View allAll Photos Tagged Solidus
Schweizweit ersten Auszeichnung «Minergie Qualitaetssicherung Bau» an ein Grossprojekt, Labeluebergabe MQS-Bau, Wohnueberbauung Solidus in Diessenhofen am Freitag 17. Mai 2019 (FOTO GACCIOLI KREUZLINGEN)
The tuatara is a reptile that is endemic to New Zealand and which, though it resembles most lizards, is part of a distinct lineage, order Rhynchocephalia.[1] The two species of tuatara are the only surviving members of its order, which flourished around 200 million years ago.[2] Their most recent common ancestor with any other extant group is with the squamates (lizards and snakes). For this reason, tuatara are of great interest in the study of the evolution of lizards and snakes, and for the reconstruction of the appearance and habits of the earliest diapsids (the group that also includes birds, dinosaurs, and crocodiles) (Souce: wikipedia).
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A suckling pig (or sucking pig[1]) is a piglet fed on its mother's milk (i.e., a piglet which is still a "suckling"). In culinary contexts, a suckling pig is slaughtered between the ages of two and six weeks. It is traditionally cooked whole, often roasted, in various cuisines. It is usually prepared for special occasions and gatherings.
The meat from suckling pig is pale and tender and the cooked skin is crisp and can be used for pork rinds. The texture of the meat can be somewhat gelatinous due to the amount of collagen in a young pig.
There are many ancient recipes for suckling pig from Roman and Chinese cuisine. Since the pig is one of the first animals domesticated by human beings for slaughter, many references to pigs are found in human culture. The suckling pig, specifically, appears in early texts such as the sixth-century Salic law. As an example of a law governing the punishment for theft, Title 2, article 1, is, in Latin, Si quis porcellum lactantem furaverit, et ei fuerit adprobatum (malb. chrane calcium hoc est) CXX dinarios qui faciunt solidos III culpabilis iudicetur. "If someone has stolen a suckling pig and this is proven against him, the guilty party will be sentenced to 120 denarii which adds up to three solidus (Latin coins)." The words "chrane calcium" are written in Frankish; "calcium" (or "galza" in other manuscripts) is the gloss for "suckling pig"; porcellum lactantem.[2] These glosses in Frankish, the so-called Malberg-Glossen, are considered the earliest attested words in Old Dutch.[3]
JOHANNES, 423-425
Solidus, Ravenna . DN IOHAN - NES PF AVG Drap., gep. Büste mit Rosettendiadem n.r. Rv. VICTORI - A AVCCC / R - V / COMOB Der Kaiser in militärischer Tracht n.r. stehend, in der Rechten Labarum haltend, auf der Linken Victoria mit Kranz auf einem Globus; der l. Fuss ist auf einen auf dem Boden sitzenden Gefangenen gesetzt. 4,39 g. C. 4 (150 frs.). Depeyrot II, 190, 12/1. DOC 819. Sehr selten . Sehr schön.
HESS-DIVO AG, Auction 328, lot 305.
Phylum： Mollusca 軟體動物門
Class： Gastropods 腹足綱
Family： Camaenidae 南亞蝸牛科
Scientific name： Amphidromus quadrasi solidus
Chinese name：
Author： Bartsch, 1917
Size： 39.03mm
Description： 39.03x18.73mm. Balabac Island. Palawan. Philippines. January, 2013.
An interesting selection of Roman Gold Coins from the B.d.B Collection
Constans augustus, 337 - 350
Solidus, Antiochia 337-347, 4.51 g. FL IVL CONS – TANS PERP AVG Pearl diademed, draped and cuirassed bust r. Rev. VICTORIA AVGVSTORVM Victory seated r. on cuirass holding shield, supported by winged genius, inscribed VOT / V / MVLT X. In exergue, SMANZ. C 140. RIC 29. Depeyrot 5/7. Biaggi 2115 (this coin).
Minor scratches on obverse, nick at seven o’clock on reverse and a few marks on edge, otherwise good very fine / about extremely fine.
NUMISMATICA ARS CLASSICA NAC AG, Auction 49, lot 490.
The obverse of a small gold tremissis (one third of a solidus and 1/18 of a Roman ounce), 15 mm, 1.46 grams (for the record, 1/18 of the Roman ounce should closer to 1.52 grams).
Struck at Constantinople (Istanbul, Turkey) in the name of and portraying the Eastern Roman emperor Zeno, 474- 491 AD.
Zeno is depicted wearing a pearl diadem on his head and a cloak over his cuirass (armor).
References include RIC x, 914.
CONSTANTINUS Ier Le Grand, vers 307-337 ap. J.-C.
