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48.45g Ksar Ghilane 024 I Harzburgitic Olivine-rich Plutonic Peridotite Diogenite Meteorite I HED Meteorite from Asteroid 4 Vesta
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- $2,331.00
On Offer: 48.45g Ksar Ghilane 024, harzburgitic peridotite diogenite HED achondrite meteorite.
Official name: Ksar Ghilane 024
Abbreviation: KG 024
Type: Diogenite-olivine
Observed fall: No
Year found: 2025
Country: Tunisia
Parent Body: Vesta or Vestoid
Description: 48.45 gram specimen of an amazing "harzburgitic" plutonic peridotite diogenite with large light green olivine crystals visible on most of the interior and exterior. Some glassy black remnant fusion crust remains from the intense plasma created during its transit through the Earth's atmosphere. This is a very rare type of plutonic olivine-rich diogenite known as a peridotite. This extraterrestrial stone displays striking petrological similarities to the terrestrial ultramafic igneous peridotite called harzburgite found in the Harz Mountains of Germany. As a peridotite with nearly 75% olivine, this diogenite is not quite a "dunite", but with only a few notable exceptions, is one of the most olivine-rich diogenites ever discovered. A truly exceptional and rare meteorite.
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: 48.45 gram diogenite-olivine meteorite specimen as shown, & signed Certificate of Authenticity.
We offer a 100% no questions asked 30 day return policy.
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Ksar Ghilane 024
Status: Official
| Basic information |
Name: Ksar Ghilane 024 This is an OFFICIAL meteorite name. Abbreviation: KG 024 Observed fall: No Year found: 2025 Country: Tunisia Mass: 1073 g |
|---|---|
| Classification history: |
Meteoritical Bulletin, MB 114 (2026): Diogenite-olivine Recommended: Diogenite-olivine This is 1 of 35 approved meteorites classified as Diogenite-olivine. |
| Comments: | Approved 23 Dec 2025 |
| Writeup | Writeup from MB 114: Ksar Ghilane 024 (KG 024) 32.999° N, 9.633° E Quibili, Tunisia Purchased: 2025 Classification: HED achondrite (Diogenite, olivine) History: Purchased in 2025 by Ahmed Saleck from a meteorite hunter in Tunisia. Physical characteristics: Three dark colored stones, 67, 453, and 545 g, all with light green crystals visible on most of the exterior. Remnant glassy fusion crust is present in some areas on all three stones. Caliche partially covers one side of the two larger stones. Saw cut reveals a course-grained crystalline interior. Petrography: (D. Dickens, LMAC) This meteorite is a coarse-grained, igneous, harzburgitic peridotite with a cumulate texture. Mineral mode is olivine ~73.5 vol.%, low-Ca pyroxene ~25.2 vol.%, with oxides, sulfides and metal making up the remaining ~1.3 vol.%. Spheroidal and subhedral olivine grains are often tightly packed and enclosing pyroxene, occasionally transitioning to areas where olivine is less dominant and poikilitically enclosed by pyroxene. Symplectic intergrowths of chromite and silica polymorph often decorate outer rims of olivine grains. Accessory phases are aluminous chromite, troilite, and low-Ni kamacite. Geochemistry: (D. Dickens, LMAC and A. S. Bell, UColo) Olivine Fa27.8±0.3 ,FeO/MnO = 46.1±2 (n=31). Low-Ca pyroxene Fs22.7±0.3Wo2.9±0.6, FeO/MnO = 29±1 (n=21). Classification: Diogenite-olivine (harzburgitic) Specimens: Type specimen of 20 g at TCU. 545g with Monnig Meteorite Collection, and remainder with Ahmed Saleck and Omar Bourki. |
| Data from: MB114 Table 0 Line 0: |
State/Prov/County: Quibili Place of purchase: Tunisia Date: P 2025 Latitude: 32.999° N Longitude: 9.633° E Mass (g): 1073 Pieces: 3 Class: Diogenite-olivine Shock stage: low Weathering grade: low Fayalite (mol%): 27.8±0.3 Ferrosilite (mol%): 22.7±0.3 Wollastonite (mol%): 2.9±0.6 Classifier: D. Dickens, LMAC Type spec mass (g): 20 Type spec location: TCU Main mass: Monnig Meteorite Collection Comments: Field name LMAC1000-CB014; submitted by Dustin Dickens |
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