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35.96g Eucrite Melt Breccia Slice I HED I Taoudenni 005
Top Meteorite
- $ 360.00
On Offer: 35.96 gram Eucrite Melt Breccia slice I Taoudenni 005
Dimensions: 92 mm x 80 mm x 2 mm
Type: HED achondrite (Eucrite, melt breccia)
Origin: Mali
Official name: Taoudenni 005
Description: 35.96 gram slice of melt breccia eucrite Taoudenni 005. This is a dark-colored eucrite meteorite with many light-colored clasts visible through the wind polished exterior. This slice is polished on one side.
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: 35.96 gram Taoudenni 005 Eucrite Meteorite specimen as shown & signed Certificate of Authenticity.
I offer a 100% no questions asked 30 day return policy.
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| Taoudenni 005 | |||||||||||||||||||||||||||||||
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| Basic information |
Name: Taoudenni 005 This is an OFFICIAL meteorite name. Abbreviation: There is no official abbreviation for this meteorite. Observed fall: No Year found: 2024 Country: Mali Mass: 2.11 kg |
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| Classification history: |
This is 1 of 132 approved meteorites classified as Eucrite-melt breccia. Search for other: Achondrites, Eucrites, and HED achondrites |
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| Comments: | Approved 19 Nov 2024 | ||||||||||||||||||||||||||||||
Writeup |
Writeup from MB 113:
Taoudenni 005 22.675981°N, 3.977780°W Gao, Mali Purchased: August 2024 Classification: HED achondrite (Eucrite, melt breccia) History: Purchased in August 2024 by Joshua Eisler from a meteorite hunter in Mali. Physical characteristics: A single 2111 g dark-colored stone with many light-colored clasts visible through the wind polished exterior. Petrography: (D. Dickens, LMAC) An igneous melt breccia with millimeter to centimeter-sized clasts with ophitic and subophitic texture composed of Ca-rich plagioclase, low-Ca pyroxene, pigeonite, and augite, with accessory silica polymorph, metal, sulfides and oxides set in a microporphyritic groundmass melt of similar composition. Most low-Ca pyroxene grains display lamellae of exsolved clinopyroxene, likely augite. Geochemistry: (D. Dickens, LMAC and A. S. Bell, UColo) Low-Ca pyroxene Fs62.4±1.2,Wo2.6±1.2, FeO/MnO 32.4±1 (n=7). Pigeonite Fs55.3±2.6Wo11.6±3.3, FeO/MnO 32.1±3 (n=8). Augite Fs38.2±7.6Wo31.8±8.9, FeO/MnO 31.9±1 (n=4). Plagioclase An89.6±1.9Ab9.9±1.9Or0.5±0.2 (n=22). Classification: Achondrite (Eucrite, melt breccia) Specimens: Type specimen of 22.58 g at TCU. Mian mass with Joshua Eisler. |
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| Data from: MB113 Table 0 Line 0: |
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| Institutions and collections |
TCU: Oscar E. Monnig Collection, Department of Geology, Texas Christian University, Ft. Worth, TX 76129, United States; Website (institutional address; updated 2012-02-24) UColo: Geological Sciences University of Colorado Boulder UCB 399 Boulder, CO 80309-0399, United States (institutional address; updated 2024-07-02) |
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