The wall effect is known to present difficulties when attempting to predict the pressure drop over randomly packed beds. The Nuclear Safety Standard Commission, “Kerntechnischer Auss-chuss" (KTA), made considerable efforts to develop an equation which predicts the pressure drop over cylindrical randomly packed beds consisting of mono-sized spheres. The KTA was able to estimate a limiting line, which defines the region for which the wall effect is negligible, however the theoretical basis for this line is unclear. The goal of this investigation was to determine the validity of the KTA limiting line, using an explicit approach. Packed beds were generated using Discrete Element Modelling (DEM), and the flow through the beds simulated using Computational Fluid Dynamics (CFD). STAR-CCM+R was used for both DEM and CFD operations, and the methods developed for this explicit approach were validated with empirical data. The KTA correlation predictions for friction factors were com- pared with the CFD results, as well as the predictions from a few other correlations. The KTA correlation predictions for friction factors did not correspond well with the CFD results at low aspect ratios and low modified Reynolds numbers, due to the influence of the wall effect. The KTA limiting line was found to be valid, but not exact. A new limiting line for the KTA correlation was suggested, however the new limiting line improved little on the existing line and was the result of some major assumptions. In order to improve the determination of the position of the KTA limiting line further, criteria need to be established which determine how small the error in predicted friction factor must be before the KTA correlation can be accepted as accurate. / MIng (Nuclear Engineering), North-West University, Potchefstroom Campus, 2014

We will consider the scenario of the co-rotation of a fluid star (in specific, a neutron star) and a black hole. The neutron star (or primary)is assumed to have constant angular velocity. The tidal effects on the primary are investigated. First, the centrally condensed approximation is applied, where both bodies are considered as point sources. In the second treatment, the primary is treated as an incompressible and homogeneous fluid mass, which in addition to its own gravity is subject to centrifugal and Coriolis forces, derived from fluid motions. The black hole (or secondary) is treated as a rigid sphere and can be regarded as a point mass. The equilibrium figure is derived. The problem is then adapted to include vorticity and a pseudo-Newtonian potential. The coalescence of neutron star - black hole binaries and their importance to gravitational wave detection is also discussed. / Mathematical Sciences / M. Sc. (Applied Mathematics)

In this dissertation, we present three complementary studies of the processes that drive planetary migration. The first is a radial-velocity survey in search of giant planets in adolescent (<1 >Gyr) open clusters. While several different mechanisms may act to drive giant planets inward, only some mechanisms will excite high eccentricities while doing so. Measuring the eccentricities of young hot Jupiters in these clusters (at a time before the orbits have had a chance to circularize due to tidal friction with their host stars) will allow us to identify which mechanisms are most important. Through this survey, we detect the first 3 hot Jupiters in open clusters (and at least 4 long-period planets), and we measure the occurrence rate of hot Jupiters in clusters to be similar to that of the field (~1%). We determine via analyses of hot Jupiter eccentricities and outer companions in these systems that high eccentricity migration mechanisms (those requiring the presence of a third body) are important for migration. The second project, an adaptive optics imaging survey for stellar companions to known hot Jupiter hosts, aims to determine the role that stellar companions in particular play in giant planet migration. Through a preliminary analysis, we derive a lower limit on the binary frequency of 45% (greater than that of the typical field star), and we find that the presence of a companion is correlated with misalignment of the spin-orbit angle of the planetary system, as would be expected for stellar Kozai-Lidov migration: at least 74% of misaligned systems reside in binaries. We thus conclude that among high eccentricity migration mechanisms, those requiring a stellar companion play a significant role. Finally, we describe simulations of measurements of the planet population expected to be discovered by TESS, and use these to demonstrate that a strong constraint on the obliquity distribution of small planets can be derived using only TESS photometry, Gaia astrometry, and vsin(i) measurements of the host stars. This obliquity distribution will be a key piece of evidence to help detemine the likely formation and migration histories of small planets, and can contribute to the assessment of the potential for Earth-like planets to harbor life.

