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Pyroclastic deposits of Ubehebe Crater, Death Valley, California, USA: Ballistics, pyroclastic surges, and dry granular flows
Citizen science campaign reveals widespread fallout of contaminated dust from mining activities in the central Peruvian Andes
The Late Bronze Age Eruption of Santorini Volcano and Its Impact on the Ancient Mediterranean World
An inclined Vulcanian explosion and associated products
The 1970 eruption on Deception Island (Antarctica): eruptive dynamics and implications for volcanic hazards
We use the occurrence of unusual or out-of-season dust storms and dissolved ion data as proxies for dust to propose a calendar-year chronology for a portion of the Greenland Ice Sheet Project 2 (GISP2) ice core during the early sixth century A.D. Our new time scale moves a small sulfate peak to early 537 A.D., which is more consistent with recent findings of a 6 mo to 18 mo time lag between volcanic eruptions and atmospheric fallout of their sulfate aerosols. Our new time scale is consistent with a small volcanic input to the A.D. 536–537 climate downturn. We use the time range of Ni-rich fragments and cosmic spherules to provide an independent test of the chronology. The time range of Ni-rich fragments and cosmic spherules matches historical observations of “dancing stars” starting in the summer of A.D. 533 and lasting until A.D. 539 or 540. These dancing stars have been previously attributed to cosmogenic dust loading of Earth's atmosphere. The time scale cannot be shifted to be either younger or older by 1 yr without destroying the match to historical accounts of dancing stars.
Stratigraphic correlation of Holocene phonolitic explosive episodes of the Teide–Pico Viejo Volcanic Complex, Tenerife
Current radiation environment in the Central Ecological Zone of the Baikal Natural Territory
A detailed total intensity magnetic survey of a local negative magnetic anomaly located in the southern sector of the inner ring in the Ries impact structure was carried out in 2006–2007. As the suevite of the Ries crater is known to have an often strong reverse remanent magnetization causing negative magnetic anomalies, a suevite body lying below shallow lake sediments upon the crystalline basement rocks of the inner ring was suspected to be the cause of the anomaly. A drilling program conducted by the Geological Service of Bavaria offered the opportunity to drill a 100-m-deep core hole into this anomaly in 2006. The core stratigraphy involves from 0 to 4.5 m fluviatile Quaternary lake sediments, from 4.5 to 21 m Neogene clays of the Ries crater lake, and from 21 to 100 m suevite and impact melt rock. The suevite and the impact melt rock have a strong reverse remanent magnetization and very high Koenigsberger ratios. Thermomagnetic and coercivity analyses indicate that magnetite is the dominant carrier of the magnetization. The borehole unfortunately did not penetrate the crystalline basement rocks of the inner ring, but modeling of the magnetic source body indicates that the bottom of the hole could not be far from the contact. A macroscopic survey shows suevite from 21 to 87 m, highly diverse in terms of suevite types, and a gradational transition to massive impact melt rock constituting the lowermost 13 m of the drill core. A detailed macroscopic description and first results of microscopic observations reveal that suevite groundmass is substantially altered to secondary phyllosilicates (mostly smectite, minor chlorite) and locally extensive development of calcite. Crystalline basement–derived lithic clasts and minerals dominate the clast population, and only traces of clastic material derived from the upper sediment parts of the target could be recorded. Macroscopically and microscopically, melt fragments have mostly irregular shapes, which lead to the tentative conclusion that only part of the melt—and by implication suevite—mass is derived from fallout of the ejecta curtain. On the other hand, most melt fragments and larger lithic clasts are seemingly oriented subperpendicular to the core axis. This could be interpreted as being due alternatively to settling through air or lateral movement within the actual crater. The gradational zone between proper suevite and massive impact melt rock is characterized by increasing enrichment of melt component and concomitant reduction of suevitic groundmass, until in the uppermost impact melt rock, only millimeter-wide stringers of groundmass remain between densely packed centimeter- to decimeter-size melt fragments.
A petrographic and geochemical comparison of suevites from the LB-07A and LB-08A cores recovered during 2004 by the International Continental Scientific Drilling Program with suevites from outside of the crater rim of the Bosumtwi impact structure indicates contrasting mechanisms of formation for these respective impact breccias. The within-crater suevites form only a small part of the lithic impact breccia–dominated impactite crater fill, in contrast to the impactites from outside of the crater, which consist solely of suevite. The clasts of suevites from within the crater display relatively low levels of shock (for most material <45 GPa). The numbers of shocked quartz grains, as well as fragments of diaplectic glass of quartz and feldspar in suevites decrease with depth through the LB-07A core (maximum three sets of planar deformation features [PDFs]). In contrast, the out-of-crater suevites sampled north and south of the crater contain up to four PDF sets in quartz clasts, ballen cristobalite, and higher proportions of diaplectic glass than the within-crater suevites. In addition, the suevites from outside of the crater contain significantly more melt particles (18–37 vol%) than the within-crater suevites (<5 vol%). Melt fragment sizes in suevites from outside the crater are much larger than those from suevites within the crater (maximum 40 cm versus 1 cm). The currently known distribution of impactites outside of the crater would be consistent with a low-angle impact from the east. We propose that the within-crater suevites and polymict lithic breccias were emplaced either via slumping off the crater walls or lateral movement of some melted and much displaced target rock within the crater. Limited admixture of fallback material from the ejecta plume is evident in the uppermost impactite deposit encountered in core LB-05B. In contrast, the out-of-crater suevites formed by fallout from a laterally differentiated ejecta plume, which resulted in different clast populations to the north and south of the crater.