Solidus, frappé à Siscia à l'occasion des tricennalia, vers 335 ap. J.-C. CONSTANTI-NVS MAX AVG Buste diadémé, drapé et cuirassé de 3/4 de face, la tête tournée à d. Rv. VICTORIA CONSTANTINI AVG / SIS Victoire, vêtue d'un chiton long et d'un manteau, assise à d. sur une cuirasse, tenant sur ses genoux un bouclier inscrit VOT / XXX; à ses côtés, bouclier rond. 4,32 g. RIC VII, 456, 242 (cet exemplaire mentionné). C. 611. Depeyrot I, 103, 23/1. Bastien, Donativa 81, g et note 3. Rare.
Provenance:
- Collection Dr. Eddé, Alexandria, 1900.
- H. C. Levis et Dresse de Lésbiolles, Naville & Cie, Genève - Ars Classica 11 (Lucerne 1925), 998.
- Naville & Cie, Genève - Ars Classica 17 (Lucerne 1934), 1905.
- Monnaies et Médailles SA, Bâle 73 (1988) 272.
HESS-DIVO AG, Auction 307, lot 1742.
Titulature avers : D N VALENTINI-ANVS P F AVG.
Description avers : Buste diadémé, drapé et cuirassé de Valentinien Ier à droite, vu de trois quarts en avant (A'c) ; diadème perlé et gemmé.
Traduction avers : “Dominus Noster Valentinianus Pius Felix Augustus”, (Notre seigneur Valentinien pieux heureux auguste). Titulature revers : RESTITVTOR - REIPVLICAE/ -|-// ANTI*.
Description revers : L'Empereur debout de face tourné à droite, vêtu militairement, tenant le labarum croiseté de la main droite et un globe nicéphore de la main gauche.
Traduction revers : “Restitutor Rei Publicæ”, (Le restaurateur du bien public (source texte CGB), Musée National, Beyrouth, Liban. Crédit Photo: François el Bacha. Tous droits réservés. Retrouvez mon blog sur larabio.com
Constantine III, 407 – 411
Solidus, Arles after 408, AV 4.48 g. D N CONSTAN – TINVS P F AVG Pearl-diademed, draped and cuirassed bust r. Rev. VICTORI – A AAVGGG Emperor standing r., holding standard and Victory on globe, spurning captive with his l. foot; in field, A – R. In exergue, CONOB. C 5. Depeyrot 22/1. LRC 804. RIC 1520 (this coin cited).
Very rare. An unusually attractive portrait, minor edge marks, otherwise good extremely fine.
Ex Archer M. Huntington collection (HSA 22127)
Constantine III, a general of obscure origins but considerable talent, was proclaimed emperor in Britain in 407 by his soldiers following the assassinations of the usurpers Marcus and Gratianus (neither of whom issued coins). He led his troops across the Channel into Gaul, where his authority was swiftly accepted locally, but was opposed by the reigning Western emperor Honorius, who sent his general Sarus from Italy to harass his defences. After initial setbacks, Constantine gained the upper hand and occupied all of Gaul up to the Alps, establishing his base at Arles. At its greatest extent, the territories controlled by Constantine included all of Western Europe, from Britain in the North and Spain in the South. Soon, however, his grip began to loosen. First Britain rose in revolt, and then Gerontius, Constantine’s own magister militum, whom he had sent to Spain to quell another revolt, ended up turning against him. His fate was sealed in 411 when Honorius sent a general by the name of Constantius (the future emperor Constantius III) to defeat him. Although he had taken refuge in a church and was ordained before surrendering, the former rebel was murdered in captivity and his head sent to Ravenna where it was exhibited for some time.
NUMISMATICA ARS CLASSICA NAC AG, Auction 67, lot 239.
Otras denominaciones:
Científicas: Boletus bulbosus, Tubiporus esculentus, Boletus solidus, Boletus citrinus,
Boletus clavipes.
Vulgares: Hongo blanco, calabaza, boleto comestible, Calabaza, viriato, aubarell, bolet de bou, cep, ciureny y sureny, cogordo, onddo zuri.
Sombrero pardo, color calabaza, regular, algo arrugado y con el borde más claro. De 6 a 20 cm. de diámetro.
El pie alcanza las mismas dimensiones que el sombrero, grueso en ejemplares jóvenes, blanco con retícula marrón. Se han encontrado ejemplares de hasta 3 kilos.
Himenio constituido por tubos blancos de joven que luego se vuelven amarillo oliva. No azulean al presionarlos. Largos y libres, fáciles de separar de la carne del sombrero.
