{"title":"Featured Meteorites","description":"\u003ch2 data-section-id=\"yk6j6i\" data-start=\"782\" data-end=\"806\"\u003eFeatured Meteorites\u003c\/h2\u003e\n\u003cp data-start=\"807\" data-end=\"840\"\u003e\u003cstrong data-start=\"807\" data-end=\"840\"\u003eCurated Specimens of Interest\u003c\/strong\u003e\u003c\/p\u003e\n\u003cp data-start=\"842\" data-end=\"1065\"\u003eThis collection highlights a selection of meteorites chosen for their rarity, classification, visual appeal, and overall collector significance. These specimens represent some of the most notable pieces currently available.\u003c\/p\u003e\n\u003cp data-start=\"1067\" data-end=\"1264\"\u003eEach item has been selected based on quality, stability, and relevance within its classification, offering collectors an opportunity to explore exceptional material across multiple meteorite types.\u003c\/p\u003e\n\u003chr data-start=\"1266\" data-end=\"1269\"\u003e\n\u003ch2 data-section-id=\"w6qxg3\" data-start=\"1271\" data-end=\"1306\"\u003eWhy These Specimens Are Featured\u003c\/h2\u003e\n\u003cp data-start=\"1308\" data-end=\"1409\"\u003eMeteorites included in this collection are selected for one or more of the following characteristics:\u003c\/p\u003e\n\u003cul data-start=\"1411\" data-end=\"1583\"\u003e\n\u003cli data-section-id=\"qudg61\" data-start=\"1411\" data-end=\"1447\"\u003eNotable classification or rarity\u003c\/li\u003e\n\u003cli data-section-id=\"qxxiko\" data-start=\"1448\" data-end=\"1488\"\u003eStrong visual or structural features\u003c\/li\u003e\n\u003cli data-section-id=\"lj6z3o\" data-start=\"1489\" data-end=\"1533\"\u003eHigh-quality preparation or presentation\u003c\/li\u003e\n\u003cli data-section-id=\"1sdogxs\" data-start=\"1534\" data-end=\"1583\"\u003eRelevance within the broader meteorite market\u003c\/li\u003e\n\u003c\/ul\u003e\n\u003cp data-start=\"1585\" data-end=\"1646\"\u003eThis collection is updated as new specimens become available.\u003c\/p\u003e\n\u003chr data-start=\"1648\" data-end=\"1651\"\u003e\n\u003ch2 data-section-id=\"17p6g7a\" data-start=\"1653\" data-end=\"1679\"\u003eExplore More Meteorites\u003c\/h2\u003e\n\u003cul data-start=\"1681\" data-end=\"1787\"\u003e\n\u003cli data-section-id=\"1pei6oo\" data-start=\"1681\" data-end=\"1706\"\u003e\u003ca href=\"https:\/\/www.tcmeteorites.com\/collections\/all\" target=\"_blank\" title=\"Browse all meteorites\" rel=\"noopener\"\u003eBrowse all meteorites\u003c\/a\u003e\u003c\/li\u003e\n\u003cli data-section-id=\"1o8c432\" data-start=\"1707\" data-end=\"1752\"\u003e\u003ca href=\"https:\/\/www.tcmeteorites.com\/pages\/meteoritical-bulletin-explained\" target=\"_blank\" title=\"Learn more about meteorite classification\" rel=\"noopener\"\u003eLearn more about meteorite classification\u003c\/a\u003e\u003c\/li\u003e\n\u003cli data-section-id=\"xi88q5\" data-start=\"1753\" data-end=\"1787\"\u003e\u003ca href=\"https:\/\/www.tcmeteorites.com\/collections\/premium-specimens\" target=\"_blank\" title=\"Explore our premium meteorites\" rel=\"noopener\"\u003eExplore our premium meteorites\u003c\/a\u003e\u003c\/li\u003e\n\u003c\/ul\u003e","products":[{"product_id":"libyan-desert-glass-impactite-353-18g","title":"Libyan Desert Glass Impactite Individual, 353.18g, Translucent Yellow-Green Silica Glass","description":"\u003ch2\u003eTranslucent silica glass from ancient impact event\u003c\/h2\u003e\u003cp\u003eThis 353.18g specimen displays the characteristic translucent yellow-green coloration of Libyan Desert Glass, with visible flow textures frozen in place from the moment of formation. The natural surface retains the sculptural forms created by aerodynamic ablation and sandblasting in the Great Sand Sea. Light passes through portions of the glass, revealing internal structures and occasional inclusions captured during the impact melt process.\u003c\/p\u003e\u003cp\u003eThe specimen's substantial mass provides exceptional display presence while maintaining the delicate transparency that makes this material visually distinctive. Surface features include natural pitting, flow lines, and the matte texture characteristic of prolonged desert weathering.\u003c\/p\u003e\u003ch2\u003eFormation and composition\u003c\/h2\u003e\u003cp\u003eLibyan Desert Glass forms from pure silica sand subjected to extreme temperatures exceeding 1,700°C during meteorite impact. The resulting material is lechatelierite, a naturally occurring silica glass that requires temperatures far beyond what volcanic processes can achieve. The impact event 29 million years ago in the Late Oligocene melted desert sand instantaneously, creating scattered glass fragments across approximately 6,500 square kilometers of the Great Sand Sea.\u003c\/p\u003e\u003cp\u003eThe yellow-green coloration results from trace iron content in the original sand, while the translucent to transparent clarity indicates minimal contamination during the melt phase. Flow textures visible in this specimen record the turbulent conditions during formation, when molten silica cooled rapidly in the air following ejection from the impact site.\u003c\/p\u003e\u003ch2\u003eScientific context\u003c\/h2\u003e\u003cp\u003eLibyan Desert Glass represents one of Earth's largest and oldest impact glass strewn fields. The source crater remains unidentified despite extensive survey work, though candidates include the partially buried Kebira crater structure. The glass composition closely matches local Nubian sandstone, confirming a terrestrial rather than extraterrestrial origin for the source material. Impact glass formations provide direct evidence of cosmic collision events and the extreme conditions they generate. For more information about impact materials and their formation, see \u003ca href=\"\/pages\/learn-about-meteorites\"\u003eLearn About Meteorites\u003c\/a\u003e.\u003c\/p\u003e\u003cp\u003eAncient Egyptians recognized the material's value, incorporating carved pieces into jewelry and ceremonial objects. A scarab carved from Libyan Desert Glass appears in the pectoral ornament discovered in Tutankhamun's burial chamber, demonstrating that this material held significance more than 3,300 years ago.\u003c\/p\u003e\u003ch2\u003eFrequently asked questions\u003c\/h2\u003e\u003cp\u003e\u003cstrong\u003eIs this authentic Libyan Desert Glass?\u003c\/strong\u003e Yes. This specimen was collected from the Great Sand Sea strewn field in Libya in 2024. Each piece includes a certificate of authenticity documenting its provenance from the established impact glass field.\u003c\/p\u003e\u003cp\u003e\u003cstrong\u003eWhat is lechatelierite?\u003c\/strong\u003e Lechatelierite is pure silica glass formed at temperatures above 1,700°C. Natural occurrence requires either meteorite impact or lightning strike conditions. Libyan Desert Glass consists primarily of this high-temperature silica glass phase, distinguishing it from volcanic glasses like obsidian which form at lower temperatures and contain additional minerals.\u003c\/p\u003e\u003cp\u003e\u003cstrong\u003eWhat is included with this specimen?\u003c\/strong\u003e You receive the 353.18g Libyan Desert Glass specimen and certificate of authenticity. No display stand is included.\u003c\/p\u003e\u003cp\u003e\u003cstrong\u003eHow old is Libyan Desert Glass?\u003c\/strong\u003e Radiometric dating places the formation event at approximately 29 million years ago during the Late Oligocene epoch. The glass has remained scattered across the desert surface since that time, subjected to weathering and wind transport.\u003c\/p\u003e\u003cp\u003e\u003cstrong\u003eCan light pass through the specimen?\u003c\/strong\u003e Yes. Libyan Desert Glass ranges from translucent to transparent depending on thickness and inclusion content. This specimen allows light transmission through thinner sections, revealing internal flow structures and color gradations.