In the last few decades, the emergence of large-scale infrared surveys has led to a revolution in the study of star formation. In particular, NASA’s Spitzer Space Telescope has recently carried out mid- and far-infrared observations of numerous star formation regions with unprecedented resolution and sensitivity, and has uncovered thousands of forming stars. In combination with present and future large-scale near-infrared and sub-mm surveys, spectral energy distributions from near-infrared to mm wavelengths will be available for these thousands of young stars. Never before has there been such a wealth of multi-wavelength data for so many young stars. Traditional techniques for studying the physical properties of young stars through their spectral energy distributions have usually focused either on the analysis of many sources using simple observational diagnostics such as colours or spectral indices, or on the analysis of a few sources through the detailed modelling of their full spectral energy distributions. The work presented in the first part of this thesis aims to bridge these two techniques through the efficient modelling of the spectral energy distributions of many young stars. In particular, the technique developed for this work makes it straightforward to find out how well different physical parameters are constrained, whether any parameters are degenerate, and whether additional data would resolve the degeneracies. In the second part of this thesis, a census of intrinsically red sources observed by Spitzer in the Galactic plane is presented, including a catalogue of over 11,000 likely young stellar objects. This sample of sources is the largest uniformly selected sample of young stars to date, and effectively provides a map of the sites of star formation in the mid-plane of the Milky-Way. In parallel, this census has uncovered over 7,000 candidate asymptotic giant branch stars, of which over 1,000 are variable at 4.5 or 8.0 microns.

This dissertation explores embodiments of citizenship in three historical pageants of 1913. As historical pageantry reached the height of its popularity in the early twentieth century, the form was criticized by those who felt it represented a limited understanding of community and citizenship. Historical pageants came to prominence at a time in the nation’s history when lynching plagued the south, women agitated for the right to vote, and labor unions organized to demand better working conditions. Popular historical pageants presented a history which ignored these pressing social issues and supported the status quo. As a result, while pageants gained popularity the form was taken up by groups seeking to use pageants for different political purposes. My dissertation interrogates embodiments of citizenship in Progressive Era pageantry through three case studies: W.E.B. Du Bois wrote and staged Star of Ethiopia, devoted to re-telling African-American history; John Reed organized members of the Industrial Workers of the World (IWW) for a performance of The Paterson Strike Pageant to aid laborers on strike; and Hazel MacKaye staged Allegory in support of women’s suffrage. While each pageant aimed to promote diversity, once each pageant’s historiography landed on live bodies, the gaps between what the pageant argued for and who the pageant simultaneously excluded were made visible. Allegory crafted an argument for white women’s suffrage by excluding recent immigrant and women of color; Du Bois sought to promote the African American middle class by denigrating the working classes; John Reed painted an image of the IWW as a fully united working class while ignoring the racial and ethnic differences that had led to tensions among the group. Despite their progressive intentions, once each pageant moved its political arguments on stage, the choices they made in performance belied their inclusive aspirations. / text