Carne blanca, inmutable, si olor especial y sabor dulzón a avellana.
Crece en otoño en bosques de hayas, robles, castaños, abetos y pinos de montaña.
Comestible excelente.
Gold solidii of Emperor Hadrian (Publius Aelius Hadrianus Augustus, 76 AD – 138 AD, reigned 117 AD - 138 AD) and Vibia Sabina (83 AD – 137 AD). Roman Imperial, 2nd Century AD. Harvard Art Museum. Cambridge, Massachusetts, USA. Copyright 2018, James A. Glazier.
The reverse of a gold Solidus, struck in the name of the eastern Roman emperor Leo I, 457- 474 AD, at Thessalonica. ,
This image depicts the emperor in the role of Consul, enthroned facing, in full consular regalia.
Schweizweit ersten Auszeichnung «Minergie Qualitaetssicherung Bau» an ein Grossprojekt, Labeluebergabe MQS-Bau, Wohnueberbauung Solidus in Diessenhofen am Freitag 17. Mai 2019
vlnr.: Michael Wenger, Mitglied der Geschaeftsleitung Wenger AG, Bauherr, mit Walter Schoenholzer Regierungsrat, Energiedirektor Thurgau mit Andreas Meyer Primavesi, Geschaeftsleiter Minergie Schweiz. (FOTO GACCIOLI KREUZLINGEN)
Display of Roman coins
Roman Coins
Beginning with the first emperor, Augustus (ruled 27 BC-AD 14), the Romans regularly issued coins displaying a portrait of the ruler or one of his family members on the obverse (front). The reverse bore an image of a deity, mythological figure, building, or a historical event. The imperial portraits are finely modeled and often represent individuals not seen in surviving sculpture.
All the coins on view here are gold aurei, except no. 34, which is a gold solidus.
The obverse of a gold tremisses (one third of a solidus or 1/18 ounce) struck in the name of and portraying the eastern Roman emperor Anastasius, 491- 518 AD, attributed to the mint of Constantinople.
The obverse of a gold Solidus, 4.37 grams, struck in the name of and portraying the Eastern Roman emperor Leo I, 457-474 AD, at Thessalonica (now in northern Greece), in commemoration of one of his terms in the traditional Roman republican office of consul. His portrait displays a pearl diadem, Consular robes or an "imperial mantle", a mappa in his right hand and a cross-topped scepter over his left shoulder.
References include RIC X, 620.
Titulature avers : D N VALENTINI-ANVS P F AVG.
Description avers : Buste diadémé, drapé et cuirassé de Valentinien Ier à droite, vu de trois quarts en avant (A'c) ; diadème perlé et gemmé.
Traduction avers : “Dominus Noster Valentinianus Pius Felix Augustus”, (Notre seigneur Valentinien pieux heureux auguste). Titulature revers : RESTITVTOR - REIPVLICAE/ -|-// ANTI*.
Description revers : L'Empereur debout de face tourné à droite, vêtu militairement, tenant le labarum croiseté de la main droite et un globe nicéphore de la main gauche.
Traduction revers : “Restitutor Rei Publicæ”, (Le restaurateur du bien public (source texte CGB), Musée National, Beyrouth, Liban. Crédit Photo: François el Bacha. Tous droits réservés. Retrouvez mon blog sur larabio.com
Gold Solidus of Valentinian I (364–75)
Date:
364–375
Geography:
Made in Nicomedia (now Izmit, Turkey)
Valentinian restored Christian symbols, including the Chi-Rho emblem atop the emperor's standard.
Coins connected an emperor to his subjects. He paid the army in coins, received taxes in coins, and was responsible for maintaining their weight and purity. These coins of early Byzantine emperors conveyed imperial ideals through inscriptions and images.
An Important Collection of Roman Gold Coins Part II
Constantius II Caesar, 324 – 337
Solidus, Siscia 334, 4.30 g. FL IVL CONSTANTIVS NOB C Laureate and cuirassed bust r. Rev. PRINCIPI – IVVE – NTVTIS Prince, in military dress, standing l., holding vexillum in r. hand and sceptre in l.; in field r., two standards. In exergus, SIS. RIC 227 (this coin). C 165. Depeyrot 22/3. Biaggi 2161 (this coin). Traces of mounting, otherwise good very fine.
NUMISMATICA ARS CLASSICA NAC AG, Auction 34, lot 213.
The Postcard
A postally unused comic postcard published by D. E. & S. Ltd. The card was printed in England.
The pound note was withdrawn in 1988 in the UK in favour of the one pound coin.
Pre-Decimal Currency
The UK 'went decimal' on the 15th. February 1971. (1971 is often called the 'Year of the Con' because manufacturers and retailers used the changeover to increase their prices).
