Structural incorporation of Cm(III) in trioctahedral smectite hectorite: A time-resolved laser fluorescence spectroscopy (TRLFS) study     

Heike Brandt  Dirk Bosbach  Petra J. Panak 《Geochimica et cosmochimica acta》2007,71(1):145-154

Structural incorporation of the actinide curium in the octahedral layer of the trioctahedral Mg-rich smectite hectorite was studied using time-resolved laser fluorescence spectroscopy. Organo-hectorite nanoparticles were synthesized at 90 °C in the presence of Cm(III). Within 120 h, hectorite particles were formed. Time-resolved laser fluorescence spectroscopy was used to identify Cm(III) species during various synthesis steps and to characterize the structural incorporation mechanism. The formation of a Cm-containing Mg hydroxide precursor and the reaction with aqueous silica in a pH range of 9-10 to form TOT layers were identified to be key steps for trivalent actinide incorporation in hectorite via coprecipitation.  相似文献   

Geological controls on the formation of alluvial meanders and floodplain wetlands: the example of the Klip River,eastern Free State,South Africa     

S. Tooth  T. S. McCarthy  D. Brandt  P. J. Hancox  R. Morris 《地球表面变化过程与地形》2002,27(8):797-815

Floodplain wetlands are common features of rivers in southern Africa, but they have been little studied from a geological or geomorphological perspective. Study of the upper Klip River, eastern Free State, South Africa, indicates strong geological controls on the formation of alluvial meanders and associated floodplain wetlands. Along this river, pronounced and abrupt changes in valley width are strongly linked to lithological variations. Where weakly cemented sandstone crops out, the Klip has laterally eroded bedrock and carved valleys up to 1500 m wide. In these valleys, the river meanders (sinuosity up to ～1·75) on moderate gradients (<0·001) within extensive floodplains marked by numerous oxbow lakes, backswamps and abandoned channels, many of which host substantial wetlands. In contrast, where highly resistant dolerite crops out, lateral erosion of bedrock is restricted, with the Klip tending instead to erode vertically along joints or fractures. Here, valleys are narrower (<200 m), channel‐bed gradients are steeper (>0·003), the river follows a much straighter course (sinuosity ～1·10–1·34), and floodplains are restricted in width. Long‐term landscape development in the Klip and numerous similar catchments depends on the interaction between fluvial processes in the sandstone and dolerite valleys. In the sandstone valleys, vertical erosion rates are controlled by erosion rates of the more resistant dolerites downstream. Hence, in the short‐ to medium‐term (decades to tens of thousands of years), lateral erosion dominates over vertical erosion, with the river concomitantly planing sandstone in the channel floor and reworking floodplain sediments. The thickness of alluvial fill in the sandstone valleys is limited (<4 m), but the resultant meanders are naturally dynamic, with processes such as point bar deposition, cutoff formation and channel avulsion resulting in an assemblage of fluvial landforms. In the longer term (greater than tens of thousands of years), however, vertical erosion will occur in the sandstone valleys as the downstream dolerites are lowered by erosion, resulting in channel incision, floodplain abandonment, and desiccation of the wetlands. Identification of the geological controls on meander and wetland formation provides information vital for the design of effective management guidelines for these ecologically rich habitats, and also contributes to a better understanding of rivers that are intermediate between fully alluvial and fully bedrock. Copyright © 2002 John Wiley & Sons, Ltd.  相似文献   

Facular excess radiation and the energy balance of solar active regions     

M. Steinegger  H. Haupt  P. N. Brandt  W. Schmidt 《Solar physics》1994,152(1):317-317

Plage areas and intensities derived from CaII K spectroheliograms are used as a proxy for the facular irradiance excess of solar active regions for the period 19 August to 4 September 1980. Using a calibration method proposed by Vrnak et al. (1991), the photospheric facular index (PFI) with constant facular contrastC _p = 0.018 is replaced by a variableC _p , depending on the plage brightness. A sgnificant increase ofC _p from 0.015 to 0.025 is found for plage areas varying from a few to approx. 6 · 10³ millionths hemispheres.Combining the facular irradiance excess with sunspot deficits (as determined for the same period by Steinegger et al. 1990) yields good aggrement with the irradiance variations measured by ACRIM I, using a center-to-limb variation ofC _p according to Chapman and Meyer (1986). The ratio of facular excess to sunspot deficit (integrated over solid angle 2) decreases from values of 1.5 to 2 for regions with sunspot areas below 100 millionths hemispheres to 0.2 for sunspots of areas > 1000 millionths hemispheres,  相似文献   

Limits on the X-ray emission from several hyperluminous IRAS galaxies     

R. J. Wilman  A. C. Fabian  R. M. Cutri  C. S. Crawford  & W. N. Brandt 《Monthly notices of the Royal Astronomical Society》1998,300(1):L7-L10

We report long, pointed ROSAT HRI observations of the hyperluminous galaxies IRAS F00235+1024, F12514+1027, F14481+4454 and F14537+1950. Two of them are optically classified as Seyfert-like. No X-ray sources are detected at the positions of any of the objects, with a mean upper limit L _X/ L _Bol ≃ 2.3 × 10⁻⁴. This indicates that any active nuclei are either atypically weak at X-ray wavelengths or obscured by column densities N _H > 10²³ cm⁻². They differ markedly from 'ordinary' Seyfert 2 galaxies, bearing a closer resemblance in the soft X-ray band to composite Seyfert 2 galaxies or to some types of starburst.  相似文献   

The ASCA spectrum of the z = 4.72 blazar GB 1428+4217     

A. C.Fabian  K.Iwasawa  A.Celotti  W. N.Brandt  R. G.McMahon  I. M.Hook 《Monthly notices of the Royal Astronomical Society》1998,295(1):l25-l28

