The lateral and vertical growth of laterite weathering profiles,Hawaiian Islands,USA

The Hawaiian Islands permit investigation of tropical chemical weathering rates and processes on a single rock type, basalt. Chronosequences are investigated as a function of rainfall due to the varying age of each island, including Kauai (~4 Ma), Oahu (~2 Ma), and Hawaii's Kohala Peninsula (~0.3 to 0.17 Ma). Understanding tropical critical zone (CZ) development is vital given the large populations in developing countries that rely on it. HVSR (horizontal-to-vertical spectral ratio) seismic soundings on Kauai indicate that ~60% of the variability in laterite thickness is due to gradients in precipitation, with errors in erosion corrections and variability in the original permeability structure of the volcanic sequence playing important roles. Basalts have higher horizontal than vertical hydraulic conductivity (K_h > K_v) , and local variability in likely drives much of the remaining differences in laterite thickness. HVSR is well suited for estimating laterite thickness as it has been shown to reliably detect the base of the weathering profile, is rapid (20 min/sounding), highly portable, and occupies a very small footprint. Comparison of Kauai and Oahu weathering profiles suggests that the Oahu laterites are fully or nearly fully formed, despite being half the age of Kauai. By contrast, the young laterites on Kohala (~170 to ~300 ka) exhibit greatly contrasting thicknesses, where coastal laterites are thick and interior laterites are thin, suggesting that early weathering on shield volcanoes produces wedge-shaped laterites near the coast. With time, the thick (coastal) end of the wedge propagates upslope such that a fully developed, constant-thickness laterite carapace can form in ~2 Ma or less. The development of thickened coastal laterites on young substrates depends on greater water–rock ratios as vertically infiltrating water upslope is diverted laterally. This view of laterite development is very different compared to endmember models of continental weathering and CZ development. © 2020 John Wiley & Sons, Ltd.     

Magmatic and metallogenetic episodes in the northern tin belt,cordillera real,Bolivia

New K-Ar determinations for granitoid rocks and ores from the northern Bolivian segment (ca. 15°-18° S.) of the Central Andean Cordillera Oriental (Eastern Cordillera) confirm that this region displays a remarkable repetition of magmatic activity and associated lithophile metal mineralization. Intrusion of monzogranites, in part peraluminous, and granodiorites took place in the Mid—to—Late Triassic (apparent age range: 225-202 Ma) and Late Oligocene-Early Miocene (28.4-ca. 19.2 Ma); the two plutonic domains are juxtaposed, with little or no areal overlap, along an essentially linear belt defining the inner boundary of the Central Andean magmatic arc. There is no conclusive evidence of granitoid intrusion during the intervening period, although at least two centres of Upper Cretaceous basic-intermediate hypabyssal-volcanic rocks are known. Whereas the Triassic episode simultaneously affected ca. 200 km of the belt, the Oligocene-Miocene domain experienced a longitudinal (southeastward) migration of activity which, in its later stages (22-19 Ma), coincided with the initiation of widespread volcanism and intrusion on the altiplano, to the west of the granitoid belt.Both intrusive domains may be regarded as the innermost expressions of relatively brief episodes of radical broadening of the Central Andean magmatic arc, possibly generated through abrupt, but minor, decrease in the inclination of eastward subduction at the western plate margin, and attended by a degree of crustal anatexis unattained in the outer parts of the arc. Our radiometric data permit the delimitation of two metallogenetic (W-Sn) sub-provinces in the northern part of the Bolivian tin belt. The tungsten-tin vein deposits associated with the Triassic and Tertiary plutons are very similar, although tungsten appears to be enriched relative to tin in the older domain. There is no radio-metric or petrographic evidence of significant reactivation of older hydrothermal systems in the Tertiary. The late-Early Miocene age (16.3 Ma) determined for the important Oruro Sn-Ag epithermal centre (17° 56' S.) represents an anomaly in the broad southward migration of volcanic and hydrothermal activity defined byGrant et al. (1979) in the central and southern, sub-volcanic, segments of the Bolivian tin-polymetallic belt. Minor Pb-Zn-Ag vein mineralization was probably associated with the Upper Cretaceous basic-intermediate magmatism.