\u003c\/p\u003e\u003ch2\u003eDisplay and collection value\u003c\/h2\u003e\u003cp\u003eImpact glasses represent direct physical evidence of cosmic collisions, making them scientifically significant additions to meteorite collections. This specimen's substantial weight and translucent quality make it suitable for backlit display, where transmitted light emphasizes the internal structure and coloration. The natural surface textures and flow patterns provide visual interest from multiple viewing angles.\u003c\/p\u003e\u003cp\u003eCollectors value Libyan Desert Glass for its combination of geological rarity, ancient Egyptian historical connection, and distinctive appearance. The material's formation mechanism links it directly to meteorite impact processes, complementing collections focused on extraterrestrial materials and impact phenomena. Browse additional impact-related specimens in our \u003ca href=\"\/collections\/tektites-impactites\"\u003eTektites \u0026amp; Impactites\u003c\/a\u003e collection.\u003c\/p\u003e","brand":"Treasure Coast Meteorite Co.","offers":[{"title":"Default Title","offer_id":44746859577391,"sku":"LIBYAN-DESERT-GLASS-353.18G-INDIVIDUAL","price":600.0,"currency_code":"USD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0726\/9724\/9839\/files\/libyan-desert-glass.png?v=1778458266"},{"product_id":"bir-ounane-001-achondrite-prim-ungrouped-slice-w-coa-6-46g-rare-1-of-16-classifications","title":"Bir Ounane 001 Achondrite-prim Meteorite Slice, Ungrouped, 6.46g, Polished Primitive Crust","description":"\u003ch2\u003ePrimitive achondrite from early planetary evolution\u003c\/h2\u003e\n\u003cp\u003eThis 6.46g polished slice captures material from the earliest stages of planetary differentiation. Bir Ounane 001 represents a transitional state between chondritic and fully differentiated material, preserving textures from incomplete melting and separation processes that occurred in the solar system's first million years. The polished surface reveals the fine-grained matrix and subtle mineral variations characteristic of primitive achondrites, offering direct evidence of how planetesimals evolved from undifferentiated rock into layered worlds.\u003c\/p\u003e\n\u003cp\u003eClassified as Achondrite-prim with no established group affiliation, this meteorite occupies a scientific middle ground. The specimen shows neither the chondrule-rich structure of primitive chondrites nor the clean crystalline texture of fully evolved achondrites. Instead, the slice displays a complex assemblage that records partial differentiation, the interrupted transformation of primordial material under thermal and gravitational forces.\u003c\/p\u003e\n\u003ch2\u003eStructure and features\u003c\/h2\u003e\n\u003cp\u003eThe polished surface exposes a fine-grained groundmass punctuated by mineralogical variations that reflect incomplete separation of silicate phases. Unlike the coarse crystals seen in eucrites or the metallic networks of differentiated bodies, this slice shows textural heterogeneity consistent with material that experienced heating sufficient to begin recrystallization but insufficient to complete planetary layering. Small-scale variations in reflectivity across the polish indicate compositional gradients frozen during early thermal processing.\u003c\/p\u003e\n\u003cp\u003eThe slice preparation emphasizes these subtle structural details. Polishing reveals mineral boundaries and melt features that would remain invisible in a natural state specimen. The thin profile allows transmitted light examination, though the opacity and fine grain size limit this technique compared to thinner petrographic sections.\u003c\/p\u003e\n\u003ch2\u003eScientific context\u003c\/h2\u003e\n\u003cp\u003ePrimitive achondrites represent a rare window into interrupted differentiation. While most meteorite parent bodies either remained completely primitive (chondrites) or differentiated fully into core-mantle-crust structures (producing irons, stony-irons, and evolved achondrites), a small population of bodies experienced intermediate thermal histories. Bir Ounane 001 belongs to this scientifically valuable category, showing evidence of metamorphism and partial melting without complete magmatic processing.\u003c\/p\u003e\n\u003cp\u003eThe ungrouped classification indicates this material does not match the chemical or isotopic signatures of established meteorite clans. Among approximately 75,000 classified meteorites, only sixteen carry the Achondrite-prim designation, placing Bir Ounane 001 within an exceptionally small statistical cohort. This scarcity reflects both the rarity of primitive achondrite parent bodies and the difficulty of recognizing these meteorites in the field, where their appearance can resemble terrestrial rocks. Collectors seeking comprehensive representation of meteorite diversity will find this classification essential, as it documents a transitional stage that most solar system bodies bypassed entirely. For broader meteorite classification context, see \u003ca href=\"\/pages\/learn-about-meteorites\"\u003eLearn About Meteorites\u003c\/a\u003e.\u003c\/p\u003e\n\u003ch2\u003eFrequently asked questions\u003c\/h2\u003e\n\u003cp\u003e\u003cstrong\u003eIs this meteorite authenticated?\u003c\/strong\u003e Yes. Bir Ounane 001 is classified in the Meteoritical Bulletin as Achondrite-prim (ungrouped). You can verify this classification through the \u003ca href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.php?sea=Bir%20Ounane%20001\u0026amp;sfor=names\" rel=\"noopener\" target=\"_blank\"\u003eMeteoritical Bulletin database\u003c\/a\u003e. This specimen includes a certificate of authenticity documenting its provenance and classification status.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat does Achondrite-prim mean?\u003c\/strong\u003e The designation indicates a primitive achondrite, a meteorite that experienced thermal processing beyond the chondritic state but did not undergo complete differentiation into distinct planetary layers. These meteorites preserve evidence of early, incomplete melting and recrystallization that occurred during planetesimal formation.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhy is this meteorite ungrouped?\u003c\/strong\u003e Ungrouped status means Bir Ounane 001's chemical and isotopic composition does not match any established meteorite group. This classification reflects either a unique parent body or insufficient material for comprehensive analysis. Ungrouped meteorites often represent small asteroids that contributed few specimens to Earth's meteorite collection.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat is included with this specimen?\u003c\/strong\u003e You receive the 6.46g polished slice and a certificate of authenticity. No display stand is included unless separately confirmed.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eHow rare are primitive achondrites?\u003c\/strong\u003e Extremely rare. Only sixteen meteorites carry the Achondrite-prim classification among tens of thousands of classified falls and finds. This scarcity makes specimens from this group particularly valuable for comprehensive meteorite collections.\u003c\/p\u003e\n\u003ch2\u003eCollector significance\u003c\/h2\u003e\n\u003cp\u003eBir Ounane 001 addresses a specific gap in systematic meteorite collections. Most collectors accumulate representatives of common chondrite groups and familiar achondrites like eucrites and diogenites, but primitive achondrites receive disproportionately little attention despite their scientific importance. The sixteen-meteorite cohort means acquiring any Achondrite-prim specimen requires deliberate effort, these do not appear regularly in dealer inventories.\u003c\/p\u003e\n\u003cp\u003eThis 6.46g slice offers entry into primitive achondrite collecting at an accessible size. The polished preparation maximizes visibility of internal features while maintaining a specimen large enough for clear visual examination without magnification. For collectors building taxonomically complete collections, this piece fills a classification slot that may not appear again for months or years. Those focusing specifically on ungrouped meteorites or early differentiation processes will find this specimen directly relevant to both themes. Explore related differentiated specimens in our \u003ca href=\"\/collections\/ungrouped-achondrites\"\u003eUngrouped Achondrites\u003c\/a\u003e collection, or examine other primitive material in our \u003ca href=\"\/collections\/stony-meteorites\"\u003eStony Meteorites\u003c\/a\u003e collection.