In this thesis, we construct a new hydrodynamical algorithm able of handling general compressible reactive flow problems, based on a finite-volume method inspired by the original MUSCL scheme of van Leer (1979). The algorithm is of second-order in the smooth part of the flow and avoids dimensional splitting. It uses MPI to achieve parallelism, and includes an astrophysical equation of state and a nuclear reaction network. It proves to be robust to tests cases. In particular it reproduces quite well the reactive and non-reactive results obtained with two different numerical methods (Fryxell & al. 1989, Busegnies & al. 2007). Moreover the time-dependent results are in agreement with the corresponding steady state solution. This gives us confidence in applying it to an astrophysical situation which has never been studied, the propagation of a detonation in conditions relevant to superbursts. The algorithm is described in (Noel & al. 2007). In a firt step we obtain the detonation profiles in pure carbon and in a mixture of carbon and iron. In both cases we underline the large difference between the total reaction length and the length on which some species burn. This difference leads to enormous numerical difficulties because all the length scales cannot be resolved at the same time in a single simulation. We show that the carbon detonation might be studied in a partial resolution approach like the one of Gamezo & al. (1999). In a second step we construct a new reduced nuclear reaction network able to reproduce the energy production due to the photo-disintegrations of heavy elements, like ruthenium, which are thought to occur during superbursts in mixed H/He accreting systems. Using this new nuclear network we simulate detonations in mixture of carbon and ruthenium. An interesting feature is that, in this case, all the reaction lengths can be resolved in the same simulation. This makes the C/Ru detonations easier to study in future multi-dimensional simulations than the pure carbon ones (Noel & al. 2007b). Finally we perform some numerical experiments which show that our algorithm is able to deal with initially inhomogeneous medium, and that the multi-dimensional simulations are attainable even if they are quite computational time consuming. - B. Van Leer, J. Comp. Phys., 21, 101, 1979 - Fryxell, B.A., Muller, E., and Arnett, W.D., Technical report MPA 449, 1989 - Busegnies, Y., Francois, J. and Paulus, G., Shock Waves, 11, 2007 - Gamezo, V.N., Wheeler, J.C., Khokhlov, A.M., and Oran, E.S., ApJ, 512, 827, 1999 - Noël, C., Busegnies, Y., Papalexandris, M.V. & al., A&A, 470, 653, 2007 - Noël, C., Goriely, S., Busegnies, Y. & Papalexandris, M.V., submitted to A&A, 2007b / Un algorithme parallèle basé sur une méthode aux volumes finis inspirée du schéma MUSCL de Van Leer (1979) a été construit. Il a été développé sur base de la méthode de Lappas & al. (1999) qui permet de résoudre simultanément toutes les dimensions spatiales. Cette méthode se base sur la construction de surfaces appropriées dans l'espace-temps, le long desquelles les équations de bilan se découplent en équations plus simples à intégrer. Cet algorithme est actuellement le seul à éviter le "splitting" des dimensions spatiales. Dans les modèles conventionnels (PPM, FCT, etc.), l'intégration spatiale des équations est réalisée de manière unidimensionnelle pour chaque direction. Un réseau de réactions nucléaires ainsi qu'une équation d'état astrophysique ont été inclus dans l'algorithme et celui-ci a ensuite été soumis à une grande variété de cas tests réactifs et non réactifs. Il a été comparé à d'autres codes généralement utilisés en astrophysique (Fryxell & al. 1989, Fryxell & al. 2000, Busegnies & al. 2007) et il reproduit correctement leurs résultats. L'algorithme est décrit dans Noël & al. (2007). Sur base de cet algorithme, les premières simulations de détonation dans des conditions thermodynamiques représentatives des Superbursts ont été réalisées. Différentes compositions du milieu ont été envisagées (carbone pur, mélange de carbone et de fer, mélange de carbone et de cendres du processus rp). Dans la plupart des systèmes où des Superbursts ont été observés, la matière accrétée est un mélange d'hydrogène et d'hélium. Dans ce cas, des phases de combustion précédant le Superburst produisent des nucléides plus lourd que le fer (Schatz & al. 2003). Ces nucléides peuvent être photodésintégrés durant le Superburst. Pour prendre en compte ces réactions endothermiques de photodésintégration, nous avons construit un nouveau réseau réduit de réactions nucléaires qui a été incorporé dans l'algorithme hydrodynamique (Noël & al. 2007b). Ce réseau réduit reproduit globalement l'énergétique d'un réseau complet et a permis de faire la première simulation numérique de détonation dans des conditions caractéristiques de systèmes accréteurs d'un mélange hydrogène-hélium. Finallement quelques simulations multidimensionelles préliminaires ont éte réalisées. - Busegnies, Y., Francois, J. and Paulus, G., Shock Waves, 11, 2007 - Fryxell, B.A., Muller, E., and Arnett, W.D., Technical report MPA 449, 1989 - Fryxell, B.A., Olson, K., Ricker, P. & al., ApJS, 131, 273, 2000 - Lappas, T., Leonard, A. and Dimotakis, P.E., SIAM J. Sci. Comput., 20, 1064, 1999 - Noël, C., Busegnies, Y., Papalexandris, M.V. & al., A&A, 470, 653, 2007 - Noël, C., Goriely, S., Busegnies, Y. & Papalexandris, M.V., submitted to A&A, 2007b - Röpke, F. K. PhD thesis, Technischen Universitat Munchen, 2003 - Schatz, H., Bildsten, L., Cumming, A. and Ouellette, M., Nuclear Physics A, 718, 247, 2003 - Van Leer, B. Comp. Phys., 21, 101, 1979 - Weinberg, N.N. and Bildsten, L., ArXiv e-prints, 0706.3062, 2007

