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57.05g Eucrite Breccia end slice I HED Northeast Africa 110
Top Meteorite
- $ 570.00
On Offer: 57.05 gram Eucrite Breccia end slice I NEA 110
Dimensions: 56 mm x 46.9 mm x 19.46 mm
Official name: Northeast Africa 110 (NEA 110)
Type: Achondrite HED, Eucrite breccia
Origin: Libya
Description: 57.05 gram end slice of the amazing eucrite breccia meteorite Northeast Africa 110 (NEA 110). This is a beautiful clastic breccia of the achondrite HED eucrite. Polished on one side and showing the natural exterior of the meteorite on the other side. This is a light-colored eucrite meteorite with many light-colored clasts visible through the interior.
The HED Meteorite Clan: petrological evidence and data from NASA's Dawn mission indicate that nearly monomineralic ultramafic orthopyroxenite, olivine-bearing, and the much more rare harzburgitic, and dunite diogenites formed alongside each other. They likely originated as cumulates within localized magma chambers (plutons) situated across Vesta's lower crust and the lower-crust/upper-mantle transition zone. While the eucrites represent more evolved plagioclase rich mafic upper to middle zone crustal material. The howardites were formed by impact mixing of the diogenitic and eucritic material both in situ and during ejection events.
The HED meteorites are so named for the three types of meteorites that comprise the group; Howardite, Eucrite and Diogenite. The Eucrite and Diogenite are meteorites with distinct chemistries, while the Howardite is a mix of the eucritic and diogenitic material. The HEDs are differentiated achondritic meteorites, thought to originate from the large differentiated asteroid 4 Vesta. Vesta is one of the only asteroids visible with the naked eye and low powered telescopes.
The Vesta parent body origin for the HED clan of meteorites is considered to have been conclusively established for many years. However, the late Dr. John Wasson, a planetary science researcher from UCLA had long held that the HED meteorite clan originated from another unknown Vesta-like asteroid that was blown apart long ago. This is because we also find a class of iron meteorites with nearly identical oxygen isotopes as the HED clan. This along with other research lead Dr. Wasson to conclude the HED clan of meteorites come from another differentiated V-type asteroid that was in a cataclysmic collision liberating part or all of its metal core along with the HED meteorites.
However, this hypothesis does not necessarily rule out the possibility that a "reaccreted" Vesta and the smaller V-type asteroids collectively known as Vestoids along with the HED meteorites and the isotopically paired irons were all once part of a much larger dwarf planet prior to a massive collision with another large body. While most researchers consider the case mostly closed on this debate, the paradox of isotopically paired core metal raised by Dr. Wasson's hypothesis has not been resolved. This leaves some to speculate that perhaps we still have more to learn about this fascinating clan of achondrite meteorites and even Vesta itself.
The HED Meteorite Clan: petrological evidence and data from NASA's Dawn mission indicate that nearly monomineralic ultramafic orthopyroxenite, olivine-bearing, and the much more rare harzburgitic, and dunite diogenites formed alongside each other. They likely originated as cumulates within localized magma chambers (plutons) situated across Vesta's lower crust and the lower-crust/upper-mantle transition zone. While the eucrites represent more evolved plagioclase rich mafic upper to middle zone crustal material. The howardites were formed by impact mixing of the diogenitic and eucritic material both in situ and during ejection events.
The HED meteorites are so named for the three types of meteorites that comprise the group; Howardite, Eucrite and Diogenite. The Eucrite and Diogenite are meteorites with distinct chemistries, while the Howardite is a mix of the eucritic and diogenitic material. The HEDs are differentiated achondritic meteorites, thought to originate from the large differentiated asteroid 4 Vesta. Vesta is one of the only asteroids visible with the naked eye and low powered telescopes.
The Vesta parent body origin for the HED clan of meteorites is considered to have been conclusively established for many years. However, the late Dr. John Wasson, a planetary science researcher from UCLA had long held that the HED meteorite clan originated from another unknown Vesta-like asteroid that was blown apart long ago. This is because we also find a class of iron meteorites with nearly identical oxygen isotopes as the HED clan. This along with other research lead Dr. Wasson to conclude the HED clan of meteorites come from another differentiated V-type asteroid that was in a cataclysmic collision liberating part or all of its metal core along with the HED meteorites.
However, this hypothesis does not necessarily rule out the possibility that a "reaccreted" Vesta and the smaller V-type asteroids collectively known as Vestoids along with the HED meteorites and the isotopically paired irons were all once part of a much larger dwarf planet prior to a massive collision with another large body. While most researchers consider the case mostly closed on this debate, the paradox of isotopically paired core metal raised by Dr. Wasson's hypothesis has not been resolved. This leaves some to speculate that perhaps we still have more to learn about this fascinating clan of achondrite meteorites and even Vesta itself.
What you get: 57.05 gram NEA 110 Eucrite Meteorite specimen as shown & signed Certificate of Authenticity.
We offer a 100% no questions asked 30 day return policy.
SEE OFFICIAL METEORITICAL SOCIETY ENTRY BELOW
| Northeast Africa 110 | |||||||||||||||||||||||||||||
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| Basic information |
Name: Northeast Africa 110 This is an OFFICIAL meteorite name. Abbreviation: NEA 110 Observed fall: No Year found: 2023 Country: Libya Mass: 1650 g |
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| Classification history: |
This is 1 of 260 approved meteorites classified as Eucrite-br. Search for other: Achondrites, Eucrites, and HED achondrites |
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| Comments: | Approved 6 Sep 2025 | ||||||||||||||||||||||||||||
| Writeup |
Writeup from MB 114:
Northeast Africa 110 (NEA 110) Libya Purchased: 2023 Oct Classification: HED achondrite (Eucrite, brecciated) History: Purchased by Isaac Schroeder in October 2023 from a meteorite hunter in Libya. Physical characteristics: A single 1650 g gray and black stone with weathered fusion crust covering approximately 20% of the exterior. Petrography: (D. Dickens, LMAC ) An igneous breccia composed of rounded and angular clasts with ophitic and subophitic textures set in a clastic matrix of similar composition. Minerals are pyroxene and plagioclase. Pyroxenes are augite, pigeonite, and low-Ca pyroxene. Plagioclase is found as laths of bytownite and anorthite with average grain size of ~1000 µm. Accessory minerals are ilmenite, chromite, titanian chromomagnetite, and slightly aluminous silica polymorph. Geochemistry: (D. Dickens, LMAC and A. S. Bell, UColo) Low-Ca pyroxene Fs59.9±0.7,Wo4.0±0.4, FeO/MnO 32±1 (n=3). Pigeonite Fs57.2±2.7Wo7.4±3.0, FeO/MnO 33±1 (n=13). Augite Fs30.8±1.5Wo39.8±1.8, FeO/MnO 33±4 (n=10). Plagioclase An89.3±1.2Ab10.2±1.2Or0.5±0.1 (n=16). Classification: Achondrite (eucrite, breccia) Specimens: Type specimen of 20 g at TCU. Mian mass with Issac Schroeder and anonomous collector. |
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| Data from: MB114 Table 0 Line 0: |
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