Crater-fill impact breccia and basement rock samples from the 1.07 Ma Bosumtwi impact structure (Ghana) were recovered for the first time in 2004 during an International Continental Scientific Drilling Program (ICDP)–sponsored drilling project. Here, we present detailed results of major- and trace-element analyses of 119 samples from drill core LB-08A, together with the chemical compositions of melt particles from suevite. The meta-graywacke and phyllite/slate crater basement rocks can be easily distinguished from each other on the basis of their bulk chemical compositions. A comparison of the chemical compositions of crater-fill and fallout suevites, as well as between proximal and distal impactites, reveals that LB-08A suevites have higher MgO, CaO, and Na 2 O contents than fallout suevites and, similarly, that the CaO and Na 2 O contents are higher by a factor of approximately two in LB-08A suevites than in Ivory Coast tektites. Noticeable differences occur in Cr, Co, and Ni contents between the different impactites; higher abundances are observed for these elements in distal impactites. The observed differences in composition in the various impactites mainly reflect mixing of different proportions of the original target lithologies, as can be seen in the differences in the clast populations between crater-fill and fallout suevites. However, the original impactite compositions may have also been modified by postimpact alteration, particularly in the proximal impactites. Melt particles in suevite show significant differences in major-element compositions between the different samples investigated, but also within a given sample, indicating that they represent melts derived from different lithologies.
TRAVELOGUE
The 1944 eruption of Vesuvius, Italy: combining contemporary accounts and field studies for a new volcanological reconstruction
Acid-fog deposition at Kilauea volcano: A possible mechanism for the formation of siliceous-sulfate rock coatings on Mars
Geochemistry, tectonomagmatic origin and chemical correlation of altered Carboniferous–Permian fallout ash tuffs in southwestern Germany
Time Variations of Natural Gamma Radiation
Contaminated Sediment in Two United Kingdom Estuaries
Isotope geochemistry of dissolved, precipitated, airborne, and fallout sulfur species associated with springs near Paige Mountain, Norman Range, N.W.T.
Impacts of kilometer-sized objects are expected to deposit many thousand megatons of energy in the air through the explosive expansion of vapor products. The fireball grows to a radius equal an atmospheric scale-height while the internal pressure is high. The fireball is accelerated upward by interaction with atmospheric pressure and density gradients. Gas velocities will reach orbital speeds before interaction with the magnetic field stops the rise, provided that the original energy deposited in the air exceeds roughly 12,000 Mt. Because the Cretaceous-Tertiary impact probably deposited several times this much energy in the atmosphere, gradient acceleration provides a probable mechanism for the worldwide dispersal of micrometer particles within a few hours after the impact.
We have simulated the evolution of an optically thick dust cloud in the Earth’s atmosphere and have also calculated the effects such a dust cloud would have both on the amount of visible light reaching the surface and on the temperature at the Earth’s surface. The dust cloud simulations utilize a sophisticated 1-D model of aerosol physics. We find that large quantities of dust remain in the atmosphere for periods of only 3 to 6 months. This duration is fixed by the physical processes of coagulation, which cause micron-sized particles to quickly form and sedimentation that swiftly removes the micron-size particles from the atmosphere. The duration of the event is nearly independent of the initial altitude, initial particle size, initial mass, atmospheric vertical diffusive mixing rate, or rainout rate. The duration depends weakly upon the particle density and the probability that colliding particles stick together to form a larger particle. The duration is also limited by the rate at which the debris spreads from the initial impact site. The dust must be uniformly spread over a large fraction of the Earth within a few weeks or the duration of the event will be less than 2 months. We used a doubling code to calculate the visible radiative transfer in these dust clouds. We find that light levels are too low for vision for 1 to 6 months and too low for photosynthesis for 2 months to 1 year. Calculations of the surface temperature show that the oceans cool by only a few degrees owing to their large heat capacity. However, continental surface temperatures drop below freezing for approximately twice as long as sub-photosynthetic light levels persist. We speculate briefly upon several other effects that might occur after the dust clears due to widespread snowfields, enhanced H 2 O amounts, or chemical changes in the atmosphere. We also speculate that low light levels would cause a collapse of the marine food chain and oceanic extinctions. Cold temperatures over the continents and low light levels would prevent some animals from finding food and would cause continental extinctions.