\u003c\/p\u003e\n\u003cp\u003eMeteoritical Bulletin entry: \u003ca href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.php?sea=Bir%20Ounane%20001\u0026amp;sfor=names\" rel=\"noopener\" target=\"_blank\"\u003eBir Ounane 001\u003c\/a\u003e | Classification: Achondrite-prim | Find, Mali, 2022\u003c\/p\u003e","brand":"Treasure Coast Meteorite Co.","offers":[{"title":"Default Title","offer_id":44755658506287,"sku":"BIR-OUNANE-001-6.46G-SLICE","price":95.0,"currency_code":"USD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0726\/9724\/9839\/files\/bir-ounane-001.png?v=1780155729"},{"product_id":"kaalijarv-iron-meteorite-slice-with-neumann-bands-rare-iron-iab-mg-38-39g","title":"Kaalijärv Iron Meteorite Slice, IAB-MG, 38.39g, Neumann Bands","description":"\u003ch2\u003eEtched iron slice with visible shock features\u003c\/h2\u003e\n\u003cp\u003eThis 38.39g slice cuts through the kamacite and taenite crystal structure of Kaalijärv, an iron meteorite linked to a well-documented crater field on Saaremaa Island, Estonia. The slice has been acid-etched to reveal its internal architecture: intersecting kamacite lamellae form the classic Widmanstätten pattern, and within those plates run narrow parallel lines called Neumann bands. These bands represent mechanical twinning in the iron crystal lattice, a permanent record of the shock event that excavated the craters roughly 3,500 years before present.\u003c\/p\u003e\n\u003cp\u003eThe surface finish allows clear observation of both features under ambient light. The Neumann bands appear as dark, thread-like traces cutting across the lighter kamacite zones. Their orientation and density in this slice provide direct evidence of shock direction and intensity. Few iron meteorite specimens display Neumann bands this prominently at a weight class accessible to most collectors.\u003c\/p\u003e\n\u003cp\u003eThe slice measures approximately 75mm by 45mm and has been stabilized after etching to prevent oxidation. No stand is included.\u003c\/p\u003e\n\u003ch2\u003eStructure and features\u003c\/h2\u003e\n\u003cp\u003eThe Widmanstätten pattern forms when kamacite (low-nickel iron) exsolves from taenite (high-nickel iron) during cooling rates of approximately one to several hundred degrees Celsius per million years. This specimen cooled within the metallic core of a disrupted asteroid, allowing the nickel-iron alloy to crystallize along preferred octahedral planes. The resulting structure consists of kamacite plates separated by taenite ribbons, with plate widths in the medium range typical of IAB-MG octahedrites.\u003c\/p\u003e\n\u003cp\u003eNeumann bands are crystallographic twins produced when shock waves exceed the elastic limit of kamacite. The twins form on specific lattice planes and remain as permanent deformation features. In this slice, the bands run in multiple orientations, reflecting the complex stress field of the impact that formed the Kaalijärv crater field. The bands are most visible within the wider kamacite lamellae where etching contrast is strongest.\u003c\/p\u003e\n\u003cp\u003eThe slice also shows minor surface pitting and small inclusions of troilite (iron sulfide), common accessory phases in IAB irons. The etched surface has developed a light patina that enhances structural contrast without obscuring fine detail.\u003c\/p\u003e\n\u003ch2\u003eScientific context\u003c\/h2\u003e\n\u003cp\u003eIAB meteorites belong to a complex group of iron meteorites with heterogeneous compositions and structures. Unlike magmatic irons that crystallized from molten metal pools, IAB irons likely formed through impact melting and reassembly of silicate-metal mixtures on a partially differentiated parent body. This formation mechanism explains the chemical and textural diversity within the IAB group, which includes both coarse and fine octahedrites as well as silicate-bearing inclusions.\u003c\/p\u003e\n\u003cp\u003eKaalijärv material specifically represents the medium-grained (MG) subgroup, characterized by kamacite bandwidth and nickel content intermediate within the IAB range. The presence of well-developed Neumann bands indicates that this meteoroid experienced at least one significant shock event prior to atmospheric entry, possibly related to the same collisional history that eventually ejected it from the asteroid belt and sent it toward Earth.\u003c\/p\u003e\n\u003cp\u003eThe fall itself occurred during the Bronze Age, making it one of the youngest meteorite impact events with observable craters. Archaeological evidence suggests the impacts may have influenced local settlement patterns and cultural development. For collectors interested in the broader science of meteorite identification and classification, see \u003ca href=\"\/pages\/learn-about-meteorites\"\u003eLearn About Meteorites\u003c\/a\u003e.\u003c\/p\u003e\n\u003ch2\u003eFrequently asked questions\u003c\/h2\u003e\n\u003cp\u003e\u003cstrong\u003eIs this meteorite authenticated?\u003c\/strong\u003e Kaalijärv is classified in the Meteoritical Bulletin as an iron meteorite (IAB-MG octahedrite). You can verify this classification through the \u003ca rel=\"noopener\" href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.php?sea=Kaalijarv\u0026amp;sfor=names\" target=\"_blank\"\u003eMeteoritical Bulletin search\u003c\/a\u003e. This specimen includes a certificate of authenticity documenting its weight, classification, and provenance.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat are Neumann bands?\u003c\/strong\u003e Neumann bands are shock-induced deformation features in kamacite (low-nickel iron). When a meteorite experiences high-pressure impacts, the crystal lattice undergoes mechanical twinning along specific planes. These twins appear as parallel lines within individual kamacite plates after etching. They provide direct evidence of shock history and are scientifically valuable markers of impact processes.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat is included with this specimen?\u003c\/strong\u003e The specimen weighs 38.39g and includes a certificate of authenticity. No display stand is included.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eHow should I store an etched iron meteorite?\u003c\/strong\u003e Store in a low-humidity environment. Etched surfaces are more reactive to moisture than polished or natural surfaces. A silica gel pack in the storage container helps prevent oxidation. Light mineral oil applied to the surface provides additional protection but may slightly darken the patina.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhy is Kaalijärv significant to collectors?\u003c\/strong\u003e Kaalijärv is one of the few iron meteorites directly associated with a known crater field and a specific historical timeframe. The impact occurred within recorded human history, approximately 3,500 years before present. This connection between material sample and terrestrial impact site makes it both geologically and culturally notable.\u003c\/p\u003e\n\u003ch2\u003eCollector significance\u003c\/h2\u003e\n\u003cp\u003eIron meteorites with visible Neumann bands represent a small subset of available material. Most irons show only Widmanstätten structure; bands require specific shock conditions and favorable crystal orientation relative to the cut plane. This 38.39g slice offers both features at a size and price point accessible to intermediate collectors building reference collections of impact phenomena.\u003c\/p\u003e\n\u003cp\u003eKaalijärv also occupies a position between common witnessed falls and high-end rarities. The total known weight from the crater field is substantial enough to support availability, but etched slices with prominent shock features remain selectively distributed. Material from this locality has been held in institutional collections for decades, establishing its scientific pedigree.