Small hypervelocity particles captured in aerogel collectors: Location,extraction, handling and storage

Abstract— It has now been about a decade since the first demonstrations that hypervelocity particles could be captured, partially intact, in aerogel collectors. But the initial promise of a bonanza of partially‐intact extraterrestrial particles, collected in space, has yet to materialize. One of the difficulties that investigators have encountered is that the location, extraction, handling and analysis of very small (10 μm and less) grains, which constitute the vast majority of the captured particles, is challenging and burdensome. Furthermore, current extraction techniques tend to be destructive over large areas of the collectors. Here we describe our efforts to alleviate some of these difficulties. We have learned how to rapidly and efficiently locate captured particles in aerogel collectors, using an automated microscopic scanning system originally developed for experimental nuclear astrophysics. We have learned how to precisely excavate small access tunnels and trenches using an automated micromanipulator and glass microneedles as tools. These excavations are only destructive to the collector in a very small area—this feature may be particularly important for excavations in the precious Stardust collectors. Using actuatable silicon microtweezers, we have learned how to extract and store “naked” particles—essentially free of aerogel—as small as 3 μm in size. We have also developed a technique for extracting particles, along with their terminal tracks, still embedded in small cubical aerogel blocks. We have developed a novel method for storing very small particles in etched nuclear tracks. We have applied these techniques to the extraction and storage of grains captured in aerogel collectors (Particle Impact Experiment, Orbital Debris Collector Experiment, Comet‐99) in low Earth orbit.     

The age of the martian meteorite Northwest Africa 1195 and the differentiation history of the shergottites

Samarium-neodymium isotopic analyses of unleached and acid-leached mineral fractions from the recently identified olivine-bearing shergottite Northwest Africa 1195 yield a crystallization age of 347 ± 13 Ma and an value of +40.1 ± 0.9. Maskelynite fractions do not lie on the Sm-Nd isochron and appear to contain a martian surface component with low ¹⁴⁷Sm/¹⁴⁴Nd and ¹⁴³Nd/¹⁴⁴Nd ratios that was added during shock. The Rb-Sr system is disturbed and does not yield an isochron. Terrestrial Sr appears to have affected all of the mineral fractions, although a maximum initial ⁸⁷Sr/⁸⁶Sr ratio of 0.7016 is estimated by passing a 347 Ma reference line through the maskelynite fraction that is least affected by contamination. The high initial value and the low initial ⁸⁷Sr/⁸⁶Sr ratio, combined with the geologically young crystallization age, indicate that Northwest Africa 1195 is derived from a source region characterized by a long-term incompatible-element depletion.The age and initial Sr and Nd isotopic compositions of Northwest Africa 1195 are very similar to those of Queen Alexandra Range 94201, indicating these samples were derived from source regions with similar Sr-Nd isotopic systematics. These similarities suggest that these two meteorites share a close petrogenetic relationship and might have been erupted from a common volcano. The meteorites Yamato 980459, Dar al Gani 476, Sayh al Uhaymir 005/008, and Dhofar 019 also have relatively old ages between 474 and 575 Ma and trace element and/or isotopic systematics that are indicative of derivation from incompatible-element-depleted sources. This suggests that the oldest group of meteorites is more closely related to one another than they are to the younger meteorites that are derived from less incompatible-element-depleted sources. Closed-system fractional crystallization of this suite of meteorites is modeled with the MELTS algorithm using the bulk composition of Yamato 980459 as a parent. These models reproduce many of the major element and mineralogical variations observed in the suite. In addition, the rare earth element systematics of these meteorites are reproduced by fractional crystallization using the proportions of phases and extents of crystallization that are calculated by MELTS. Other shergottites that demonstrate enrichments in incompatible-elements and have evolved Sr and Nd isotopic systematics have some geochemical systematics that are similar to those observed in the depleted group. Most notably, although they exhibit a very limited range of incompatible trace element and isotopic compositions, they have highly variable major element compositions. This is also consistent with evolution from a common mantle source region by variable amounts of fractional crystallization. If this scenario is correct, it suggests that the combined effects of source composition and fractional crystallization are likely to account for the major element, trace element, and isotopic diversity of all shergottites.     

