The Extreme Precipitation Event of 11 to 16 February 1996 over South Africa

Summary  The extreme precipitation event of 11 to 16 February 1996 was one of four significant events during the 1995/96 rainfall season over southern Africa. Extensive flooding and related damage was recorded at this time, with historical records showing one of the highest flood peaks of the past century. This extreme event is analysed using a combination of mesoscale numerical modelling and Lagrangian trajectory analysis, allowing a comprehensive three-dimensional reconstruction of the associated atmospheric structure and its evolution. The adjustments in the circulation patterns as well as the timing and contribution of different moisture source regions are clearly important in influencing the duration and intensity of this extreme rainfall event over southern Africa. The moisture that contributed to precipitation during the event, as well as to the south-western part of the country, was imported mainly from the Indian Ocean tothe east and south-east, suggesting that the equatorial Indian Ocean may not be the predominant source of moisture as previously believed. Received October 13, 1998 Revised December 28, 1998     

Cross-correlation of the unresolved X‐ray background with faint galaxies

At the faint end of the deepest X-ray surveys, a population of X-ray luminous galaxies is seen. In this paper, we present the results of a cross-correlation between the residual, unresolved X-ray photons in a very deep X-ray survey and the positions of faint galaxies, in order to examine the importance of these objects at even fainter flux levels. We measure a significant correlation on all angular scales up to ∼1 arcmin. This signal could account for a significant fraction of the unresolved X‐ray background, approximately 35 per cent if the clustering is similar to optically selected galaxies. However, the angular form of the correlation is seen to be qualitatively similar to that expected for clusters of galaxies and the X-ray emission could be associated with hot gas in clusters or with QSOs within galaxy clusters rather than emission from individual faint galaxies. The relative contribution from each of these possibilities cannot be determined with the current data.     

A numerical study of cloud streets in the planetary boundary layer

A two-dimensional numerical model is used to study the influence of small non-precipitating clouds on horizontal roll vortices in the planetary boundary layer. The model explicitly represents the large-scale two-dimensional motions whilst small-scale eddies are parameterized by a buoyancy dependent mixing-length hypothesis. It is applied to conditions corresponding to an observed case of cloud street formation.     

Flow over the summit of an isolated hill

Observations of the mean flow and turbulence statistics over the summit of an isolated, roughly circular hill, Nyland hill, are presented, Nyland hill rises 70 m above the surrounding terrain and has a base diameter of about 500 m. The summit of the hill is very smooth and allows representative measurements to be made close to the surface. The flow speed 8 m above the summit is increased by a factor of 2 over the upstream speed 8 m above level terrain, and flow separation occurs in the lee of the hill. The mean velocity profile over the summit shows an increase in velocity with height up to about 2 m and then a near constant velocity between 2 and 16 m. The flow perturbation relative to the upstream profile is thus a maximum at about 2 m. The measurements of turbulence structure show how the influence of the hill depends on the length scale of the turbulent eddies involved. Scales greater than the scale of the hill are modified through the flow speed-up whilst scales shorter than the hill suffer complex changes. The short-scale turbulence over the summit is only in local equilibrium in the lowest fraction of a metre. Above this equilibrium region, there is a complex adjustment towards the rapid distortion dynamics which appear to dominate at heights above about 8 m. The detailed results are compared with previous studies and available theories.     