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Zusammenfassung Neue K-Ar Bestimmungen für die granitoiden Gesteine und Erze aus dem nord-bolivischen Segment (ca. 15°-18° S) der mittleren andeanischen Cordillera Oriental (östlichen Cordillera) bestätigen, daß dieses Gebiet eine beachtenswerte Wiederholung der magmatischen Aktivität und der damit verbundenen Erzmineralisierung aufweist. Granodiorite und teilweise Monzogranite mit Aluminium-Überschuß sind in der Mittel- und Spät-Trias (225-202 Ma) und im Spät-Oligozän bis Früh-Miozän (28.4-ca. 19.2 Ma) eingedrungen; die beiden plutonischen Bereiche liegen mit nur geringer oder fehlender Überlappung benachbart längs einem im wesentlichen linearen Gürtel, der den inneren Rand des mittelandinischen magmatischen Bogen abgrenzt. Es gibt keine entscheidende Anzeichen für granitische Intrusionen in der dazwischen liegenden Zeit, obwohl wenigstens zwei Zentren der oberkretazischen basischen bis intermediären, hypabyssalen bis vulkanischen Gesteinen bekannt sind. Während die triassische Episode gleichzeitig ungefähr 200 km des Gebiets beeinflußte, erfuhr der oligozän-miozäne Bereich jedoch eine longitudinale (südöstliche) Wanderung der Aktivität, die, in den jüngeren Stufen, mit der Einleitung des ausgedehnten Vulkanismus und der Intrusion auf dem Altiplano, westlich des granitoiden Gebietes zusammenfiel.Die beiden intrusiven Gebiete könnte man als die innersten Vorgänge verhältnismägig kurzer Episoden einer drastischen Verbreitung des mittleren andinischen magmatischen Bogens betrachten. Diese könnten vielleicht durch die plötzliche Verringerung des Winkels der östlichen Subduktion an der westlichen Plattengrenze entstanden sein, mit einem Grad der Anatexis, der in den äußeren Teilen des Bogens nicht erreicht wurde. Unsere radiometrischen Daten ermöglichen die Abgrenzung zweier metallogenetischen (W-Sn) Unterprovinzen im nördlichen Teil des bolivischen Zinn-Gebiets. Obwohl die mit den triassischen und tertiären Plutonen verbundenen Wolfram-Zinn-Erzgänge einander sehr ähneln, scheint das Wolfram im älteren Bereich dem Zinn gegenüber etwas angereichert zu sein. Es liegen keine radiometrischen oder petrographischen Zeugnisse für eine erhebliche Reaktivierung von älteren hydrothermalen Systemen im Tertiär vor. Ein spätes früh-miozänes Alter (16.3 Ma) wurde für das wichtige Sn-Ag epithermale Zentrum von Oruro bestimmt. Dieses weicht von der allgemeinen nach S gerichteten Wanderung der vulkanischen und hydrothermalen Aktivität in den zentralen und südlichen subvulkanischen Segmenten der bolivischen Zinn-polymetallischen Gürtel ab, die vonGrant et al. (1979) beschrieben wurde. Geringere Pb-Zn-Ag-Erzgangbildung stand wahrscheinlich mit dem oberkretazischen basisch-intermediären Magmatismus in Verbindung.

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Résumé De nouvelles determinations K-Ar sur des roches granitiques et sur du minerais provenant du segment bolivien septentrional (ca. 15°-18° S) de la Cordillère orientale des Andes centrales (Cordillère est) confirme que cette région fut affectée par une activité magmatique répétée auquelle s'associa une activité metalifère riche en métaux lithophiles. Des intrusions de monzogranites, en partie peralumineux et de granodiorites se mirent en place durant le Triassique moyen et supérieur (intervalle d'âge apparent: 225-202 Ma) et durant l'Oligocène moyen et le début du Miocène (24.4-ca. 19.2 Ma). Ces deux domaines plutoniques se juxtaposent avec un recouvrement spatial faible ou nul, le long d'une ceinture essentiellement linéaire définissant la bordure interne de l'arc magmatique des Andes centrales. Bien qu'aucune indication concluante nesitue la mise en place d'intrusions granitiques durant la période intermédiaire, au moins deux centres volcaniques hypabyssaux de composition basique à intermédiaire se sont formés au Crétacé supérieur. L'épisode magmatique du Triassique a affecté simultanément ca. 200 km de la ceinture. Le domaine Oligocène-Miocène, pour sa part, a subi une migration longitudinale (sudest) de l'activité magmatique dont les étapes tardives (22-19 Ma) coîcident avec le déput d'une longue période de volcanisme et d'intrusions sur l'altiplano, à l'ouest de la ceinture granitique.celle des aggregats de grande taille, par des mécanismes de dislocation. La transition est Les deux domaines intrusifs peuvent être causés par un fort élargissement répété et bref de l'arc magmatique des Andes centrales. neut-être dû à une diminution abrupte de l'inclinaison de la zone de subduction orientale à la bordure ouest de la plaque, accompagnée par un degré d'anatexie crustale qui n'atteignit pas la partie externe de l'arc. Les résultats radiométriques obtenus permettent de délimiter deux sous-provinces métallogéniques (W-Sn) dans la partie septentrionale de la ceinture bolivienne stannifère. Les gisements filoniens d'étain et de tungsténe associés aux plutons triassiques et tertiaires sont très semblables; cependant le tungstène semble être plus abondant rapport à l'étain dans le plus vieux domaine. Il n'y a aucune évidence radiométrique ou pétrographique d'une réactivation signicative du système hydrothermal tertiaire. L'age Miocène (16.3 Ma) obtenu pour l'important centre épithermal Sn-Ag d'Oruro (17° 56' S.) représente une anomalie dans la vaste migration sud-est de l'activité volcanique et hydrothermale définie parGrant et al. (1979) dans les segments «sub-volcaniques» central et sud-est de la ceinture polymétallique et stannifére bolivienne. Une faible minéralisation filonienne Pb-Zn-Ag était probalement associée avec le magmatisme intermédiaire à basique du Crétacé supérieur.

