IDENTIFICATION AND ASSESSMENT OF PROBLEMATIC EXPANSIVE SOILS

Published ThesisIn the last few decades the construction of small dwellings, particularly government subsidy houses, has increased markedly in South Africa. Large numbers of these light structures have suffered severe damage and many have been demolished after being occupied for only a small fraction of their expected life-span. The research detailed in this thesis deals with a search for reasons for these widespread failures and investigations into economically feasible solutions. The investigation began with an assessment of the current methods of identification and assessment of potentially problematic expansive soils. This revealed serious shortcomings in a number of the standard testing procedures. These shortcomings may have consequences for a wider range of engineering projects than just housing development. Progress towards more reliable testing methods has led to an appreciation of the importance of variability of soil properties and the necessity of taking this into account in engineering design. Investigation of clay fraction determination by the hydrometer has led to the realization that the unreliability of this procedure has been a cause of failure in subsidy housing projects as well as other light structure developments. Assessment of expansive potential cannot safely rely on hydrometer determination of clay fraction, which is a principal parameter for a number of popular design procedures. It was also established that attractive alternatives in the form of automatic particle sizing equipment (designed for the analysis of industrial powders) are not suitable for natural soils containing the clays commonly found in South African soils. Alternative procedures, particularly small-scale suction testing, have been found to provide more reliable insights into design for expansive clays. The investigations suggest that some form of Reliability Based Design, which takes account of specific variability in soil properties, may be the only way to achieve rational design for foundations on expansive clay

The evolution of galaxies in massive clusters

We present a study of the evolution of galaxies in massive X-ray selected clusters across half the age of the Universe. This encompasses galaxies on the red sequence from the Brightest Cluster Galaxy (BCG) to the faint red population. We begin at the tip of the red sequence with an investigation into the near infrared evolution of BCGs since z =1. By comparing the BCG Hubble diagram and near-infrared colour evolution to a set of stellar population and semi-analytic models we constrain the evolution and formation redshift of these massive galaxies. Moving down in luminosity from the BCG, in chapter 3 we study the build up of the red sequence in massive clusters. To achieve this we compare the luminosity functions for red galaxies in a homogeneous sample of ten X-ray luminous clusters at z ~ 0.5 to a similarly selected X-ray cluster sample at z ~ 0.1. We quantify this result by measuring the dwarf to giant ratio to ascertain whether faint galaxies have joined the red sequence over the last 5 Gyr. In chapter 4 we study the evolution of the red sequence slope in massive clusters from z=l to present day. We compare our observed slope evolution to that predicted from semi- analytical models based on the Millennium simulation. We also look for trends between the red sequence slope and other cluster observables, such as X—ray luminosity, to investigate whether this will effect cluster detection methods which search for a colour-magnitude relation. In the final science chapter we present the details of our own cluster detection algorithm. This simple algorithm is based on finding clusters through the near-infrared and optical properties of the red sequence, drawing on our galaxy cluster evolution research. We describe the application of the algorithm to object catalogues from the UKIDSS DXS fields in order to find clusters at z ~ 1. To confirm the presence of the clusters we employ deep multi-object spectroscopy on the photometric members. The clusters found in this study are fed back into the high redshift regime of our galaxy evolution research

The moose, purine degradation, and environmental adaptation

It is accepted that allantoin is the end-product of purine degradation in mammals, except that uricase activity has been lost during the evolution of humans in which uric acid protects the brain from oxidative damage. However, we have found that the moose Alces americanus excretes extremely low urinary concentrations of allantoin and high concentrations of uric acid very similar to those of humans. Exposure to extreme cold is known to cause oxidative damage, and we suggest that the retention of uric acid by the moose represents an adaptation enabling the species to survive at high latitudes.Weiqi Zhang, Philip Stott, Minghai Zhan

Duplicate Testing Conducted On The Input Parameters For The Estimation Of Potential Expansiveness Of Clay

Conference: 16Th African Regional Conference on Soil Mechanics and Geotechnical Engineering, At unisia, Volume: Innovative Geotechnics for Africa - Bouassida, Khemakhem & Haffoudhi (Eds.) 2015This paper presents a study conducted on three active clay soils analysed at seven commercial laboratories in South Africa. Commercial test results are often used as input parameters for prediction models used to estimate potential heave expected from active clays, especially when designing foundations for light structures. This paper briefly looks at the typical results obtained from such laboratories and comments on the correlation achieved

Interpretation and application of carbon isotope ratios in freshwater diatom silica

Carbon incorporated into diatom frustule walls is protected from degradation enabling analysis for carbon isotope composition (δ13Cdiatom). This presents potential for tracing carbon cycles via a single photosynthetic host with well-constrained ecophysiology. Improved understanding of environmental processes controlling carbon delivery and assimilation is essential to interpret changes in freshwater δ13Cdiatom. Here relationships between water chemistry and δ13Cdiatom from contemporary regional data sets are investigated. Modern diatom and water samples were collected from river catchments within England and lake sediments from across Europe. The data suggest dissolved, biogenically produced carbon supplied proportionately to catchment productivity was critical in the rivers and soft water lakes. However, dissolved carbon from calcareous geology overwhelmed the carbon signature in hard water catchments. Both results demonstrate carbon source characteristics were the most important control on δ13Cdiatom, with a greater impact than productivity. Application of these principles was made to a sediment record from Lake Tanganyika. δ13Cdiatom co-varied with δ13Cbulk through the last glacial and Holocene. This suggests carbon supply was again dominant and exceeded authigenic demand. This first systematic evaluation of contemporary δ13Cdiatom controls demonstrates that diatoms have the potential to supply a record of carbon cycling through lake catchments from sediment records over millennial timescales

