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42.22g Diogenite Meteorite piece I HED Meteorite from Asteroid 4 Vesta I NWA 18094
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On Offer: 42.22g NWA 18094, orthopyroxenite diogenite HED achondrite meteorite.
Name: Northwest Africa 18094
Abbreviation: NWA 18094
Type: Diogenite
Observed fall: No
Year found: 2018
Country: Morocco
Parent Body: Vesta or Vestoid
Description: 42.22 gram specimen of an amazing orthopyroxenite diogenite. This diogenite has a coarse grained texture of mostly low-Ca pyroxene with several large black chromite crystals visible throughout the cut surfaces. Only a single small 86 gram gray-green stone was found with a small amount of remnant glassy black fusion crust on one side. This specimen represents the remaining main mass of this classification after analysis with only one smaller end piece available.
Description: 23.80 gram end piece of an amazing orthopyroxenite diogenite. This diogenite has a coarse grained texture of mostly low-Ca pyroxene with several large black chromite crystals visible throughout the cut surfaces. Only a single small 86 gram gray-green stone was found with a small amount of remnant glassy black fusion crust on one side. This specimen represents the remaining main mass of this classification after analysis with only one smaller end piece available.
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 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: 42.22 gram NWA 18094 diogenite meteorite specimen as shown, & signed Certificate of Authenticity.
We offer a 100% no questions asked 30 day return policy.
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Northwest Africa 18094
| Basic information |
Name: Northwest Africa 18094 This is an OFFICIAL meteorite name. Abbreviation: NWA 18094 Observed fall: No Year found: 2018 Country: Morocco Mass: 86 g |
|---|---|
| Classification history: |
Meteoritical Bulletin, MB 114 (2026): Diogenite |
| Comments: | Approved 5 Dec 2025 |
| Writeup |
Writeup from MB 114: Northwest Africa 18094 (NWA 18094) Morocco Purchased: 2018 Classification: HED achondrite (Diogenite) History: Purchased from a meteorite dealer in Erfoud, Morocco, in 2018 by Kathryn O'Flynn and sold to Maria Aguayo later that same year. The stone was misplaced along with several other meteorites until it was rediscovered in a storage box with the other misplaced stones in 2025. Physical characteristics: A single gray-green stone with remnant glassy black fusion crust covering approximately 20% of the surface. Saw cut reveals a mottled gray interior with some black specks. Petrography: (D. Dickens, LMAC ) This meteorite is a coarse-grained orthopyroxenite. It is a monomineralic rock composed of >98% equilibrated orthopyroxene. Chromite makes up <2% and is the only minor phase present. Chromite is found as either well-formed large grains up to 4 mm, or as μm to sub-μm inclusions in orthopyroxene. Geochemistry: (D. Dickens, LMAC and A. S. Bell, UColo) Orthopyroxene Fs23.6±0.3Wo2.5±0.1, FeO/MnO = 29±1 (n=13). Classification: Achondrite HED (Diogenite) Specimens: Type specimen of 21 g at TCU. Main mass with Issac Schroeder. |
| Data from: MB114 Table 0 Line 0: |
Place of purchase: Morocco Date: P 2018 Mass (g): 86 Pieces: 1 Class: Diogenite Shock stage: low Weathering grade: low Ferrosilite (mol%): 23.6±0.3 Wollastonite (mol%): 2.5±0.1 Classifier: D. Dickens, LMAC Type spec mass (g): 17.4 Type spec location: TCU Main mass: Maria Aguayo Comments: Field name LMAC 500; submitted by Dustin Dickens |
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