Pre-decimalisation money (L S D) was divided into pounds (£/L), shillings (s.) and pennies (d.).
'L S D' also stands for the hallucinogenic drug Lysergic Acid Diethylamide, but in this context it stands for the Latin words 'Libra', 'Solidus' and 'Denarius'. The coinage was as follows:
- 20 shillings (s.) in £1 (L)
- 12 pennies (d.) in 1 shilling (s.)
- 240 pennies in £1
- 480 halfpennies in £1
- 960 farthings in £1
The £ was represented by a printed note, and there was also a 10-shilling note.
A 'Guinea' (beloved of private medical consultants and solicitors) was 21 shillings - a way of extracting an additional 5% from the patient or client.
-- The British Pound and Inflation
The British pound has lost 94% its value since 1971, such that £100 in 1971 is equivalent in purchasing power to about £1,806 today. The pound has had an average inflation rate of 5.51% per year between 1971 and today.
This means that today's prices are 18 times as high as average prices since 1971, according to the Office for National Statistics. A pound today only buys 5.54% of what it could buy back then.
Landes
Iron, IAB-MG
United States
Find: 1930
TKW: 69,8 kg / OBJ: 2,15 g
LANDES
Found ~1930; Recognized 1968
38° 54' N., 79° 11' W.
A 69.8 kg mass was plowed up in a cornfield about a mile east of Landes Post Office, West Virginia; however, it was not recognized as meteoritic until 1968. Landes was previously classified as an anomalous IAB member due to its high Cu content. The IAB iron-meteorite complex, a systematic model recently proposed by Wasson and Kallemeyn (2002), comprises iron meteorites from the former IAB–IIICD group, as well as numerous related irons. The following compositional values were determined for inclusion into the IAB complex:
Au >1.3 ppm
As >10 ppm
Co >3,900 ppm
Sb >0.18 ppm
Ge/Ga ratio between 0.4 and 7
Many of the IAB complex members contain silicate inclusions, including types which are sulfide-rich, silicate-rich chondritic, silicate-rich non-chondritic, graphite-rich, and phosphate bearing. Based on bulk composition and REE abundance data for Landes, silicate inclusions are generally found to be chondritic, comprising nearly 40 vol% of the meteorite. The precursor of the IAB complex irons is considered to have been a volatile-rich planetesimal related to carbonaceous chondrites (Ruzicka, 2014).
On a Ni–Au diagram, Landes plots within the IAB main group and shares an Ar–Ar retention age of ~4.43 b.y. with Copiapo and certain other members, somewhat younger than that of typical IAB meteorites.
This younger age could be due to later impact-heating events, or to terrestrial weathering processes (Bogard et al., 2005). The different trends found among IAB complex irons are most consistent with separate impact melt pools within the regolith of a carbonaceous chondrite parent body, which then experienced variable degrees of impact mixing and crystal segregation/fractional crystallization as well as different cooling rates and equilibration conditions. It remains unresolved whether or not some IAB subgroups (e.g., sLM, sLH) share a genetic relationship with the IAB main group, while another subgroup (sHL) has been shown to be most consistent with formation on a separate parent body (Worsham et al., 2016, 2017).
Based on similar silicate textures, reduced mineral chemistry, and O-isotopes, it is presumed that the winonaites and the IAB complex irons originated on a common parent body. Utilizing a Ge/Ni vs. Au/Ni coupled diagram, Hidaka et al. (2015) determined that FeNi-metal in the winonaite Y-8005 plots in the field of the sLL subgroup of the IAB complex irons. In addition, the metal in this winonaite retains a near chondritic composition likely representative of the precursor material of the parent body. In view of these findings, they suggest that the sLL subgroup rather than the main group of the IAB complex represents the primitive metal of the IAB–winonaite parent body, with the main group possibly representing a partial melt of the sLL subgroup.