VIS3COS:III. nature and nurture in galaxy structure and morphology

We study the impact of local density and stellar mass on the morphology of ~500 quiescent (Q) and SFGs from the VIS3COS survey. We perform B/D decomposition of the SBPs and find ~41% of 10^10 Msun galaxies to be best fitted with 2 components. We complement our analysis with non-parametric measurements and qualitative visual classifications. We find that galaxy morphology depends on stellar mass and environment for our sample as a whole. We only find an impact of the environment on galaxy sizes for galaxies more massive than 10^11 Msun. We find higher n and B/T in high-density regions when compared to low-density counterparts at similar stellar masses. We also find that higher stellar mass galaxies have steeper light profiles compared to the lower ones. Using visual classifications, we find a morphology-density relation at z~0.84 for galaxies more massive than 10^10 Msun, with elliptical galaxies being dominant at high-density regions and disks more common in low-density regions. However, when splitting the sample into colour-colour selected SF and Q sub-populations, there are no statistically significant differences between low- and high-density regions. We find that Q galaxies are smaller, have higher n, and higher B/T when compared to SF counterparts. We confirm these trends with non-parametric quantities, finding Q galaxies to be smoother and having most of their light over smaller areas than SFGs. Overall, we find that the dependence of morphology on stellar mass is stronger than with local density and these relations are strongly correlated with the quenching fraction. The change in average morphology corresponds to a change in the relative fractions of blue disk-like galaxies and red elliptical galaxies with stellar mass and environment. We hypothesize that the processes responsible for the quenching of SF must also affect the galaxy morphology on similar timescales

The XMM Cluster Survey: The interplay between the brightest cluster galaxy and the intra-cluster medium via AGN feedback

Using a sample of 123 X-ray clusters and groups drawn from the XMM-Cluster Survey first data release, we investigate the interplay between the brightest cluster galaxy (BCG), its black hole, and the intra-cluster/group medium (ICM). It appears that for groups and clusters with a BCG likely to host significant AGN feedback, gas cooling dominates in those with Tx > 2 keV while AGN feedback dominates below. This may be understood through the sub-unity exponent found in the scaling relation we derive between the BCG mass and cluster mass over the halo mass range 10^13 < M500 < 10^15Msol and the lack of correlation between radio luminosity and cluster mass, such that BCG AGN in groups can have relatively more energetic influence on the ICM. The Lx - Tx relation for systems with the most massive BCGs, or those with BCGs co-located with the peak of the ICM emission, is steeper than that for those with the least massive and most offset, which instead follows self-similarity. This is evidence that a combination of central gas cooling and powerful, well fuelled AGN causes the departure of the ICM from pure gravitational heating, with the steepened relation crossing self-similarity at Tx = 2 keV. Importantly, regardless of their black hole mass, BCGs are more likely to host radio-loud AGN if they are in a massive cluster (Tx > 2 keV) and again co-located with an effective fuel supply of dense, cooling gas. This demonstrates that the most massive black holes appear to know more about their host cluster than they do about their host galaxy. The results lead us to propose a physically motivated, empirical definition of 'cluster' and 'group', delineated at 2 keV.Comment: Accepted for publication in MNRAS - replaced to match corrected proo

The XMM Cluster Survey: Evidence for energy injection at high redshift from evolution of the X-ray luminosity-temperature relation

We measure the evolution of the X-ray luminosity-temperature (L_X-T) relation since z~1.5 using a sample of 211 serendipitously detected galaxy clusters with spectroscopic redshifts drawn from the XMM Cluster Survey first data release (XCS-DR1). This is the first study spanning this redshift range using a single, large, homogeneous cluster sample. Using an orthogonal regression technique, we find no evidence for evolution in the slope or intrinsic scatter of the relation since z~1.5, finding both to be consistent with previous measurements at z~0.1. However, the normalisation is seen to evolve negatively with respect to the self-similar expectation: we find E(z)^{-1} L_X = 10^{44.67 +/- 0.09} (T/5)^{3.04 +/- 0.16} (1+z)^{-1.5 +/- 0.5}, which is within 2 sigma of the zero evolution case. We see milder, but still negative, evolution with respect to self-similar when using a bisector regression technique. We compare our results to numerical simulations, where we fit simulated cluster samples using the same methods used on the XCS data. Our data favour models in which the majority of the excess entropy required to explain the slope of the L_X-T relation is injected at high redshift. Simulations in which AGN feedback is implemented using prescriptions from current semi-analytic galaxy formation models predict positive evolution of the normalisation, and differ from our data at more than 5 sigma. This suggests that more efficient feedback at high redshift may be needed in these models.Comment: Accepted for publication in MNRAS; 12 pages, 6 figures; added references to match published versio