\u003c\/p\u003e\n\u003cp\u003eFor collectors building comprehensive iron meteorite reference sets, see our full \u003ca href=\"\/collections\/iron-meteorites\"\u003eIron Meteorites\u003c\/a\u003e collection.\u003c\/p\u003e\n\u003cp\u003eMeteoritical Bulletin entry: \u003ca rel=\"noopener\" href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.php?sea=Kaalijarv\u0026amp;sfor=names\" target=\"_blank\"\u003eKaalijarv\u003c\/a\u003e | Classification: Iron meteorite (IAB-MG octahedrite) | Find, Estonia, 1937\u003c\/p\u003e","brand":"Treasure Coast Meteorite Co.","offers":[{"title":"Default Title","offer_id":44814229143599,"sku":"KAALIJARV-38.39G-SLICE","price":460.0,"currency_code":"USD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0726\/9724\/9839\/files\/kaalijarv-iron-meteorite-slice-iab-mg-neumann-bands-estonia-38-39g.heic?v=1774156498"},{"product_id":"nwa-18048-eucrite-pmict-meteorite-hed-large-mirror-polished-slice-120-00g","title":"NWA 18048 Eucrite-pmict Meteorite Slice, 120.00g, Mirror Polished HED Achondrite from Vesta","description":"\u003ch2\u003eMirror-polished polymict eucrite with vivid clast structure\u003c\/h2\u003e\n\u003cp\u003eThis 120.00g slice showcases the complex architecture of a polymict eucrite breccia. The mirror polish on one face reveals distinct light and dark clasts suspended in an impact-processed matrix. Lighter eucritic fragments contrast sharply against darker melt zones, creating a mosaic that documents Vesta's violent surface history. The finish brings out fine-scale details invisible in rough specimens: clast boundaries, melt veins threading between fragments, and variations in mineral grain size across different lithologies.\u003c\/p\u003e\n\u003cp\u003eAt 120.00g, this specimen offers substantial display presence. The slice is large enough to show the full spectrum of polymict textures while remaining manageable for cabinet storage. The mirror polish eliminates surface irregularities that can obscure internal features, making this piece suitable for detailed examination under magnification or display lighting.\u003c\/p\u003e\n\u003ch2\u003eBrecciation and impact melt architecture\u003c\/h2\u003e\n\u003cp\u003eThe slice preserves multiple generations of impact processing. Eucritic clasts, fragments of basaltic crust from Vesta's surface, appear as angular to subangular inclusions. These clasts vary in size and composition, indicating they were excavated from different depths or locations on the asteroid before being mixed together. The matrix surrounding these fragments contains impact melt, dark material formed when kinetic energy from high-velocity collisions liquefied rock.\u003c\/p\u003e\n\u003cp\u003eMelt veins cut through the specimen in irregular pathways. These veins represent shock-melted material that intruded into fractures during impact events. The thickness and distribution of these veins indicate the intensity of the collisions that created this breccia. Some clasts show sharp, well-defined boundaries against the matrix, while others grade into surrounding material, suggesting partial melting or recrystallization at their margins.\u003c\/p\u003e\n\u003ch2\u003eVesta's basaltic crust and HED meteorite formation\u003c\/h2\u003e\n\u003cp\u003eNWA 18048 originated from asteroid 4 Vesta, the second-largest body in the asteroid belt. NASA's Dawn spacecraft confirmed that eucrites, diogenites, and howardites, collectively called HED meteorites, come from Vesta's differentiated crust and mantle. Eucrites specifically represent basaltic material from Vesta's surface, formed when the asteroid's interior melted early in solar system history. Magma rose to the surface and crystallized into basaltic crust, similar to lunar mare basalts or terrestrial flood basalts.\u003c\/p\u003e\n\u003cp\u003ePolymict eucrites like this specimen formed when massive impacts shattered Vesta's crust, mixing fragments from different crustal layers. The mixing process created breccias containing both pristine eucritic material and impact-modified components. Study of these meteorites has revealed Vesta's thermal history, differentiation processes, and the role of impact bombardment in shaping asteroid surfaces. For more context on meteorite classification and identification, see \u003ca href=\"\/pages\/learn-about-meteorites\"\u003eLearn About Meteorites\u003c\/a\u003e.\u003c\/p\u003e\n\u003ch2\u003eFrequently asked questions\u003c\/h2\u003e\n\u003cp\u003e\u003cstrong\u003eIs this meteorite authenticated?\u003c\/strong\u003e Yes. NWA 18048 is classified in the Meteoritical Bulletin as a eucrite-pmict. You can verify the classification here: \u003ca href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.php?sea=NWA%2018048\u0026amp;sfor=names\" rel=\"noopener\" target=\"_blank\"\u003eMeteoritical Bulletin entry for NWA 18048\u003c\/a\u003e. This specimen includes a certificate of authenticity documenting its classification, weight, and origin.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat does \"pmict\" mean in the classification?\u003c\/strong\u003e The abbreviation \"pmict\" stands for polymict, indicating this eucrite is a breccia containing multiple rock types. Unlike monomict eucrites (single-composition rocks), polymict eucrites contain clasts of different compositions mixed together during impact events. This specimen contains eucritic basalt fragments, impact melt, and possibly minor amounts of other HED material, all welded together by subsequent impacts.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhy is this specimen mirror polished?\u003c\/strong\u003e Mirror polishing removes surface irregularities and reveals internal structure with maximum clarity. The technique uses progressively finer abrasives to create an optically smooth surface that reflects light uniformly. This finish allows detailed examination of clast boundaries, melt veins, and mineral textures that would be obscured on a rough or sawn surface. It also makes the specimen suitable for photomicrography and educational display.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat is included with this specimen?\u003c\/strong\u003e You receive the 120.00g mirror-polished slice and a certificate of authenticity. The certificate documents the meteorite's classification, weight, and find location. No display stand is included.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eHow did this meteorite reach Earth from Vesta?\u003c\/strong\u003e Large impacts on Vesta ejected fragments into space at velocities exceeding the asteroid's escape velocity (approximately 360 meters per second). These fragments entered independent orbits around the Sun, where gravitational interactions with planets gradually altered their trajectories. Eventually, some fragments intersected Earth's orbit and fell as meteorites. The process can take millions of years from initial ejection to atmospheric entry.\u003c\/p\u003e\n\u003ch2\u003eDisplay-grade HED specimen for planetary collections\u003c\/h2\u003e\n\u003cp\u003eCollectors focused on differentiated asteroids prioritize polymict eucrites for their scientific and visual complexity. This 120.00g slice combines size, structural clarity, and professional preparation. The mirror polish eliminates the preparation artifacts common in hastily finished specimens, saw marks, uneven surfaces, edge chipping, that detract from serious collections.\u003c\/p\u003e\n\u003cp\u003eLarge eucrite slices are underrepresented in the market compared to chondrites or common iron meteorites. Most NWA finds are recovered as small fragments requiring reassembly or irregular pieces unsuitable for full polishing. A complete slice at this weight, showing clear polymict textures across its entire face, represents a specimen tier above typical dealer offerings. For collectors building comprehensive HED suites, explore our complete \u003ca href=\"\/collections\/eucrites\"\u003eEucrites\u003c\/a\u003e and \u003ca href=\"\/collections\/hed-meteorites\"\u003eHED Meteorites\u003c\/a\u003e collections.