Large Museum Quality Nwa 869 L-5 Chondrite Stone Meteorite North West Africa For SaleLARGE MUSEUM QUALITY NWA 869 L-5 CHONDRITE STONE METEORITE NORTH WEST style="text-align: center;">
BIG NWA 869 METEORITE70% primary fusion crust with 30% secondary fusion crust anddesert varnishThe huge meteorite is 1 1/2" x 2" x 3 1/2" inchesIt weights 289 gramsPhysical characteristics: Most samples are individual meteorites but some fragments(mostly >1 kg) also occur. In most cases the fusion crust has been polished orablated by wind erosion. Many samples are more severely affected and show faceswith deep wind erosion features. Fracture faces, formed by ground collision, showa typical gray-green color and sometimes visible brecciation (light and/or darkclasts). Due to the coarseness of this breccia, there are some stones that consistof only a single lithology.Petrography: This chondritic breccia consists of about 75 vol% matrix withunequilibrated and equilibrated L-chondrite clasts (up to 5.5 cm), some of whichdisplay shock-darkening. Impact melt-rock clasts, themselves either clast-free orclast-poor, also occur and are strongly depleted in Fe,Ni metal and sulfide.Geochemistry: Northwest Africa 869 is a regolith breccia, containing solar noblegases and preirradiated lithologies. Olivine in lithic clasts: Fa0.2-49.2; olivinein matrix: Fa10.3-29.3; low-Ca pyroxene in lithic clasts: Fs2.1-35.9; low-Ca pyroxene inmatrix: Fs7.0-23.9. Bulk oxygen isotopes: δ17O = 3.52; δ18O = 4.67; Δ17O = 1.09 per mil.Terrestrial age: 4.4 ± 0.7 ka. Preatmospheric meteoroid size and mass: 225 ± 25 cm, 120-230 T.Classification: Because NWA 869 contains unequilibrated clasts, its classification is revisedto L3-6.
Chondrites are stony meteorites that have not been modified due to melting ordifferentiation of the parent body. They formed when various types of dust andsmall grains that were present in the early solar system accreted to formprimitive asteroids. Prominent among the components present in chondrites arethe enigmatic chondrules, millimeter-sized objects that originated as freelyfloating, molten or partially molten droplets in space; most chondrules arerich in the silicate minerals olivine and pyroxene. Chondrites also containrefractory inclusions (including Ca-Al Inclusions), which are among the oldestobjects to form in the solar system, particles rich in metallic Fe-Ni andsulfides, and isolated grains of silicate minerals. The remainder of chondritesconsists of fine-grained (micrometer-sized or smaller) dust, which may either bepresent as the matrix of the rock or may form rims or mantles around individualchondrules and refractory inclusions. Embedded in this dust are presolar grains,which predate the formation of our solar system and originated elsewhere in thegalaxy.
Most meteorites that are recovered on Earth are chondrites: ~86% of witnessedfalls are chondrites, as is the overwhelming majority of meteorites that arefound. There are currently over 27,000 chondrites in the world's collections.The largest individual stone ever recovered, weighing 1770 kg, was part of theJilin meteorite shower of 1976. Chondrite falls range from single stones toextraordinary showers consisting of thousands of individual stones, as occurredin the Holbrook fall of 1912, where an estimated 14,000 stones rained down onnorthern Arizona.VERY NICE SPACE ROCK
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