Meteorite**NWA 14137, LUNAR MARE BASALT**5.372 Grams, RAREST LUNAR EVER!!!

Description

Hello up for sale is one of the rarest meteorite on the market, classified as NWA 14137. This gorgeous and unique slice weighs 5.372 grams, it has a perfect polish to one side with insanely beautiful features and vesicle pits!! This meteorite is classified as a
LUNAR MARE BASALT AND ONE OF THE ONLY FROM THE NEARSIDE OF THE MOON!!!!!!
Single stone, with smooth to irregular exterior surface, no fusion crust present, and numerous vesicles pits visible in hand sample. Polished saw cuts reveal a fine-grained mix of dark-gray and light-brown grains, many dark shock melt pockets present. Unbrecciated!!
Based on the TiO2 content of quench melt this is meteorite transitional between low-Ti and intermediate-Ti mare basalt (Giguere et al. 2000).
It comes with a COA card and display case. Thanks for your interest and take care.
LAST SLICE AVAILABLE FROM PERSONAL COLLECTION!!!
Northwest Africa 14137 (NWA 14137)
(Northwest Africa)
Find: 2021
Classification: Lunar meteorite (basalt)
History: Reportedly found in 2021 and purchased by Doug Chenin in 2021 from a meteorite dealer in Mauritania.
Physical characteristics: Single stone, with smooth to irregular exterior surface, no fusion crust present, and numerous vesicles pits visible in hand sample. Polished saw cuts reveal a fine-grained mix of dark-gray and light-brown grains, many dark shock melt pockets present. Unbrecciated.
Petrography: (C. Agee, UNM) Backscattered electron images shown igneous-zoned olivines and pyroxenes. Maskelynite makes up approximately 25% of the modal mineralogy, ubiquitous acicular ilmenite ~5%, minor ulvospinel, troilite, chromite and silica observed. Quench melt pockets are present throughout.
Geochemistry: (A. Ross and C. Agee, UNM) Olivine Fa57.7±21.1, Fe/Mn=99±4, n=9; clinopyroxene Fs46.1±19.2Wo25.1±5.6, Fe/Mn=64±12, n=12;, maskelynite An88.5±0.8Ab11.0±0.8, n=6. Quench melt SiO2=43.7±0.7, TiO2=4.1±0.3, Cr2O3=0.24±0.08, Al2O3=10.1±1.2, MgO=5.9±1.6, FeO=22.2±1.0, MnO=0.28±0.02, CaO=10.7±0.5, Na2O=0.42±0.16, K2O=0.12±0.05 (all wt%, 30 μm defocused beam), n=8. Clinopyroxene shows Fe-enrichment trends that are continuous from Mg-augite and Mg-pigeonite to subcalcic-ferroaugite/ferropigeonite.
Classification: Lunar (mare basalt). Based on the TiO2 content of quench melt this is meteorite transitional between low-Ti and intermediate-Ti mare basalt (Giguere et al. 2000).
Specimens: 15.9 g including a probe mount on deposit at UNM, DChenin holds the main mass.
Date: 2021
Mass (g): 77
Pieces: 1
Class: Lunar (basalt)
Shock stage: high
Weathering grade: moderate
Fayalite (mol%): 57.7±21.1
Ferrosilite (mol%): 46.1±19.2
Wollastonite (mol%): 25.1±5.6
Classifier: C. Agee, UNM
Type spec mass (g): 15.9
Type spec location: UNM
Main mass: DChenin
Comments: Submitted by C. Agee
NOTICE: THE SHIPPING FOR INTERNATIONAL ORDERS WILL BE SENT BY FEDEX WITH FULL TRACKING AND SAFE DELIVERY!!!
DOMESTIC SHIPPING WILL BE PRIORITY WITH FULL TRACKING AND SIGNATURE IF DESIRED.
Most lunar meteorites are polymict breccias from the lunar highlands. In contrast the Apollo missions were all nearside where mare basalts are most abundant. Your meteorite is also most likely from the lunar nearside."
Origin of the Mare Basalts
Mare basalts originate by partial melting, at temperatures of about 1200°C, deep in the lunar interior (see Fig. 8), probably at depths between 200 and 400 km. The lunar volcanic glasses appear to come from greater depths, but still from a differentiated source. The basalts are derived from the zones and piles of cumulate minerals developed, at various depths, during crystallization of the magma ocean. The isotopic systematics of the mare basalts indicate that the source region had crystallized by 4.4 billion years. Partial melting occurred in these diverse mineral zones some hundreds of millions of years later due to the slow buildup of heat from the presence of the radioactive elements K, U, and Th. The melting was not extensive. Over 25 distinct types of mare basalt were erupted over an interval of more than 1 billion years, but the total amount of melt so generated amounted to only about 0.1% of the volume of the Moon. This forms a stark contrast to the state of the Moon at accretion, when it may have been entirely molten.