Trace and minor elements in sphalerite: A LA-ICPMS study

Sphalerite is an important host mineral for a wide range of minor and trace elements. We have used laser-ablation inductively coupled mass spectroscopy (LA-ICPMS) techniques to investigate the distribution of Ag, As, Bi, Cd, Co, Cu, Fe, Ga, Ge, In, Mn, Mo, Ni, Pb, Sb, Se, Sn and Tl in samples from 26 ore deposits, including specimens with wt.% levels of Mn, Cd, In, Sn and Hg. This technique provides accurate trace element data, confirming that Cd, Co, Ga, Ge, In, Mn, Sn, As and Tl are present in solid solution. The concentrations of most elements vary over several orders of magnitude between deposits and in some cases between single samples from a given deposit. Sphalerite is characterized by a specific range of Cd (typically 0.2-1.0 wt.%) in each deposit. Higher Cd concentrations are rare; spot analyses on samples from skarn at Baisoara (Romania) show up to 13.2 wt.% (Cd²⁺ ↔ Zn²⁺ substitution). The LA-ICPMS technique also allows for identification of other elements, notably Pb, Sb and Bi, mostly as micro-inclusions of minerals carrying those elements, and not as solid solution. Silver may occur both as solid solution and as micro-inclusions. Sphalerite can also incorporate minor amounts of As and Se, and possibly Au (e.g., Magura epithermal Au, Romania). Manganese enrichment (up to ∼4 wt.%) does not appear to enhance incorporation of other elements. Sphalerite from Toyoha (Japan) features superimposed zoning. Indium-sphalerite (up to 6.7 wt.% In) coexists with Sn-sphalerite (up to 2.3 wt.%). Indium concentration correlates with Cu, corroborating coupled (Cu⁺In³⁺) ↔ 2Zn²⁺ substitution. Tin, however, correlates with Ag, suggesting (2Ag⁺Sn⁴⁺) ↔ 3Zn²⁺ coupled substitution. Germanium-bearing sphalerite from Tres Marias (Mexico) contains several hundred ppm Ge, correlating with Fe. We see no evidence of coupled substitution for incorporation of Ge. Accordingly, we postulate that Ge may be present as Ge²⁺ rather than Ge⁴⁺. Trace element concentrations in different deposit types vary because fractionation of a given element into sphalerite is influenced by crystallization temperature, metal source and the amount of sphalerite in the ore. Epithermal and some skarn deposits have higher concentrations of most elements in solid solution. The presence of discrete minerals containing In, Ga, Ge, etc. also contribute to the observed variance in measured concentrations within sphalerite.     

Paleogene crustal anatexis and metamorphism in Lhasa terrane, eastern Himalayan syntaxis: Evidence from U-Pb zircon ages and Hf isotopic compositions of the Nyingchi Complex

In the eastern Himalayan syntaxis, the southern Lhasa terrane is dominated by middle- to high-grade metamorphic rocks (Nyingchi Complex), which are intruded by felsic melts. U-Pb zircon dating and zircon Hf isotopic composition of these metamorphic and magmatic rocks provide important constraints on the tectono-thermal evolution of the Lhasa terrane during convergent process between Indian and Asian continents. U-Pb zircon data for an orthogneiss intruding the Nyingchi Complex yield a protolith magma crystallization age of 83.4 ± 1.2 Ma, with metamorphic ages of 65-46 Ma. This orthogneiss is characterized by positive ε_Hf (t) values of + 8.3 and young Hf model ages of ~ 0.6 Ga, indicating a derivation primarily from a depleted-mantle or juvenile crustal source. Zircons from a quartz diorite yield a magma crystallization age of 63.1 ± 0.6 Ma, with ε_Hf (t) values of − 8.2 to − 2.7, suggesting that this magma was sourced from partial melting of older crustal materials. Zircon cores from a foliated biotite granite show ages ranging from 347 to 2690 Ma, with age peaks at 347-403 Ma, 461-648 Ma and 1013-1183 Ma; their zircon ε_Hf (t) values range from − 30.6 to + 6.9. Both the U-Pb ages and Hf isotopic composition of the zircon cores are similar to those of detrital zircons from the Nyingchi Complex paragneiss, implying that the granite was derived from anatexis of the Nyingchi Complex metasediments. The zircon rims from the granite indicate crustal anatexis at 64.4 ± 0.7 Ma and subsequent metamorphism at 55.1 ± 1.3 and 41.4 ± 2.3 Ma. Our results suggest that the late Cretaceous magmatism in the southern Lhasa terrane resulted from Neo-Tethys oceanic slab subduction and we infer that Paleocene crustal anatexis and metamorphism were related to the thermal perturbation caused by rollback of the northward subducted Neo-Tethyan oceanic slab.     