\u003c\/p\u003e\n\u003cp\u003eMeteoritical Bulletin entry: \u003ca href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.php?sea=NWA%2018048\u0026amp;sfor=names\" rel=\"noopener\" target=\"_blank\"\u003eNWA 18048\u003c\/a\u003e | Classification: Eucrite-pmict | Find, Northwest Africa, 2024\u003c\/p\u003e","brand":"Treasure Coast Meteorite Co.","offers":[{"title":"Default Title","offer_id":44859333312559,"sku":"NWA-18048-120.00G-SLICE-MP","price":480.0,"currency_code":"USD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0726\/9724\/9839\/files\/IMG_7549.heic?v=1768190492"},{"product_id":"erg-chech-002-0-8g-ungrouped-achondrite-red-individual","title":"Erg Chech 002 Ungrouped Achondrite Meteorite Individual, Achondrite-ung, 0.80g, Andesitic Crust Fragment","description":"\u003ch2\u003eA fragment of the oldest volcanic crust\u003c\/h2\u003e\u003cp\u003eThis 0.80g individual preserves the andesitic composition that distinguishes Erg Chech 002 from all other achondrites in world collections. The specimen displays noticeable reddish-brown terrestrial staining across portions of the surface and interior matrix, consistent with the Saharan Desert environment where this meteorite was recovered in 2020. The Meteoritical Bulletin reports minor goethite as a secondary weathering product in EC 002 specimens, a direct result of groundwater interaction in the find location.\u003c\/p\u003e\u003cp\u003eThe surface shows the characteristic gray-green matrix typical of this meteorite's pyroxene-plagioclase assemblage, with staining concentrated in fractures and exposed interior surfaces. This individual retains its natural exterior geometry from the breakup of the parent mass during atmospheric entry or ground impact.\u003c\/p\u003e\u003ch2\u003eAndesitic mineralogy and texture\u003c\/h2\u003e\u003cp\u003eErg Chech 002 consists predominantly of plagioclase feldspar and pyroxene crystals in proportions that match terrestrial andesite, a volcanic rock type commonly found in subduction zones on Earth. This mineralogy requires formation through partial melting and fractional crystallization in a silica-rich magma system, processes that occurred on a differentiated protoplanet with a defined crust-mantle boundary.\u003c\/p\u003e\u003cp\u003eThe fine-grained texture indicates rapid cooling at or near the surface of its parent body, consistent with extrusive volcanism. This specimen preserves that crystallization history in a hand-sized fragment representing crustal geology from the first few million years of solar system formation.\u003c\/p\u003e\u003ch2\u003eScientific context\u003c\/h2\u003e\u003cp\u003eErg Chech 002 crystallized approximately 4.565 billion years ago, making it older than any other volcanic rock yet analyzed. This age predates the formation of Earth's crust by tens of millions of years. The meteorite formed on a protoplanet that achieved full differentiation into core, mantle, and crust before catastrophic disruption during the early bombardment phase of solar system evolution. No parent body has been identified; the protoplanet that produced this crust no longer exists as an intact object.\u003c\/p\u003e\u003cp\u003eThe andesitic composition indicates a complex magmatic evolution rare among differentiated asteroids, most of which produced basaltic or ultramafic crustal rocks. Erg Chech 002 demonstrates that protoplanetary volcanism in the early solar system was more geologically diverse than the surviving asteroid belt suggests. Collectors seeking specimens that document primordial planetary processes will find few examples with greater scientific significance. For comprehensive context on meteorite classification systems and formation mechanisms, see \u003ca href=\"\/pages\/learn-about-meteorites\"\u003eLearn About Meteorites\u003c\/a\u003e.\u003c\/p\u003e\u003ch2\u003eFrequently asked questions\u003c\/h2\u003e\u003cp\u003e\u003cstrong\u003eIs this meteorite authenticated?\u003c\/strong\u003e Erg Chech 002 is classified in the Meteoritical Bulletin as an ungrouped achondrite. Meteoritical Bulletin entry: \u003ca href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.php?sea=Erg%20Chech%20002\u0026amp;sfor=names\" target=\"_blank\" rel=\"noopener\"\u003eErg Chech 002\u003c\/a\u003e. This specimen includes a certificate of authenticity documenting its classification and provenance.\u003c\/p\u003e\u003cp\u003e\u003cstrong\u003eWhat does the reddish-brown staining indicate?\u003c\/strong\u003e The staining results from terrestrial weathering in the Algerian Sahara, where groundwater introduced iron-bearing minerals into fractures and porous regions of the meteorite. The Meteoritical Bulletin identifies goethite as a weathering product in EC 002 specimens. This staining does not affect the specimen's scientific integrity or primary mineralogy.\u003c\/p\u003e\u003cp\u003e\u003cstrong\u003eWhat is included with this specimen?\u003c\/strong\u003e This listing includes the 0.80g individual meteorite and a certificate of authenticity. No display stand is included.\u003c\/p\u003e\u003cp\u003e\u003cstrong\u003eWhat does \"ungrouped achondrite\" mean?\u003c\/strong\u003e Ungrouped achondrites do not fit into established meteorite groups based on mineralogy, oxygen isotopes, or chemistry. Erg Chech 002's andesitic composition and ancient age distinguish it from HED meteorites, lunar samples, Martian meteorites, and all other classified achondrite groups, placing it in its own category.\u003c\/p\u003e\u003cp\u003e\u003cstrong\u003eWhy is the age of this meteorite significant?\u003c\/strong\u003e At 4.565 billion years, Erg Chech 002 crystallized within the first few million years of the solar system's existence, before most planetary bodies had completed differentiation. It represents a snapshot of crustal geology from a time period for which no other volcanic samples are available, making it the oldest known piece of planetary crust.\u003c\/p\u003e\u003ch2\u003eCollector significance\u003c\/h2\u003e\u003cp\u003eErg Chech 002 stands alone among meteorites for its combination of extreme age, andesitic composition, and protoplanetary origin. No other specimen type in private hands represents volcanic crust from the first epoch of planetary formation. The 2020 recognition of this meteorite expanded the known diversity of early solar system geology and provided the first andesitic sample from beyond Earth.\u003c\/p\u003e\u003cp\u003eThis 0.80g individual offers an accessible entry point into one of the most scientifically important meteorite finds of the 21st century. The visible weathering staining provides a documentary record of the specimen's terrestrial residence time while preserving the primary igneous texture beneath. For collectors building representative suites of achondrite types, Erg Chech 002 fills a category no other meteorite can occupy. Additional ungrouped achondrite specimens and related differentiated meteorite types are available in the \u003ca href=\"\/collections\/ungrouped-achondrites\"\u003eUngrouped Achondrites\u003c\/a\u003e collection.\u003c\/p\u003e\u003cp\u003eMeteoritical Bulletin entry: \u003ca href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.php?sea=Erg%20Chech%20002\u0026amp;sfor=names\" target=\"_blank\" rel=\"noopener\"\u003eErg Chech 002\u003c\/a\u003e | Classification: Achondrite-ung | Find, Algeria, 2020\u003c\/p\u003e","brand":"Treasure Coast Meteorite Co.","offers":[{"title":"Default Title","offer_id":44864528384047,"sku":"ERG-CHECH-002-0.8G-INDIVIDUAL","price":80.0,"currency_code":"USD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0726\/9724\/9839\/files\/erg-chech-002-ungrouped-achondrite-0-8g-front-view.heic?v=1769834996"},{"product_id":"gebel-kamil-550g-whole-shrapnel-iron-meteorite","title":"Gebel Kamil Iron Meteorite Individual, Ungrouped Ataxite, 550.00g, Impact Crater Specimen","description":"\u003ch2\u003eWhole shrapnel fragment from one of Earth's youngest impact craters\u003c\/h2\u003e\n\u003cp\u003eThis 550.00g Gebel Kamil whole shrapnel fragment preserves the structural signature of hypervelocity impact in unusually clear form. The specimen displays pronounced lizard skin texture across its outer surfaces, well-defined shear lines running through the metal, and rollover lips along the fragment edges where the iron plastically deformed during disintegration. The piece is intact and uncut, recovered from the strewnfield surrounding the 45-meter Kamil Crater in Egypt's southwestern desert, formed less than 5,000 years ago.