In their study of plagioclase separates derived from individual silicate grains composing different inclusions within Landes, Caddo County, Campo del Cielo, and Ocotillo, Vogel and Renne (2008) found that corrected Ar–Ar ages have a significant range—from as old as ~4.55 b.y., near the probable onset of differentiation from radiogenic heating (26Ar), to as young as ~4.43 b.y., presumably reflecting grains that experienced the latest closure of the K–Ar system following reassembly and/or late impact events. The slope of a Pd–Ag isochron corresponds to an age of ~14.6 (+6.7/–7) m.y. after CAI formation (4.559–4.545 b.y. ago), reflecting closure of the Pd–Ag system and the mixing of metal and silicates (Theis et al., 2010). Schulz et al. (2012) identified some silicates in IAB Caddo County indicating that metal–silicate segregation occurred as early as 0.86 (+0.93/–0.86) m.y. after CAIs. Other age measurements based on the I–Xe system for IAB iron silicates give a range of 4.564–4.558 b.y. (Pravdivtseva et al., 2013). Schulz et al. (2012) established the period for metal–silicate segregation in IAB irons at 5.06 (+0.42/–0.41) m.y. after CAIs, while modeling by Ruzicka (2014) based on the Hf–W chronometer for metal and silicate led to the determination of 3.6 (±3.1) m.y. after CAIs. Taken together, the Hf–W and I–Xe chronometer ages provided an average closure age of 4.5622 (±0.004) b.y. It was suggested that this wide range of ages represents silicate grains that were cooled at different rates and different depths within the IAB parent body, consistent with an origin from multiple impact melt accumulation pools that were buried deeply in a regolith (Ruzicka, 2014).
Only after collisional disruption leading to the mixing of solid-to-partially melted silicates with molten metal from diverse accumulation pools, and the subsequent gravitational reassembly of this planetesimal, were the individual silicate grains from different source regions intermixed to form the composite IAB inclusions we observe today (Benedix et al., 2000). Following this catastrophic disruption, which is calculated to have likely occurred ~4.47–4.54 b.y. ago, reassembly and initial cooling proceeded rapidly to preserve the pre-established Ar–Ar ages of individual grains. Reburial of this silicated iron material allowed for sub-solidus cooling at a slow rate over an extended period (Worsham et al., 2016).
Utilizing the short-lived 182Hf–182W chronometer, corrected for neutron capture by 182W due to galactic cosmic rays, Hunt et al. (2018) derived the timing of metal–silicate separation of all genetically-related IAB irons (at least the MG and sLL subgroup [possibly also the sLM subgroup] and the ungrouped Caddo County [Udei Station grouplet] and Livingstone [Algarrabo duo]) to 6.0 (±0.8) m.y. after CAIs. Based on the constraints provided by the timing of metal segregation, they modeled the early history of the 120(+)-km-diameter IAB parent body as outlined in the following diagram:
Since the highest Ar–Ar-based age estimate for Landes is younger than the highest measured for Caddo County, and since the cooling rate of metal was determined to be lower for Landes than that for Caddo County, it was inferred that Landes was the more deeply buried of the two, both pre-disruption and post-reassembly of the IAB planetesimal (Vogel and Renne, 2008). In contrast to these meteorites, they demonstrated that the Ar–Ar-based age of Campo del Cielo reflects resetting in a more high-temperature thermal environment, probably at a deeper burial location pre- and/or post-reassembly.
A refinement of IAB iron CRE ages is under development through a broad cosmogenic noble gas study of silicates and metal in IAB silicated irons (Vogel and Leya, 2007). Data indicate a CRE age of ~200 m.y. for Landes, which was calculated based on metal 38Ar, 21Ne, and 3He, and on silicate 38Ar; the lower CRE age obtained for Landes based on silicate 3He and 21Ne might indicate loss of cosmogenic He and Ne (Vogel and Leya, 2008). Their studies revealed a pre-atmospheric diameter for Landes of ~40 cm. The Landes specimen shown above is a 27.1 g etched partial slice.
Otras denominaciones:
Científicas: Boletus bulbosus, Tubiporus esculentus, Boletus solidus, Boletus citrinus,
Boletus clavipes.
Vulgares: Hongo blanco, calabaza, boleto comestible, Calabaza, viriato, aubarell, bolet de bou, cep, ciureny y sureny, cogordo, onddo zuri.
Sombrero pardo, color calabaza, regular, algo arrugado y con el borde más claro. De 6 a 20 cm. de diámetro.
El pie alcanza las mismas dimensiones que el sombrero, grueso en ejemplares jóvenes, blanco con retícula marrón. Se han encontrado ejemplares de hasta 3 kilos.
Himenio constituido por tubos blancos de joven que luego se vuelven amarillo oliva. No azulean al presionarlos. Largos y libres, fáciles de separar de la carne del sombrero.
Carne blanca, inmutable, si olor especial y sabor dulzón a avellana.
Crece en otoño en bosques de hayas, robles, castaños, abetos y pinos de montaña.
Comestible excelente.
Landes
Iron, IAB-MG
United States
Find: 1930
TKW: 69,8 kg / OBJ: 2,15 g
LANDES
Found ~1930; Recognized 1968
38° 54' N., 79° 11' W.