Strike and dip of crustal boundaries — A method and its application

Summary If for a point on the earth's surface, the apparent (moveout) seismic velocities have been determined for a number of profiles in different directions, a possibility is offered to calculate true strike and dip of crustal boundaries. In the present paper the theory is developed, partly for a sloping Mohorovii discontinuity only, partly for sloping Conrad and Mohorovii discontinuities with parallel strikes. The theory for the sloping Mohorovii discontinuity is applied to field measurements at a place about 30 km west of Uppsala performed in June 1969. With a crustalP-wave velocity of 6.3 km/sec, a good fit to the observations is obtained for aPn-velocity of 8.55 km/sec and a downdip of Moho of 7.2° in the direction S 3.8° E. These numerical values are not the most important output of this paper. On the other hand, the testing of the method appears far more important, and also that improvements can be suggested in the experimental procedure in future applications of this method.     

Uranium-lead isotope systematics of Mars inferred from the basaltic shergottite QUE 94201

Uranium-lead ratios (commonly represented as ²³⁸U/²⁰⁴Pb = μ) calculated for the sources of martian basalts preserve a record of petrogenetic processes that were active during early planetary differentiation and formation of martian geochemical reservoirs. To better define the range of μ values represented by the source regions of martian basalts, we completed U-Pb elemental and isotopic analyses on whole rock, mineral and leachate fractions from the martian meteorite Queen Alexandra Range 94201 (QUE 94201). The whole rock and silicate mineral fractions have unradiogenic Pb isotopic compositions that define a narrow range (²⁰⁶Pb/²⁰⁴Pb = 11.16-11.61). In contrast, the Pb isotopic compositions of weak HCl leachates are more variable and radiogenic. The intersection of the QUE 94201 data array with terrestrial Pb in ²⁰⁶Pb/²⁰⁴Pb-²⁰⁷Pb/²⁰⁴Pb-²⁰⁸Pb/²⁰⁴Pb compositional space is consistent with varying amounts of terrestrial contamination in these fractions. We calculate that only 1-7% contamination is present in the purified silicate mineral and whole rock fractions, whereas the HCl leachates contain up to 86% terrestrial Pb. This terrestrial Pb contamination generated a ²⁰⁶Pb-²⁰⁷Pb array in the QUE fractions that appears to represent an ancient age, which contrasts with a much younger crystallization age of 327 ± 10 Ma derived from Rb-Sr and Sm-Nd isochrons (Borg L. E., Nyquist L. E., Taylor L. A., Wiesmann H. and Shih C. -Y. (1997) Constraints on Martian differentiation processes from Rb-Sr and Sm-Nd isotopic analyses of the basaltic shergottite QUE 94201. Geochim. Cosmochim. Acta61, 4915-4931). Despite the contamination, and accepting 327 ± 10 Ma as the crystallization age, we use the U-Pb data to determine the initial ²⁰⁶Pb/²⁰⁴Pb of QUE 94201 to be 11.086 ± 0.008 and to calculate the μ value of its mantle source to be 1.82 ± 0.01. The μ value calculated for the QUE 94201 source is the lowest determined for any martian basalt source, and, when compared to the highest values determined for martian basalt sources, indicates that μ values in martian source reservoirs vary by at least a factor of two. Additionally, the range of source μ values indicates that the μ value of bulk silicate Mars is approximately three. The amount of variation in the μ values of the mantle sources (μ ∼ 2-4) is greater than can be explained by igneous processes involving silicate phases alone. We suggest the possibility that a small amount of sulfide crystallization may generate greater extents of U-Pb fractionation during formation of the mantle sources of martian basalts.     

Some implications of low altitude observations of isotropic precipitation of ring current protons beyond the plasmapause

The precipitation patterns of 6 keV protons at 10° and 80° pitch angles have been mapped at altitudes <1500 km from the ESRO 1A and 1B spacecraft. Equatorward of the trapping boundary, a region of isotropic precipitation, bounded on its equatorward border by a region of anisotropic (depleted loss cone) precipitation, is always observed. The latitudinal location of this transition appears to be nearly spatially coincident with the plasmapause. Similar precipitation patterns are shown to exist for higher energy protons. The general absence of enhanced precipitation at the plasmapause suggests that the inner boundary of the ring current is not usually produced by an enhanced proton pitch angle diffusion process. The isotropic precipitation observed beyond the plasmapause is most consistent with the occurence of an electrostatic instability throughout the ring current zone. It is doubtful whether the proposed cold Li plasma seeding experiments beyond the plasmapause could significantly increase the observed natural proton precipitation rates.     

