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174.46g Eucrite Monomict end piece I HED NWA 8555
Top Meteorite
- $ 1,750.00
On Offer: 174.46 gram Eucrite Monomict end piece of NWA 8555
Official name: NWA 8555
Type: HED achondrite (Eucrite, monomict)
Origin: Morocco
Description: 174.46 NWA 8555 gram polished beautiful end piece of monomict eucrite NWA 8555.
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: 174.46 gram NWA 8555 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
| Northwest Africa 8555 | |||||||||||||||||||||||
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| Basic information |
Name: Northwest Africa 8555 This is an OFFICIAL meteorite name. Abbreviation: NWA 8555 Observed fall: No Year found: 2013 Country: (Northwest Africa) Mass: 2.92 kg |
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| Classification history: |
This is 1 of 187 approved meteorites classified as Eucrite-mmict. [show all] Search for other: Achondrites,Eucrites, and HED achondrites |
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| Comments: | Approved 18 Oct 2014 | ||||||||||||||||||||||
| Writeup |
Writeup from MB 103:
Northwest Africa 8555 (NWA 8555) (Northwest Africa) Purchased: 2013 Classification: HED achondrite (Eucrite, monomict) History: Purchased by Brahim Tahiri from a Moroccan hunter and sent to his partner Sean Tutorow for classification, April, 2013. Physical characteristics: Two matching stones, 1729 g and 1198 g. Irregular weathered exterior. Saw cut reveals a breccia with tan lithic clasts up to 1 cm set in a dark-gray matrix. Petrography: (C. Agee, UNM) Microprobe examination of a polished mount show basaltic eucrite clasts cross-cut by shock melt veins, pyroxenes show exsolution lamellae. Ubiquitous chromite, ilmenite, and silica, some barite found. Moderate weathering. Geochemistry: (C. Agee and N. Muttik, UNM) Low-Ca pyroxene Fs60.7±2.2Wo4.5±2.4, Fe/Mn=33±1, n=12; high-Ca pyroxene Fs29.3±1.5Wo41.1±1.6, Fe/Mn=33±1, n=12; plagioclase An89.0±1.2, n=8. Classification: Achondrite (monomict eucrite) Specimens: 59.78 g including a probe mount on deposit at UNM, Sean Tutorow holds the main mass. |
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| Data from: MB103 Table 0 Line 0: |
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| Institutions and collections |
UNM: Institute of Meteoritics MSC03 2050 University of New Mexico Albuquerque NM 87131-1126 USA, United States; Website (institutional address; updated 12 Feb 2015) | ||||||||||||||||||||||
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