A 69.8 kg mass was plowed up in a cornfield about a mile east of Landes Post Office, West Virginia; however, it was not recognized as meteoritic until 1968. Landes was previously classified as an anomalous IAB member due to its high Cu content. The IAB iron-meteorite complex, a systematic model recently proposed by Wasson and Kallemeyn (2002), comprises iron meteorites from the former IAB–IIICD group, as well as numerous related irons. The following compositional values were determined for inclusion into the IAB complex:
Au >1.3 ppm
As >10 ppm
Co >3,900 ppm
Sb >0.18 ppm
Ge/Ga ratio between 0.4 and 7
Many of the IAB complex members contain silicate inclusions, including types which are sulfide-rich, silicate-rich chondritic, silicate-rich non-chondritic, graphite-rich, and phosphate bearing. Based on bulk composition and REE abundance data for Landes, silicate inclusions are generally found to be chondritic, comprising nearly 40 vol% of the meteorite. The precursor of the IAB complex irons is considered to have been a volatile-rich planetesimal related to carbonaceous chondrites (Ruzicka, 2014).
On a Ni–Au diagram, Landes plots within the IAB main group and shares an Ar–Ar retention age of ~4.43 b.y. with Copiapo and certain other members, somewhat younger than that of typical IAB meteorites.
This younger age could be due to later impact-heating events, or to terrestrial weathering processes (Bogard et al., 2005). The different trends found among IAB complex irons are most consistent with separate impact melt pools within the regolith of a carbonaceous chondrite parent body, which then experienced variable degrees of impact mixing and crystal segregation/fractional crystallization as well as different cooling rates and equilibration conditions. It remains unresolved whether or not some IAB subgroups (e.g., sLM, sLH) share a genetic relationship with the IAB main group, while another subgroup (sHL) has been shown to be most consistent with formation on a separate parent body (Worsham et al., 2016, 2017).
Based on similar silicate textures, reduced mineral chemistry, and O-isotopes, it is presumed that the winonaites and the IAB complex irons originated on a common parent body. Utilizing a Ge/Ni vs. Au/Ni coupled diagram, Hidaka et al. (2015) determined that FeNi-metal in the winonaite Y-8005 plots in the field of the sLL subgroup of the IAB complex irons. In addition, the metal in this winonaite retains a near chondritic composition likely representative of the precursor material of the parent body. In view of these findings, they suggest that the sLL subgroup rather than the main group of the IAB complex represents the primitive metal of the IAB–winonaite parent body, with the main group possibly representing a partial melt of the sLL subgroup.
In their study of plagioclase separates derived from individual silicate grains composing different inclusions within Landes, Caddo County, Campo del Cielo, and Ocotillo, Vogel and Renne (2008) found that corrected Ar–Ar ages have a significant range—from as old as ~4.55 b.y., near the probable onset of differentiation from radiogenic heating (26Ar), to as young as ~4.43 b.y., presumably reflecting grains that experienced the latest closure of the K–Ar system following reassembly and/or late impact events. The slope of a Pd–Ag isochron corresponds to an age of ~14.6 (+6.7/–7) m.y. after CAI formation (4.559–4.545 b.y. ago), reflecting closure of the Pd–Ag system and the mixing of metal and silicates (Theis et al., 2010). Schulz et al. (2012) identified some silicates in IAB Caddo County indicating that metal–silicate segregation occurred as early as 0.86 (+0.93/–0.86) m.y. after CAIs. Other age measurements based on the I–Xe system for IAB iron silicates give a range of 4.564–4.558 b.y. (Pravdivtseva et al., 2013). Schulz et al. (2012) established the period for metal–silicate segregation in IAB irons at 5.06 (+0.42/–0.41) m.y. after CAIs, while modeling by Ruzicka (2014) based on the Hf–W chronometer for metal and silicate led to the determination of 3.6 (±3.1) m.y. after CAIs. Taken together, the Hf–W and I–Xe chronometer ages provided an average closure age of 4.5622 (±0.004) b.y. It was suggested that this wide range of ages represents silicate grains that were cooled at different rates and different depths within the IAB parent body, consistent with an origin from multiple impact melt accumulation pools that were buried deeply in a regolith (Ruzicka, 2014).
Only after collisional disruption leading to the mixing of solid-to-partially melted silicates with molten metal from diverse accumulation pools, and the subsequent gravitational reassembly of this planetesimal, were the individual silicate grains from different source regions intermixed to form the composite IAB inclusions we observe today (Benedix et al., 2000). Following this catastrophic disruption, which is calculated to have likely occurred ~4.47–4.54 b.y. ago, reassembly and initial cooling proceeded rapidly to preserve the pre-established Ar–Ar ages of individual grains. Reburial of this silicated iron material allowed for sub-solidus cooling at a slow rate over an extended period (Worsham et al., 2016).