The COMET experiment

Abstract— The COMET program is a program for the collection of micron to submicron interplanetary dust particles in low Earth orbits. Since collection takes place as the Earth crosses a given meteor stream, the particles are mainly of cometary origin. The grain remnants, located at their impact positions on high purity metallic collectors, are analysed in the laboratory for chemical and isotopical identification. The COMET-1 experiment took place in 1985 October, during encounter with the Draconid meteor stream, related to the Giacobini-Zinner comet. The fluence of extraterrestrial grains that had impacted our detectors was ～10x higher than the value of the mean meteroid fluence at ～1AU, which suggests that most of the grains originated from the Giacobini-Zinner comet. One of the most important results of their chemical analysis was that ～90% of them are enriched in low Z elements (C and O have undoubedly been identified). They could contain a CHON phase similar to that observed in the close environment of Halley's nucleus. The first imagery of the grain remnants by field emission scanning electron microscopy suggests that they are very low density aggregates still present at the impacting positions which, in most cases, are very different from the impact craters observed for the same mean relative velocity for full grains of the same size. These results show that the COMET program has constituted an important step towards the analysis of cometary material and the understanding of the evolution of the early Solar System.     

Genetic aspects of the Geita and Jubilee Reef Archean BIF-hosted gold deposits,Tanzania

The Sukumaland Greenstone Belt (new name), which is located in north-western Tanzania hosts a large number of gold deposits, prospects and occurrences. The Archean stratigraphy comprises an older basement of granitic gneisses (Dodoman System) overlain by mafic and ultramafic volcanics which are succeeded by felsic volcanic rocks and a banded iron formation (BIF), predominantly as oxide facies. The volcanics and BIF together make up the Nyanzian System. The uppermost part of the Archean stratigraphy (Kavirondian System) consists of conglomerates and quartzites which rest unconformably on the older units. The sequence has been intruded by both syn- and post-orogenic granitoids and by several generations of felsic and intermediate dykes and sills. Gold mineralisation is abundant in all stratigraphic units except for the granitic rocks. Six types of mineralisation can be distinguished. These are BIF-hosted, hear zone type, (quartz-) vein type, clastic sedimenthosted alluvial/eluvial, and massive sulphide type deposits. The last is represented by only one deposit in this area.The location of the BIF-hosted gold mineralisation is controlled by trachytic rocks of both dyke- and sill-like appearance and brecciated shear zones which follow the contacts between BIF and intercalations of tuff. The host rocks around these trachytes and shear zones have been pervasively mineralised with pyrite, auriferous pyrite and native gold, selectively replacing magnetite layers.The mineralisation grades from massively replaced layers at the trachyte/BIF- or tuff/BIF-contact into disseminated layers, rare specks of pyrite and eventually into barren BIF. Permeable features such as veins, fractures, breccia zones and shear zones may contain mineralisation even away from the main ore zones.Ore textures and fire assay results from Geita and Jubilee Reef indicate the introduction of ore fluids via epigenetic conduits into the adjacent wall rocks. Neither a depletion halo in the adjacent BIF (lateral secretion) nor a zone of footwall alteration or stringer ore, which might support a syngenetic/replacement concept for the mineralisation have been found.The main precipitating mechanism was probably a redox reaction of the ascending, reducing ore fluids with the magnetite of the BIF. This reaction resulted in the replacement of magnetite by pyrite, a rise in Eh, and the precipitation of gold together with the pyrite. The authors propose an epigenetic mineralisation process which produced ore-grade mineralisation of different styles in all stratigraphic units. The special physico-chemical trap of the magnetite layers led to the development of pyrite/gold mineralisation of generally stratabound appearance. The ore fluids originated probably from granitic intrusions and the underlying mafic volcanics are a possible gold source. For textural reasons the surrounding BIF is unlikely to have supplied a major portion of the gold.