Internal structure of a barrier beach as revealed by ground penetrating radar (GPR): Chesil beach, UK

Chesil Beach (Dorset) is one of the most famous coastal landforms on the British coast. The gravel beach is over 18 km long and is separated for much of its length from land by a tidal lagoon known as The Fleet. The beach links the Isle of Portland in the east to the mainland in the west. Despite its iconic status there is little available information on its internal geometry and evolutionary history. Here we present a three-fold model for the evolution of Chesil Beach based on a series of nine ground penetrating radar (GPR) traverses located at three sites along its length at Abbotsbury, Langton Herring and at Ferry Bridge. The GPR traverses reveal a remarkably consistent picture of the internal structure of this barrier beach. The first phase of evolution involves the landward transgression of a small sand and gravel beach which closed upon the coast leading to deposition of freshwater peat between 5 and 7 k yr BP. The second evolutionary phase involves the ‘bulking-out’ of the beach during continued sea level rise, but in the presence of abundant gravel supplied by down-drift erosion of periglacial slope deposits. This episode of growth was associated with a series of washover fans which accumulated on the landward flank of the barrier increasing its breadth and height but without significant landward transgression of the barrier as a whole. The final phase in the evolution of Chesil Beach involves the seaward progradation of the beach crest and upper beach face associated with continued sediment abundance, but during a still-stand or slight fall in relative sea level. This phase may provide further evidence of a slight fall in relative sea level noted elsewhere along the South Coast of Britain and dated to between 1.2 and 2.4 k yr BP. Subsequently the barrier appears to have become largely inactive, except for the reworking of sediment on the beach face during storm events. The case study not only refines the evolutionary picture of Chesil Beach, but illustrates the importance of the subtle interplay between relative sea level and sediment supply in the evolution of a barrier system. In addition, it also illustrates the potential of GPR in resolving the evolutionary history of gravel-rich coastal landforms such as Chesil Beach.     

A volcano under China's Great Wall

Cone sheets are rare in China but are found in the Houshihushan sub‐volcanic Ring Complex (HRC) near the town of Shanhaiguan, Hebei Province. The HRC rises above a narrow coastal plain as the Houshihushan mountain massif (Fig. 1 ) in a scenic region about 400 km ENE of Beijing by the Bohai Gulf, where the Great Wall reaches the sea. It has a discontinuous outer ring‐dyke of porphyritic quartz syenite, separated from an inner stock of alkaline granite by a discontinuous screen of pyroclastic rocks down‐faulted to the present erosion level by caldera subsidence. The pyroclastic rocks, which have similar petrographic and geochemical characteristics to intrusive rocks of the ring‐dyke, cone‐sheets and central stock, were erupted from the same volcano and subsequently foundered during caldera subsidence.     

The abundance of ammonia in the atmosphere of Jupiter

A laboratory curve of growth analysis was made on the lines in two ammonia bands located at 6450 Å and 10800 Å and the abundance of ammonia in the atmosphere of Jupiter was determined. Lines in the 6450 Å band appear to fall on the weak line section of the curve of growth, while those in the 10800 Å band fall in the transition region. The abundance values obtained from these bands are 13.0±3 m atm and 15±8 m atm, respectively.Measurements of the intensity distribution in the 6450 Å band in the laboratory and in the Jovian spectra show that the intensity of several lines in this band is highly dependent on the temperature. Strengths for some of the lines in the 6450 Å band were determined and half-widths of some strong lines were also measured. The effective pressure found from these half-width values is 2.5 atmospheres.Contributions from the University of Illinois, Chicago Circle Physics Department, No. 12.