrix is composed of recrystallized pigeonite displaying mottled compositional zoning and fine-grained, mostly fibrous feldspar. Minor phases include silica, Ti-chromite, ilmenite, and FeS. No metallic iron has been detected. This meteorite comes with 2 COA cards, Streaming Meteorites and Mark Lyon. Thanks for your interest and take care.
Name: Jikharra 001
This is an OFFICIAL meteorite name.
Abbreviation: There is no official abbreviation for this meteorite.
Observed fall: No
Year found: 2022
Country: Libya
Mass: 2.5 t
Jikharra 001        29°58’08.2’’ N, 21°52’05.0’’ E
Ajdabiya, Libya
Purchased: 2022
Classification: HED achondrite (Eucrite, melt breccia)
History: Numerous fragments reportedly totalling at least 2.5 metric tons, and possibly more that 3 T, were recovered in Northeastern Libya. Fifty kg of it were subsequently purchased by the main mass holder from a meteorite dealer in Libya.
Physical characteristics: Many brownish fragments some of which with small patches of fusion crust.
Petrography: Achondritic melt breccia composed of several cm-sized lithic clasts set in abundant recrystallized shock melt. Lithic clasts consist of calcic plagioclase and aggregates of fine-grained, 30-70 µm sized pigeonite crystals displaying patchy compositional zoning. The melt matrix is composed of recrystallized pigeonite displaying mottled compositional zoning and fine-grained, mostly fibrous feldspar. Minor phases include silica, Ti-chromite, ilmenite, and FeS. No metallic iron has been detected.
Geochemistry: patchily zoned pigeonite: Fs50.1±1.5Wo11.6±1.7 (Fs48.1-53.4Wo6.9-13.3, FeO/MnO=27-31, n=12); calcic plagioclase: An90.2±0.7 (An88.9-91.3, n=10)
Specimens:: 83.5 g at MNB; 205 g including two polished thin sections at UWB; 50 kg with M. Cimala; 63.36 kg with WangZ, 350 kg with M. Lyon, 845.8 kg with DPitt; (including a single 215 kg specimen), ~150 kg with Ali Benamar; 1000 kg with an anonymous Chinese collector.
Data from:
MB111
Table 0
Line 0:
State/Prov/County:Ajdabiya
Place of purchase:Libya
Date:P 2022
Latitude:29°58'08.2'' N
Longitude:21°52'05.0'' E
Mass (g):2500000
Pieces:many
Class:Eucrite-melt breccia
Shock stage:high
Weathering grade:moderate
Ferrosilite (mol%):50.1
Wollastonite (mol%):11.6
Classifier:A. Greshake, MNB
Type spec mass (g):289
Type spec location:83.5 g MNB, 205 g UWB
Main mass:M. Cimala, WangZ, M. Lyon, DPitt, A. Benamar
Comments:Submitted by Ansgar Greshake
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ASTERIOD 4 VESTA
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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.