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Zusammenfassung Der Sukumaland Greenstone Belt (neuer Name) im Nordwesten Tanzanias beherbergt eine große Zahl von Goldvorkommen unterschiedlicher wirtschaftlicher Bedeutung. Die Archaische Stratigraphie umfaßt ein aus granitischem Gneiss bestehendes Grundgebirge (Dodoman-System), auf dem mafische und ultramafische Vulkanite ruhen, die wiederum von felsischen Vulkaniten und hauptsächlich oxydischer banded iron formation (BIF) überlagert werden. Diese Vulkanit- und BIF-Serien stellen die stratigraphische Einheit des Nyanzian-Systems dar. Der Top der Archaischen Stratigraphie wird von Konglomeraten und Quarziten des Kavirondian gebildet, welches diskordant auf den älteren Einheiten liegen. Synund postorogene Granitoide sowie mehrere Generationen von felsischen und intermediären Gängen sind in die Archaische Abfolge intrudiert.Goldindikationen und -vorkommen sind relativ häufig und treten in allen stratigraphischen Einheiten mit Ausnahme der Granitoide auf. Dabei lassen sich sechs Typen von Goldmineralisationen unterscheiden; diese sind: Gold in BIF, in Scherzonen, in Goldquarzgängen, in klastischen Archaischen Sedimenten, in Alluvionen und in massiven Sulfiden. Vom letztgenannten Typ ist bisher lediglich ein Vorkommen im Untersuchungsgebiet bekannt. Die Position der Goldmineralisation in den BIFs wird von trachitischen Dykes und Sills sowie von Scherzonen im Kontaktbereich zwischen BIF und Tuffeinschaltungen kontrolliert. Die Kontaktbereiche zu den brekziierten Scherzonen und trachytischen Gesteinen sind stark mineralisiert, wobei Pyrit, goldhaltiger Pyrit und Freigold selektiv Magnetitlagen verdrängt und sulfidisiert haben.Der Verdrängungsprozeß Magnetit/Pyrit hat im direkten Kontaktbereich zwischen Trachit bzw. Tuffzwischenlagen und BIF zur Bildung von massiven Pyrit-Lagen geführt. Lateral gehen diese massiv sulfidisierten Bereiche in Lagen von Magnetit mit disseminierter Pyritmineralisation über, weiter distal in vereinzelte Pyritkörner und schließlich in sulphidfreie Oxydfazies-BIF. Außerhalb dieser mineralisierten Kon taktzonen, teilweise in erheblichem Abstand zur Hauptmineralisation, enthalten auch Bereiche erhöhter (tektonischer) Permeabilität, wie z. B. kleine Trümer, Klüfte, Brekzien- und Scherzonen, stellenweise reiche Pyrit/Gold-Mineralisationen.Untersuchungen von Erzverteilung und -texturen sowie Goldanalysen (fire assay) von Geita und Jubilee Reef belegen eine Wanderung der Erzlösungen durch epigenetische Strukturen in die Magnetitlagen des umgebenden Gesteins. Es konnten weder Zeichen für Lateralsekretion — vom umliegenden Gestein in Erzzonen oder Goldquarzgänge — noch eine Alterationszone im stratigraphisch Liegenden festgestellt werden; beide Phänomene wären deutliche Argumente für ein syngenetisches Konzept (mit teilweiser späterer Umverteilung der Mineralisation). Die Verteilungsmuster der Goldgehalte sprechen gegen eine intraformationelle Herkunft des Goldes.Der Hauptausfällungsmechanismus dürfte eine Redoxreaktion der aufsteigenden reduzierten Erzlösungen mit den Magnetitlagen der BIF gewesen sein. Diese Redoxreaktion hatte die Verdrängung des Magnetit durch Pyrit (Sulfidisierung) sowie eine drastische Erhöhung des Eh-Wertes zur Folge und bedingte so die Ausfällung des Goldes zusammen mit dem Pyrit.Ein epigenetischer Mineralisationsprozeß führte zur Bildung reicher Goldvererzungen unterschiedlicher Typen in sämtlichen stratigraphischen Einheiten. Innerhalb der BIF bedingte die spezielle physiko-chemische Falle der Magnetitlagen die Bildung schichtgebundener Pyrit/Goldmineralisation epigenetischen Ursprungs. Die Erzlösungen stammten vermutlich von granitischen Intrusionen wobei die mafischen Vulkanite des tieferen Nyanzian als naheliegende Lieferanten des Goldes in Betracht kommen.