The X-ray-luminous quasar GB 1428+4217 at redshift 4.72 has been observed with ASCA . The observed 0.5–10 keV flux is 3.2 Å– 10⁻¹² erg cm⁻² s⁻¹. We report here on the intrinsic 4 − 57 keV X-ray spectrum, which is very flat (photon index 1.29). We find no evidence for flux variability within the ASCA data set or between it and ROSAT data. We show that the overall spectral energy distribution of GB 1428+4217 is similar to that of lower redshift MeV blazars, and present models that fit the available data. The Doppler beaming factor is likely to be at least 8. We speculate on the number density of such high-redshift blazars, which must contain rapidly formed massive black holes.  相似文献   

General astrophysics with elements of geophysics: J. S. Stodólkiewicz. Elsevier,New York, 1973. 218 pp. price $10.50     

John C. Brandt 《Icarus》1974,23(1):136-137

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Visualisation and evaluation of flood uncertainties based on ensemble modelling   总被引：1，自引：0，他引：1  

N. J. Lim  S. A. Brandt  S. Seipel 《International journal of geographical information science》2016,30(2):240-262

This study evaluates how users incorporate visualisation of flood uncertainty information in decision-making. An experiment was conducted where participants were given the task to decide building locations, taking into account homeowners’ preferences as well as dilemmas imposed by flood risks at the site. Two general types of visualisations for presenting uncertainties from ensemble modelling were evaluated: (1) uncertainty maps, which used aggregated ensemble results; and (2) performance bars showing all individual simulation outputs from the ensemble. Both were supplemented with either two-dimensional (2D) or three-dimensional (3D) contextual information, to give an overview of the area.

The results showed that the type of uncertainty visualisation was highly influential on users’ decisions, whereas the representation of the contextual information (2D or 3D) was not. Visualisation with performance bars was more intuitive and effective for the task performed than the uncertainty map. It clearly affected users’ decisions in avoiding certain-to-be-flooded areas. Patterns to which the distances were decided from the homeowners’ preferred positions and the uncertainties were similar, when the 2D and 3D map models were used side by side with the uncertainty map. On the other hand, contextual information affected the time to solve the task. With the 3D map, it took the participants longer time to decide the locations, compared with the other combinations using the 2D model.

Designing the visualisation so as to provide more detailed information made respondents avoid dangerous decisions. This has also led to less variation in their overall responses.  相似文献   

Evolution of the Molopo drainage and its possible disruption by the Morokweng impact event at the Jurassic-Cretaceous boundary     

Cornelis S. Bootsman  Wolf Uwe Remold  Dion Brandt 《Journal of African Earth Sciences》1999,29(4):437

A large, deeply eroded impact structure, known as the Morokweng impact structure, has recently been positively identified in the North West Province of South Africa, centred on the Ganyesa Dome about 80 km northwest of Vryburg. The marked geomorphic effect of the Morokweng impact event at 145 ± 2 Ma is identified through large-scale analysis of the long-term evolution of the Molopo River drainage system. A comparison of the pre- and post-impact drainage patterns shows that a dramatic change in both drainage direction and pattern occurred after the impact event. Prior to the impact, the regional drainage direction of the proto-Molopo had been towards the northwest, where it connected with the major southwest trending drainage line of the Permo-Carboniferous (300 Ma) Kalahari Basin. Reconstruction of the post-impact drainage pattern, as it existed in the Late Cretaceous ( 75 Ma), just before the formation of the rejuvenated Cenozoic Kalahari Basin, shows a generally southward flowing system with annular drainage pattern components. With the filling of the Kalahari Basin since Tertiary times, the affinity between the Molopo drainage and the Morokweng impact structure became less obvious.  相似文献   

Variability of the extreme z = 4.72 blazar, GB 1428+4217     

A. C. Fabian  A. Celotti  G. Pooley  K. Iwasawa  W. N. Brandt  R. G. McMahon  M. D. Hoenig 《Monthly notices of the Royal Astronomical Society》1999,308(1):L6-L10

On 1998 May 9–11, the highly variable, low-luminosity Seyfert 1 galaxy NGC 4051 was observed in an unusual low-flux state by BeppoSAX , RXTE and EUVE . We present fits of the 4–15 keV RXTE spectrum and BeppoSAX MECS spectrum obtained during this observation, which are consistent with the interpretation that the source had switched off, leaving only the spectrum of pure reflection from distant cold matter. We place this result in context by showing the X-ray light curve of NGC 4051 obtained by our RXTE monitoring campaign over the past two and a half years, which shows that the low state lasted for ∼150 d before the May observations (implying that the reflecting material is >10¹⁷ cm from the continuum source) and forms part of a light curve showing distinct variations in long-term average flux over time-scales > months. We show that the long-time-scale component to X-ray variability is intrinsic to the primary continuum and is probably distinct from the variability at shorter time-scales. The long-time-scale component to variability maybe associated with variations in the accretion flow of matter on to the central black hole . As the source approaches the low state, the variability process becomes non-linear. NGC 4051 may represent a microcosm of all X-ray variability in radio-quiet active galactic nuclei (AGNs), displaying in a few years a variety of flux states and variability properties which more luminous AGNs may pass through on time-scales of decades to thousands of years.  相似文献   

Shift-and-add reconstruction of solar granulation images     

Baba  N.  Miura  N.  Sakurai  T.  Ichimoto  K.  Soltau  D.  Brandt  P. 《Solar physics》1999,188(1):41-46

To restore an atmospherically degraded image of solar granulation the shift-and-add (SAA) method is applied to its specklegrams. It is the first time, to the best of our knowledge, that such a technique has been used for image reconstruction of solar granulation, a largely extended target. SAA, therefore, enables us to monitor restored images of solar granulation in a simple and fast way.  相似文献