Utilizing the short-lived 182Hf–182W chronometer, corrected for neutron capture by 182W due to galactic cosmic rays, Hunt et al. (2018) derived the timing of metal–silicate separation of all genetically-related IAB irons (at least the MG and sLL subgroup [possibly also the sLM subgroup] and the ungrouped Caddo County [Udei Station grouplet] and Livingstone [Algarrabo duo]) to 6.0 (±0.8) m.y. after CAIs. Based on the constraints provided by the timing of metal segregation, they modeled the early history of the 120(+)-km-diameter IAB parent body as outlined in the following diagram:
Since the highest Ar–Ar-based age estimate for Landes is younger than the highest measured for Caddo County, and since the cooling rate of metal was determined to be lower for Landes than that for Caddo County, it was inferred that Landes was the more deeply buried of the two, both pre-disruption and post-reassembly of the IAB planetesimal (Vogel and Renne, 2008). In contrast to these meteorites, they demonstrated that the Ar–Ar-based age of Campo del Cielo reflects resetting in a more high-temperature thermal environment, probably at a deeper burial location pre- and/or post-reassembly.
A refinement of IAB iron CRE ages is under development through a broad cosmogenic noble gas study of silicates and metal in IAB silicated irons (Vogel and Leya, 2007). Data indicate a CRE age of ~200 m.y. for Landes, which was calculated based on metal 38Ar, 21Ne, and 3He, and on silicate 38Ar; the lower CRE age obtained for Landes based on silicate 3He and 21Ne might indicate loss of cosmogenic He and Ne (Vogel and Leya, 2008). Their studies revealed a pre-atmospheric diameter for Landes of ~40 cm. The Landes specimen shown above is a 27.1 g etched partial slice.
Landes
Iron, IAB-MG
United States
Find: 1930
TKW: 69,8 kg / OBJ: 2,15 g
LANDES
Found ~1930; Recognized 1968
38° 54' N., 79° 11' W.
A 69.8 kg mass was plowed up in a cornfield about a mile east of Landes Post Office, West Virginia; however, it was not recognized as meteoritic until 1968. Landes was previously classified as an anomalous IAB member due to its high Cu content. The IAB iron-meteorite complex, a systematic model recently proposed by Wasson and Kallemeyn (2002), comprises iron meteorites from the former IAB–IIICD group, as well as numerous related irons. The following compositional values were determined for inclusion into the IAB complex:
Au >1.3 ppm
As >10 ppm
Co >3,900 ppm
Sb >0.18 ppm
Ge/Ga ratio between 0.4 and 7
Many of the IAB complex members contain silicate inclusions, including types which are sulfide-rich, silicate-rich chondritic, silicate-rich non-chondritic, graphite-rich, and phosphate bearing. Based on bulk composition and REE abundance data for Landes, silicate inclusions are generally found to be chondritic, comprising nearly 40 vol% of the meteorite. The precursor of the IAB complex irons is considered to have been a volatile-rich planetesimal related to carbonaceous chondrites (Ruzicka, 2014).
On a Ni–Au diagram, Landes plots within the IAB main group and shares an Ar–Ar retention age of ~4.43 b.y. with Copiapo and certain other members, somewhat younger than that of typical IAB meteorites.
This younger age could be due to later impact-heating events, or to terrestrial weathering processes (Bogard et al., 2005). The different trends found among IAB complex irons are most consistent with separate impact melt pools within the regolith of a carbonaceous chondrite parent body, which then experienced variable degrees of impact mixing and crystal segregation/fractional crystallization as well as different cooling rates and equilibration conditions. It remains unresolved whether or not some IAB subgroups (e.g., sLM, sLH) share a genetic relationship with the IAB main group, while another subgroup (sHL) has been shown to be most consistent with formation on a separate parent body (Worsham et al., 2016, 2017).
Based on similar silicate textures, reduced mineral chemistry, and O-isotopes, it is presumed that the winonaites and the IAB complex irons originated on a common parent body. Utilizing a Ge/Ni vs. Au/Ni coupled diagram, Hidaka et al. (2015) determined that FeNi-metal in the winonaite Y-8005 plots in the field of the sLL subgroup of the IAB complex irons. In addition, the metal in this winonaite retains a near chondritic composition likely representative of the precursor material of the parent body. In view of these findings, they suggest that the sLL subgroup rather than the main group of the IAB complex represents the primitive metal of the IAB–winonaite parent body, with the main group possibly representing a partial melt of the sLL subgroup.