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Résumé Le «Sukumaland Greenstone Belt» (nouveau nom), situé dans le nord-ouest de la Tanzanie, renferme un grand nombre de venues aurifères, d'importances économiques diverses. Au point de vue stratigraphique, l'Archéen comprend un socle ancien de gneiss granitiques (Système de Dodoman), surmonté de volcanites mafiques à ultramafiques auxquelles succèdent des volcanites felsitiques et une formation ferrugineuse rubanée (BIF = banded iron formation) de faciès essentiellement oxydé. L'ensemble des volcanites de la BIF constitue le Système Nyanzien. La partie supérieure de l'Archéen (Système Kavirondien) consiste en conglomérats et quartzites discordants sur les unités plus anciennes. Le tout a été intrudé par des granitoïdes syn- et post-orogéniques et par plusieurs générations de dykes et sills felsitiques et intermédiaires. La minéralisation en or est abondante dans toutes les unités stratigraphiques, à l'exception des roches granitiques. On peut distinguer six types de minéralisations: celles qui sont contenues dans la BIF, celles qui sont associées à des shear-zones, à des veines de quartz, des paléo-placers, des minéralisations alluviales et éluviales et un type à sulfures massifs, ce dernier représenté seulement par un seul exemplaire.L'emplacement des minéralisations contenues dans la BIF est en relation avec la présence de roches trachytiques en sills ou en dykes et avec des shear-zones bréchiées qui jalonnent le contact entre la BIF et des intercalations de tuf. Les rocheshôtes au voisinage de ces trachytes et de ces shear-zones ont été imprégnées de pyrite, de pyrite aurifère et d'or natif, qui ont remplacé sélectivement les lits de magnétite. Il existe tous les intermédiaires entre les lits remplacés massivement aux contacts trachyte/BIF ou tuf/BIF, les lits à pyrites éparses et les lits stériles. En dehors, et même assez loin de ces zones de contact favorables, des concentrations minéralisées se rencontrent en des endroits perméables, tels que veines, fractures, zones bréchiques et shear-zones.Les textures des minerais ainsi que les analyses (fire assay) du «Geita and Jubilee reef» montrent l'envahissement des roches adjacentes par des solutions minéralisantes circulant dans des conduits épigénétiques. On n'a observé ni halos appauvris dans les roches BIF adjacentes, ni zones d'altération dans les roches stratigraphiquement sous-jacentes, phénomènes susceptibles d'être invoqués à l'appui d'un modèle de remplacement syngénétique.Le mécanisme principal de la précipitation a probablement consisté en une réaction d'oxydo-réduction entre la magnétite de la BIF et les fluides minéralisés réducteurs ascendants. Cette réaction a entraîné le remplacement de la magnétite par la pyrite, une augmentation de Eh et la précipitation simultanée de l'or. Les auteurs proposent un processus de minéralisation épigénétique aboutissant à des dépôts de types divers dans chaque unité stratigraphique. Les pièges physico-chimiques que constituaient les niveaux à magnétite ont conduit à des corps minéralisés de pyrite aurifère d'allure généralement stratiforme. L'origine des fluides minéralisateurs aurifères doit probablement être trouvée dans les intrusions granitiques et les volcanites mafiques sous-jacentes. Des raisons structurales rendent peu probable qu'une fraction importante de l'or provienne de la BIF avoisinante.

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Lead isotopic signatures at the Klein Aub Mine,Namibia — Implications for mineralisation models

Pb and U isotopic data have been obtained for stratabound, sediment-hosted Cu-mineralisation and igneous, volcanic and sedimentary rocks from other stratigraphic levels in the vicinity of the Klein Aub Mine, Namibia, with the aim of investigating possible sources and metal emplacement mechanisms. The results indicate the existence of a pervasive Cu-sulphide mineralisation event, and support metal introduction during a syn-metamorphic (epigenetic) phase. Some indications are also found of another, earlier and possibly syn- or diagenetic, mineralisation event but this aspect requires confirmation by further study. Differences in the degree of radiogenicity of the Pb characterize the various mineralisation styles, the epigenetically mineralised laminite containing Pb of a more radiogenic nature than the other laminites, but also having lower absolute concentrations of Pb and U. A mineralisation age of ca. 600 Ma is indicated but the Pb data can neither confirm nor disprove the conclusions of Borg (1988) and Borg and Maiden (1987) that the basalt of the Doornpoort Formation is a source of the Cu in the Klein Aub deposits.