\u003c\/p\u003e\n\u003cp\u003eThe visible features document the mechanics of the impact itself rather than atmospheric entry. The lizard skin surface forms the characteristic rough, dark-brown exterior of \u003ca href=\"\/collections\/gebel-kamil\"\u003eGebel Kamil shrapnel\u003c\/a\u003e, produced as the impactor disintegrated against the quartz-arenite target rock. Shear lines trace the curvilinear deformation bands that propagated through the mass during fragmentation, recording the direction and intensity of the shock event. Rollover lips along multiple edges show where ductile metal curled and folded as it tore away from neighboring fragments at impact.\u003c\/p\u003e\n\u003ch3\u003eAtaxite structure and composition\u003c\/h3\u003e\n\u003cp\u003eGebel Kamil is classified as an ungrouped \u003ca href=\"\/collections\/iron-meteorites\"\u003eiron meteorite\u003c\/a\u003e, a Ni-rich ataxite per the Meteoritical Bulletin No. 95 (Weisberg et al., 2010). Ataxites lack the crystalline Widmanstätten pattern characteristic of octahedrites, instead forming a fine-grained nickel-iron structure too Ni-rich for visible kamacite and taenite banding to develop under acid etching. Gebel Kamil specifically assays approximately 20 wt percent Ni, 0.75 wt percent Co, with unusually high Ge and Ga contents and a very fine-grained duplex plessite matrix.\u003c\/p\u003e\n\u003cp\u003eThe \"ungrouped\" designation means Gebel Kamil's bulk chemistry does not fall within any of the established iron meteorite chemical groups (IAB, IIAB, IIIAB, IVA, IVB, etc.). It derives from a distinct, otherwise-unrepresented parent body. Accessory mineral phases identified in Gebel Kamil include schreibersite, troilite, daubréelite, and trace native copper.\u003c\/p\u003e\n\u003ch3\u003eScientific context\u003c\/h3\u003e\n\u003cp\u003eThe Kamil Crater is one of the best-preserved young impact structures on Earth. Identified via Google Earth imagery in 2009 by V. De Michele, the crater was confirmed by Italian-Egyptian field expeditions in February 2009 and 2010, which recovered approximately 1.6 metric tons of meteoritic material from in and around the 45-meter structure. The crater excavates Cretaceous sandstone bedrock and remains exceptionally well preserved due to the hyperarid climate of the East Uweinat Desert.\u003c\/p\u003e\n\u003cp\u003eGebel Kamil represents a complete impact system: crater morphology, ejecta distribution, and the recovered impactor material itself. This correlation has enabled detailed reconstruction of impact velocity, angle, and energy release. The structure formed during human prehistory, less than 5,000 years ago, though no historical or archaeological records document the event. Gebel Kamil belongs to a small group of impact sites worldwide where the impactor has been recovered and formally classified. \u003ca href=\"\/pages\/learn-about-meteorites\"\u003eLearn about meteorites\u003c\/a\u003e for further reading on crater formation and impact-recovered material.\u003c\/p\u003e\n\u003ch3\u003eFrequently asked questions\u003c\/h3\u003e\n\u003cp\u003e\u003cstrong\u003eIs this meteorite authenticated?\u003c\/strong\u003e Yes. Gebel Kamil is classified in the Meteoritical Bulletin as Iron, ungrouped (Ni-rich ataxite). You can verify the classification here: \u003ca href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.cfm?code=52031\" rel=\"noopener\" target=\"_blank\"\u003eGebel Kamil\u003c\/a\u003e. This specimen ships with a certificate of authenticity from Treasure Coast Meteorite Co. (IMCA #3323).\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat does ungrouped ataxite mean?\u003c\/strong\u003e Ataxites are iron meteorites with sufficiently high nickel content that visible Widmanstätten patterns do not form under standard etching. Ungrouped means Gebel Kamil's chemistry does not match any established iron meteorite group, indicating a distinct parent body in the asteroid belt.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat is shrapnel, and how does it differ from a regmaglypted individual?\u003c\/strong\u003e Shrapnel refers to fragments produced when a meteorite disintegrates on impact rather than during atmospheric flight. Of the approximately 1.6 metric tons of Gebel Kamil recovered, almost all of it is shrapnel. Only a single 83 kg specimen was found as a complete regmaglypted individual. This piece is whole shrapnel: an intact, uncut fragment from the explosive impact, displaying the shear and rollover features that distinguish crater-recovered material.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat are shear lines and rollover lips?\u003c\/strong\u003e Shear lines are curvilinear bands of deformation that record the direction of shock propagation through the metal at the moment of impact. Rollover lips are folds and curls along fragment edges where the ductile nickel-iron deformed plastically as fragments separated. Both are hallmarks of hypervelocity impact disintegration and are found primarily in crater-recovered material.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat is included with this specimen?\u003c\/strong\u003e The 550.00g Gebel Kamil whole shrapnel fragment, certificate of authenticity, and specimen card with full classification details. No display stand is included.\u003c\/p\u003e\n\u003ch3\u003eCollector significance\u003c\/h3\u003e\n\u003cp\u003eGebel Kamil occupies a position few \u003ca href=\"\/collections\/iron-meteorites\"\u003eiron meteorites\u003c\/a\u003e can match: a classified ungrouped specimen with confirmed crater association, recovered under controlled scientific survey, with visible structural evidence of the impact event itself. Whole shrapnel fragments at the 550g range, displaying clear lizard skin, well-defined shear lines, and intact rollover lips on a single uncut piece, are uncommon. Most material in this weight class has been cut down for slice production, making intact fragments increasingly difficult to source as the original recovery stock is dispersed.\u003c\/p\u003e\n\u003cp\u003eThe combination of mass, surface preservation, and structural detail on this fragment makes it both a strong display piece and a meaningful portfolio addition for collectors focused on crater-recovered material. Specimens from Gebel Kamil connect the buyer to a specific, identifiable geological event, a category of meteorite that remains a small minority of what has ever been classified.\u003c\/p\u003e\n\u003cp\u003e \u003c\/p\u003e\n\u003cp\u003eMeteoritical Bulletin entry: \u003ca rel=\"noopener\" href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.cfm?code=52031\" target=\"_blank\"\u003eGebel Kamil\u003c\/a\u003e | Classification: Iron (ungrouped, ataxite) | Find, Egypt, 2009\u003c\/p\u003e","brand":"Treasure Coast Meteorite Co.","offers":[{"title":"Default Title","offer_id":45328332488751,"sku":"GEBEL-KAMIL-550.00G-INDIVIDUAL","price":1100.0,"currency_code":"USD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0726\/9724\/9839\/files\/gebel-kamil-550g-shrapnel-fold-shear-detail.jpg?v=1779329747"},{"product_id":"nwa-18592-mesosiderite-meteorite-complete-individual-stony-iron-161-00g-remnant-fusion-crust","title":"NWA 18592 Mesosiderite Meteorite Complete Individual, Stony-Iron, 161.00g, Remnant Fusion Crust","description":"\u003ch2\u003eA complete individual mesosiderite with remnant fusion crust\u003c\/h2\u003e\n\u003cp\u003eNWA 18592 is a 161.00g complete individual stony-iron meteorite from the mesosiderite class, displaying remnant patches of black fusion crust against the weathered exterior. Mesosiderites are one of the rarest meteorite types known, comprising less than 0.3% of all classified falls and finds. This specimen was recovered in Northwest Africa, classified in 2026 by \u003cmeta charset=\"utf-8\"\u003e\u003cspan\u003eD. Sheikh\u003c\/span\u003e at Cascadia Meteorite Laboratory, and accepted by the Meteoritical Society in May 2026.