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Integration of P- and SH-wave high-resolution seismic reflection and micro-gravity techniques to improve interpretation of shallow subsurface structure: New Madrid seismic zone

Shallow high-resolution seismic reflection surveys have traditionally been restricted to either compressional (P) or horizontally polarized shear (SH) waves in order to produce 2-D images of subsurface structure. The northernmost Mississippi embayment and coincident New Madrid seismic zone (NMSZ) provide an ideal laboratory to study the experimental use of integrating P- and SH-wave seismic profiles, integrated, where practicable, with micro-gravity data. In this area, the relation between “deeper” deformation of Paleozoic bedrock associated with the formation of the Reelfoot rift and NMSZ seismicity and “shallower” deformation of overlying sediments has remained elusive, but could be revealed using integrated P- and SH-wave reflection. Surface expressions of deformation are almost non-existent in this region, which makes seismic reflection surveying the only means of detecting structures that are possibly pertinent to seismic hazard assessment. Since P- and SH-waves respond differently to the rock and fluid properties and travel at dissimilar speeds, the resulting seismic profiles provide complementary views of the subsurface based on different levels of resolution and imaging capability. P-wave profiles acquired in southwestern Illinois and western Kentucky (USA) detect faulting of deep, Paleozoic bedrock and Cretaceous reflectors while coincident SH-wave surveys show that this deformation propagates higher into overlying Tertiary and Quaternary strata. Forward modeling of micro-gravity data acquired along one of the seismic profiles further supports an interpretation of faulting of bedrock and Cretaceous strata. The integration of the two seismic and the micro-gravity methods therefore increases the scope for investigating the relation between the older and younger deformation in an area of critical seismic hazard.     

The Bolton spring site,Connecticut; Early holocene human occupation and environmental changes in southern New England

The recent discovery and excavation of the Bolton Spring Site, located in the glaciated uplands of eastern Connecticut, presents an enigma to archaeologists and geologists interested in dating and interpreting prehistoric human habitation sites. A single discrete charcoal-bearing occupation level at the site was characterized by artifacts of the Middle Archaic Period (8000-6000 B.P.) and contained an abundance of small-mammal remains typical of the Holocene woodland fauna. Although the site seemed to present a clearcut opportunity for radiocarbon-dating, C13-corrected radiocarbon dates from the cultural horizon span nearly three thousand years. Our interpretation is that occupation occurred near the end of a depositional hiatus during which noncultural charcoal accumulated. Subsequent burial of the cultural layer by eolian sediments may have resulted from deflation of pre-existing eolian sediments in the Connecticut River Valley during drier, mid-Holocene conditions. Substantial rockfall activity and rubble movement on adjacent slopes may have been restricted to late Holocene time.     