In their study of plagioclase separates derived from individual silicate grains composing different inclusions within Landes, Caddo County, Campo del Cielo, and Ocotillo, Vogel and Renne (2008) found that corrected Ar–Ar ages have a significant range—from as old as ~4.55 b.y., near the probable onset of differentiation from radiogenic heating (26Ar), to as young as ~4.43 b.y., presumably reflecting grains that experienced the latest closure of the K–Ar system following reassembly and/or late impact events. The slope of a Pd–Ag isochron corresponds to an age of ~14.6 (+6.7/–7) m.y. after CAI formation (4.559–4.545 b.y. ago), reflecting closure of the Pd–Ag system and the mixing of metal and silicates (Theis et al., 2010). Schulz et al. (2012) identified some silicates in IAB Caddo County indicating that metal–silicate segregation occurred as early as 0.86 (+0.93/–0.86) m.y. after CAIs. Other age measurements based on the I–Xe system for IAB iron silicates give a range of 4.564–4.558 b.y. (Pravdivtseva et al., 2013). Schulz et al. (2012) established the period for metal–silicate segregation in IAB irons at 5.06 (+0.42/–0.41) m.y. after CAIs, while modeling by Ruzicka (2014) based on the Hf–W chronometer for metal and silicate led to the determination of 3.6 (±3.1) m.y. after CAIs. Taken together, the Hf–W and I–Xe chronometer ages provided an average closure age of 4.5622 (±0.004) b.y. It was suggested that this wide range of ages represents silicate grains that were cooled at different rates and different depths within the IAB parent body, consistent with an origin from multiple impact melt accumulation pools that were buried deeply in a regolith (Ruzicka, 2014).
Only after collisional disruption leading to the mixing of solid-to-partially melted silicates with molten metal from diverse accumulation pools, and the subsequent gravitational reassembly of this planetesimal, were the individual silicate grains from different source regions intermixed to form the composite IAB inclusions we observe today (Benedix et al., 2000). Following this catastrophic disruption, which is calculated to have likely occurred ~4.47–4.54 b.y. ago, reassembly and initial cooling proceeded rapidly to preserve the pre-established Ar–Ar ages of individual grains. Reburial of this silicated iron material allowed for sub-solidus cooling at a slow rate over an extended period (Worsham et al., 2016).
Utilizing the short-lived 182Hf–182W chronometer, corrected for neutron capture by 182W due to galactic cosmic rays, Hunt et al. (2018) derived the timing of metal–silicate separation of all genetically-related IAB irons (at least the MG and sLL subgroup [possibly also the sLM subgroup] and the ungrouped Caddo County [Udei Station grouplet] and Livingstone [Algarrabo duo]) to 6.0 (±0.8) m.y. after CAIs. Based on the constraints provided by the timing of metal segregation, they modeled the early history of the 120(+)-km-diameter IAB parent body as outlined in the following diagram:
Since the highest Ar–Ar-based age estimate for Landes is younger than the highest measured for Caddo County, and since the cooling rate of metal was determined to be lower for Landes than that for Caddo County, it was inferred that Landes was the more deeply buried of the two, both pre-disruption and post-reassembly of the IAB planetesimal (Vogel and Renne, 2008). In contrast to these meteorites, they demonstrated that the Ar–Ar-based age of Campo del Cielo reflects resetting in a more high-temperature thermal environment, probably at a deeper burial location pre- and/or post-reassembly.
A refinement of IAB iron CRE ages is under development through a broad cosmogenic noble gas study of silicates and metal in IAB silicated irons (Vogel and Leya, 2007). Data indicate a CRE age of ~200 m.y. for Landes, which was calculated based on metal 38Ar, 21Ne, and 3He, and on silicate 38Ar; the lower CRE age obtained for Landes based on silicate 3He and 21Ne might indicate loss of cosmogenic He and Ne (Vogel and Leya, 2008). Their studies revealed a pre-atmospheric diameter for Landes of ~40 cm. The Landes specimen shown above is a 27.1 g etched partial slice.
Schweizweit ersten Auszeichnung «Minergie Qualitaetssicherung Bau» an ein Grossprojekt, Labeluebergabe MQS-Bau, Wohnueberbauung Solidus in Diessenhofen am Freitag 17. Mai 2019
vlnr.: Michael Wenger, Mitglied der Geschaeftsleitung Wenger AG, Bauherr, mit Walter Schoenholzer Regierungsrat, Energiedirektor Thurgau mit Andreas Meyer Primavesi, Geschaeftsleiter Minergie Schweiz. (FOTO GACCIOLI KREUZLINGEN)