\u003c\/p\u003e\n\u003cp\u003eThe complete individual form means this specimen retains its full atmospheric entry shape rather than being cut from a larger mass. The dark fusion crust, formed during the brief seconds when the meteorite blazed through Earth atmosphere, remains visible across portions of the surface. Mesosiderites are mixtures of roughly equal parts metallic iron-nickel and silicate rock, making them visually and structurally distinct from any other meteorite class.\u003c\/p\u003e\n\u003ch2\u003eStructure and features\u003c\/h2\u003e\n\u003cp\u003eMesosiderites display a brecciated texture in which metallic iron-nickel and silicate clasts are intermingled in roughly equal proportions. The silicate component of NWA 18592 contains low-calcium pyroxene clasts up to 1 millimeter, often with high-calcium pyroxene inclusions, along with lesser plagioclase feldspar. Accessory minerals include silica, merrillite, troilite, and chromite. The classification work documents moderate shock and moderate weathering throughout the specimen.\u003c\/p\u003e\n\u003cp\u003eThe metallic phase in this specimen has been substantially converted to iron hydroxide weathering products, common in mesosiderites recovered from desert finds. Patches of original fusion crust survive on portions of the exterior, dark and contrasting against the weathered surface. As a complete individual the specimen carries a distinctive sculpted exterior shape produced by ablation during atmospheric passage.\u003c\/p\u003e\n\u003ch2\u003eDiscovery and provenance\u003c\/h2\u003e\n\u003cp\u003eNWA 18592 was recovered in Northwest Africa in 2024 and submitted for classification through Cascadia Meteorite Laboratory. The total known weight is 903 grams distributed across 11 stones, with the main mass held by Brian McDonald. A 24.6 gram type specimen is held at Cascadia. Classification was completed by D. Sheikh and accepted into the official record in May 2026, published in the Meteoritical Bulletin Database.\u003c\/p\u003e\n\u003cp\u003eGeochemical analysis confirmed mesosiderite classification with low-calcium pyroxene composition of Fs33.8 plus or minus 1.3 and Wo3.7 plus or minus 0.4, high-calcium pyroxene composition of Fs18.4 plus or minus 2.0 and Wo38.5 plus or minus 3.2, and plagioclase composition of An94.6 plus or minus 1.6. These compositional ranges are diagnostic of the mesosiderite parent body and distinguish this specimen from other stony-iron meteorites such as pallasites.\u003c\/p\u003e\n\u003ch2\u003eScientific context\u003c\/h2\u003e\n\u003cp\u003eMesosiderites represent one of the most puzzling meteorite classes known. Their formation requires the violent mixing of crustal silicates with molten metallic core material, a combination that is difficult to reconcile with standard models of asteroid differentiation. The leading hypothesis involves a catastrophic collision between a differentiated parent body and the metallic core of a smaller asteroid, with the resulting debris recombining under conditions that allowed both phases to coexist in roughly equal abundance.\u003c\/p\u003e\n\u003cp\u003eThe presence of low-calcium and high-calcium pyroxenes along with calcium-rich plagioclase places mesosiderites in the broader igneous achondrite family, sharing some compositional similarities with HED meteorites believed to originate from Vesta. The high metal content separates mesosiderites from the achondrites and places them in the stony-iron meteorite group along with pallasites, though the two classes formed under very different conditions.\u003c\/p\u003e\n\u003ch2\u003eFrequently asked questions\u003c\/h2\u003e\n\u003cp\u003e\u003cstrong\u003eIs this meteorite authenticated?\u003c\/strong\u003e Yes. NWA 18592 is an officially classified meteorite. See the \u003ca href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.cfm?code=87168\" rel=\"noopener\" target=\"_blank\"\u003eofficial Meteoritical Bulletin entry\u003c\/a\u003e. This specimen includes a Certificate of Authenticity issued by Treasure Coast Meteorite Co., IMCA #3323.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat makes a mesosiderite different from other stony-iron meteorites?\u003c\/strong\u003e Stony-iron meteorites come in two classes: pallasites and mesosiderites. Pallasites contain olivine crystals embedded in iron-nickel metal and formed at the core-mantle boundary of a differentiated asteroid. Mesosiderites contain brecciated silicate clasts mixed with metal in roughly equal proportions and formed through catastrophic impact mixing. They are visually and texturally distinct.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat is fusion crust and why does it matter?\u003c\/strong\u003e Fusion crust is the dark glassy coating produced when a meteorite passes through Earth atmosphere at hypersonic velocity. The outer layer of the stone briefly melts and then solidifies as the meteorite slows below ablation speed. Surviving fusion crust is a key authentication feature and is more commonly preserved on complete individuals than on cut specimens.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat does complete individual mean?\u003c\/strong\u003e A complete individual is a meteorite that has not been cut, sliced, or fragmented since recovery. It retains its full atmospheric entry shape, including any fusion crust, oriented features, and regmaglypts. Complete individuals are generally more desirable to collectors than cut fragments of equal weight because they preserve the natural form of the specimen.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat is included?\u003c\/strong\u003e The specimen pictured plus a printed Certificate of Authenticity. The COA documents the official classification, weight, and provenance through Treasure Coast Meteorite Co., IMCA member #3323.\u003c\/p\u003e\n\u003ch2\u003eCollector significance\u003c\/h2\u003e\n\u003cp\u003eMesosiderites are among the rarest meteorite classes, comprising fewer than 250 distinct classifications worldwide and representing less than 0.3% of the entire meteorite catalog. NWA 18592 was newly classified in 2026 with a modest 903 gram total known weight distributed across 11 stones, which places it among the smaller mesosiderite finds and increases the relative importance of each surviving piece. The complete individual form with surviving fusion crust makes this specimen particularly desirable for collectors building a representative stony-iron section.\u003c\/p\u003e\n\u003cp\u003eMeteoritical Bulletin entry: \u003ca href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.cfm?code=87168\" rel=\"noopener\" target=\"_blank\"\u003e903g TKW | MB 114 (2026)\u003c\/a\u003e\u003c\/p\u003e\n\u003cp\u003e \u003c\/p\u003e","brand":"Treasure Coast Meteorite Co.","offers":[{"title":"Default Title","offer_id":45377993670703,"sku":null,"price":805.0,"currency_code":"USD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0726\/9724\/9839\/files\/NWA-18592-Mesosiderite-161g-Hero-White.jpg?v=1779408328"},{"product_id":"gebel-kamil-iron-meteorite-individual-ungrouped-ataxite-1414-00g-impact-crater-specimen","title":"Gebel Kamil Iron Meteorite Individual, Ungrouped Ataxite, 1414.00g, Impact Crater Specimen","description":"\u003ch2\u003eWhole shrapnel fragment from one of Earth's youngest impact craters\u003c\/h2\u003e\n\u003cp\u003eAt 1414 grams, this is a substantial Gebel Kamil whole shrapnel fragment, large enough to fill the hand (see the in-hand image) and heavy in a way that smaller fragments simply are not. As the photographs show from several angles, the specimen carries pronounced lizard skin texture across its outer surfaces, well-defined shear lines running through the metal, and rollover lips along the fragment edges where the iron deformed plastically during disintegration. The piece is intact and uncut, recovered from the strewnfield surrounding the 45-meter Kamil Crater in Egypt's southwestern desert, a structure formed less than 5,000 years ago.