High-mass X-ray binary SXP18.3 undergoes the longest type II outburst ever seen in the Small Magellanic Cloud

On 2006 August 30, SXP18.3 a high-mass X-ray binary (HMXB) in the Small Magellanic Cloud (SMC) with an 18.3 s pulse period was observed by Rossi X-ray Timing Explorer ( RXTE ). The source was seen continuously for the following 36 weeks. This is the longest type II outburst ever seen from a HMXB in the SMC. During the outburst, SXP18.3 was located from serendipitous XMM–Newton observations. The identification of the optical counterpart has allowed SXP18.3 to be classified as a Be/X-ray binary. This paper will report on the analysis of the optical and weekly RXTE X-ray data that span the last 10 yr. The extreme length of this outburst has for the first time enabled us to perform an extensive study of the pulse timing of a SMC Be/X-ray binary. We present a possible full orbital solution from the pulse timing data. An orbital period of 17.79 d is proposed from the analysis of the Optical Gravitational Lensing Experiment (OGLE) III light curve placing SXP18.3 on the boundary of known sources in the Corbet diagram.     

Sample return of interstellar matter (SARIM)

The scientific community has expressed strong interest to re-fly Stardust-like missions with improved instrumentation. We propose a new mission concept, SARIM, that collects interstellar and interplanetary dust particles and returns them to Earth. SARIM is optimised for the collection and discrimination of interstellar dust grains. Improved active dust collectors on-board allow us to perform in-situ determination of individual dust impacts and their impact location. This will provide important constraints for subsequent laboratory analysis. The SARIM spacecraft will be placed at the L2 libration point of the Sun–Earth system, outside the Earth’s debris belts and inside the solar-wind charging environment. SARIM is three-axes stabilised and collects interstellar grains between July and October when the relative encounter speeds with interstellar dust grains are lowest (4 to 20 km/s). During a 3-year dust collection period several hundred interstellar and several thousand interplanetary grains will be collected by a total sensitive area of 1 m². At the end of the collection phase seven collector modules are stored and sealed in a MIRKA-type sample return capsule. SARIM will return the capsule containing the stardust to Earth to allow for an extraction and investigation of interstellar samples by latest laboratory technologies.     

DuneXpress

The DuneXpress observatory will characterize interstellar and interplanetary dust in-situ, in order to provide crucial information not achievable with remote sensing astronomical methods. Galactic interstellar dust constitutes the solid phase of matter from which stars and planetary systems form. Interplanetary dust, from comets and asteroids, represents remnant material from bodies at different stages of early solar system evolution. Thus, studies of interstellar and interplanetary dust with DuneXpress in Earth orbit will provide a comparison between the composition of the interstellar medium and primitive planetary objects. Hence DuneXpress will provide insights into the physical conditions during planetary system formation. This comparison of interstellar and interplanetary dust addresses directly themes of highest priority in astrophysics and solar system science, which are described in ESA’s Cosmic Vision. The discoveries of interstellar dust in the outer and inner solar system during the last decade suggest an innovative approach to the characterization of cosmic dust. DuneXpress establishes the next logical step beyond NASA’s Stardust mission, with four major advancements in cosmic dust research: (1) analysis of the elemental and isotopic composition of individual interstellar grains passing through the solar system, (2) determination of the size distribution of interstellar dust at 1 AU from 10^− 14 to 10^− 9 g, (3) characterization of the interstellar dust flow through the planetary system, (4) establish the interrelation of interplanetary dust with comets and asteroids. Additionally, in supporting the dust science objectives, DuneXpress will characterize dust charging in the solar wind and in the Earth’s magnetotail. The science payload consists of two dust telescopes of a total of 0.1 m² sensitive area, three dust cameras totaling 0.4 m² sensitive area, and a nano-dust detector. The dust telescopes measure high-resolution mass spectra of both positive and negative ions released upon impact of dust particles. The dust cameras employ different detection methods and are optimized for (1) large area impact detection and trajectory analysis of submicron sized and larger dust grains, (2) the determination of physical properties, such as flux, mass, speed, and electrical charge. A nano-dust detector searches for nanometer-sized dust particles in interplanetary space. A plasma monitor supports the dust charge measurements, thereby, providing additional information on the dust particles. About 1,000 grains are expected to be recorded by this payload every year, with 20% of these grains providing elemental composition. During the mission submicron to micron-sized interstellar grains are expected to be recorded in statistically significant numbers. DuneXpress will open a new window to dusty universe that will provide unprecedented information on cosmic dust and on the objects from which it is derived.     

An optical and X-ray study of the counterpart to the Small Magellanic Cloud X-ray binary pulsar system SXP327

Optical and X-ray observations are presented here of a newly reported X-ray transient system in the Small Magellanic Cloud. The data reveal many previously unknown X-ray detections of this system and clear evidence for a 45.99 d binary period. In addition, the optical photometry shows recurring outburst features at the binary period which may be well indicative of the neutron star interacting with a circumstellar disc around a Be star.