\u003c\/p\u003e\n\u003cp\u003eThe macro images make these features easy to read, and they document the mechanics of the impact itself rather than atmospheric entry. The lizard skin surface forms the characteristic rough, dark-brown exterior of \u003ca href=\"\/collections\/gebel-kamil\"\u003eGebel Kamil shrapnel\u003c\/a\u003e, produced as the impactor disintegrated against the quartz-arenite target rock. Shear lines trace the curvilinear deformation bands that propagated through the mass during fragmentation, recording the direction and intensity of the shock event. Rollover lips along multiple edges show where ductile metal curled and folded as it tore away from neighboring fragments at impact.\u003c\/p\u003e\n\u003ch3\u003eAtaxite structure and composition\u003c\/h3\u003e\n\u003cp\u003eGebel Kamil is classified as an ungrouped \u003ca href=\"\/collections\/iron-meteorites\"\u003eiron meteorite\u003c\/a\u003e, a Ni-rich ataxite per the Meteoritical Bulletin No. 95 (Weisberg et al., 2010). Ataxites lack the crystalline Widmanstätten pattern characteristic of octahedrites, instead forming a fine-grained nickel-iron structure too Ni-rich for visible kamacite and taenite banding to develop under acid etching. Gebel Kamil specifically assays approximately 20 wt percent Ni, 0.75 wt percent Co, with unusually high Ge and Ga contents and a very fine-grained duplex plessite matrix.\u003c\/p\u003e\n\u003cp\u003eThe \"ungrouped\" designation means Gebel Kamil's bulk chemistry does not fall within any of the established iron meteorite chemical groups (IAB, IIAB, IIIAB, IVA, IVB, etc.). It derives from a distinct, otherwise-unrepresented parent body. Accessory mineral phases identified in Gebel Kamil include schreibersite, troilite, daubréelite, and trace native copper.\u003c\/p\u003e\n\u003ch3\u003eScientific context\u003c\/h3\u003e\n\u003cp\u003eThe Kamil Crater is one of the best-preserved young impact structures on Earth. Identified via Google Earth imagery in 2009 by V. De Michele, the crater was confirmed by Italian-Egyptian field expeditions in February 2009 and 2010, which recovered approximately 1.6 metric tons of meteoritic material from in and around the 45-meter structure. The crater excavates Cretaceous sandstone bedrock and remains exceptionally well preserved due to the hyperarid climate of the East Uweinat Desert.\u003c\/p\u003e\n\u003cp\u003eGebel Kamil represents a complete impact system: crater morphology, ejecta distribution, and the recovered impactor material itself. This correlation has enabled detailed reconstruction of impact velocity, angle, and energy release. The structure formed during human prehistory, less than 5,000 years ago, though no historical or archaeological records document the event. Gebel Kamil belongs to a small group of impact sites worldwide where the impactor has been recovered and formally classified. \u003ca href=\"\/pages\/learn-about-meteorites\"\u003eLearn about meteorites\u003c\/a\u003e for further reading on crater formation and impact-recovered material.\u003c\/p\u003e\n\u003ch3\u003eFrequently asked questions\u003c\/h3\u003e\n\u003cp\u003e\u003cstrong\u003eIs this meteorite authenticated?\u003c\/strong\u003e Yes. Gebel Kamil is classified in the Meteoritical Bulletin as Iron, ungrouped (Ni-rich ataxite). You can verify the classification here: \u003ca href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.cfm?code=52031\" rel=\"noopener\" target=\"_blank\"\u003eGebel Kamil\u003c\/a\u003e. This specimen ships with a certificate of authenticity from Treasure Coast Meteorite Co. (IMCA #3323).\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat does ungrouped ataxite mean?\u003c\/strong\u003e Ataxites are iron meteorites with sufficiently high nickel content that visible Widmanstätten patterns do not form under standard etching. Ungrouped means Gebel Kamil's chemistry does not match any established iron meteorite group, indicating a distinct parent body in the asteroid belt.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat is shrapnel, and how does it differ from a regmaglypted individual?\u003c\/strong\u003e Shrapnel refers to fragments produced when a meteorite disintegrates on impact rather than during atmospheric flight. Of the approximately 1.6 metric tons of Gebel Kamil recovered, almost all of it is shrapnel. Only a single 83 kg specimen was found as a complete regmaglypted individual. This piece is whole shrapnel: an intact, uncut fragment from the explosive impact, displaying the shear and rollover features that distinguish crater-recovered material.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat are shear lines and rollover lips?\u003c\/strong\u003e Shear lines are curvilinear bands of deformation that record the direction of shock propagation through the metal at the moment of impact, visible as the parallel ridges in the close-up images. Rollover lips are folds and curls along fragment edges where the ductile nickel-iron deformed plastically as fragments separated, seen along the torn edges in the macro shots. Both are hallmarks of hypervelocity impact disintegration and are found primarily in crater-recovered material.\u003c\/p\u003e\n\u003cp\u003e\u003cstrong\u003eWhat is included with this specimen?\u003c\/strong\u003e The 1414 gram Gebel Kamil whole shrapnel fragment pictured, a certificate of authenticity, and a specimen card with full classification details. The display stand and scale cube shown in the photos are for scale and are not included.\u003c\/p\u003e\n\u003ch3\u003eCollector significance\u003c\/h3\u003e\n\u003cp\u003eGebel Kamil occupies a position few \u003ca href=\"\/collections\/iron-meteorites\"\u003eiron meteorites\u003c\/a\u003e can match: a classified ungrouped specimen with confirmed crater association, recovered under controlled scientific survey, with visible structural evidence of the impact event itself. At 1414 grams it sits well above the more common hand-sample fragments, giving it real presence as a display piece. Intact shrapnel fragments breaking the 1400 gram mark, and showing this much character at once, clear lizard skin, well-defined shear lines, and folded-over rollover lips on a single uncut piece, are decidedly scarce. A large share of the surviving material in this size class has been sliced for the slab trade, so a complete fragment of this heft becomes harder to find as the original recovery stock is dispersed.\u003c\/p\u003e\n\u003cp\u003eThe combination of mass, surface preservation, and structural detail on this fragment makes it both a strong display piece and a meaningful portfolio addition for collectors focused on crater-recovered material. Specimens from Gebel Kamil connect the buyer to a specific, identifiable geological event, a category of meteorite that remains a small minority of what has ever been classified.\u003c\/p\u003e\n\u003cp\u003e \u003c\/p\u003e\n\u003cp\u003eMeteoritical Bulletin entry: \u003ca rel=\"noopener\" href=\"https:\/\/www.lpi.usra.edu\/meteor\/metbull.cfm?code=52031\" target=\"_blank\"\u003eGebel Kamil\u003c\/a\u003e | Classification: Iron (ungrouped, ataxite) | Find, Egypt, 2009\u003c\/p\u003e","brand":"Treasure Coast Meteorite Co.","offers":[{"title":"Default Title","offer_id":45408186564655,"sku":"GEBEL-KAMIL-1414.00G-INDIVIDUAL","price":2800.0,"currency_code":"USD","in_stock":true}],"thumbnail_url":"\/\/cdn.shopify.com\/s\/files\/1\/0726\/9724\/9839\/files\/gebel-kamil-iron-meteorite-1414g-front-face-shear-lines.jpg?v=1780381160"}],"url":"https:\/\/www.tcmeteorites.com\/collections\/featured-meteorites.oembed","provider":"Treasure Coast Meteorite Co.","version":"1.0","type":"link"}