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Determining the cosmic star formation history of the Universe is fundamental for our understanding of galaxy formation and evolution. While surveys now suggest that the "epoch" of galaxy formation occurred more than 6 billion years ago, our measurements still suff er from signi ficant scatter and uncertainties due to the use of diff erent indicators, dust extinction and the e ffects of cosmic variance in the current samples. Furthermore, understanding galaxy formation and evolution require us to go much beyond simply determining the star formation history of the Universe with high accuracy: what are the physical mechanisms driving the strong evolution that we observe? How does star formation depend on stellar mass and environment and how does that change with cosmic time? This thesis presents both a completely self-consistent determination of the star formation history of the Universe (based on a single, sensitive and well-calibrated star formation indicator up to redshift z ~ 2:3: the H α luminosity) and investigates its drivers by exploring large area surveys (probing a range of environments and overcoming cosmic variance) obtained with the High-redshift Emission Line Survey (HiZELS). HiZELS is a panoramic extragalactic survey using the WFCAM instrument on the 3.8-m UK Infrared Telescope (UKIRT) which utilizes a set of existing and custom-made narrow-band filters in the J, H and K bands to detect emission line galaxies (main targets are H α emitters at z = 0:84, z = 1:47 and z = 2:23) up to z ~ 9 over square degree areas of extragalactic sky. Detailed measurements of the H α luminosity function and its evolution with redshift are presented, revealing a signi ficant luminosity evolution. The clustering properties of H α emitters at high-redshift are quantifi ed and investigated for the first time, revealing that these distant galaxies reside in Milky-Way type dark matter haloes at z ~ 1. Mass and environment are found to have important and inter-dependent roles on star formation at high-z and the results are able to reconcile previously contradictory results in the literature. Furthermore, by conducting a novel double-narrow band survey at z = 1:47, the relationship between the [Oii]3727 and H α emission lines is studied in detail and directly compared to z ~ 0, showing no signifi cant evolution in the dust properties of star-forming galaxies, despite the very strong luminosity evolution. Finally, this thesis also presents the widest search for very distant Ly α emitters at z ~ 9.

A unique K-band selected high-redshift spectroscopic dataset (UDSz) is exploited to gain further understanding of galaxy evolution at z > 1. Acquired as part of an ESO Large Programme, this thesis presents the reduction and analysis of a sample of ∼ 450 deep optical spectra of a random 1 in 6 sample of the KAB < 23, z > 1 galaxy population. Based on the final reduced dataset, spectrophotometric modelling of the optical spectra and multi-wavelength photometry available for each galaxy is performed using a combination of single and dual component stellar population models. The stellarmass and age estimates provided by the spectrophotometric modelling are exploited throughout the rest of the thesis to investigate the evolution of massive galaxies at z > 1. Focusing on a K-band bright (K < 21.5) sub-sample in the redshift range 1.3 < z < 1.5 the galaxy size-mass relation has been studied in detailed. In agreement with some previous studies it is found that massive, old, early-type galaxies (ETGs) have characteristic radii a factor ~- 1.5 − 3.0 smaller than their local counterparts at a given stellar-mass. Due to the potential errors in spectrophotometric estimates of the stellarmasses at high redshift velocity dispersion measurements are derived for a sub-sample of massive ETGs at z > 1.3 in order to calculate dynamical mass estimates. To date, only a handful of objects at z > 1.3 have individual velocity dispersion estimates in the literature. Here the largest single sample (13 objects) of velocity dispersion measurements at high redshift is presented. The results for the sub-sample of objects with dynamical mass estimates confirm the results based on stellar mass estimates that high redshift massive systems are more compact than their local counterparts. The fraction of K-band bright objects at high redshift that are passively evolving is calculated with specific star-formation rates from the UV rest-frame continuum, [OII] emission and 24μm data. It is concluded that ∼ 58 ± 10% of the K < 21.5, 1.3 < z < 1.5 galaxy population is passively evolving. Various photometric techniques for separating star-forming and passively evolving galaxies are assessed by exploiting the accurate spectral types derived for the UDSz spectroscopic sample. Popular highredshift selection techniques are shown to fail to effectively select complete samples of passive objects with low levels of contamination. Using detailed information available for the UDSz dataset, various techniques are optimised and then used to estimate the passive fraction from the full UDS photometric catalog. The passive fraction results from the full photometric catalog are found to agree well with the results derived from the UDSz sample. With the Visible and Infrared Survey Telescope for Astronomy (VISTA) now starting to produce data, the opportunity has been taken to develop high-redshift galaxy population dividers based on the VISTA filters. Using the first data release from the VISTA Deep Extragalactic Observations (VIDEO) survey (VVDS D1 field), the passive fractions of K-band limited samples have been estimated to compare with results derived in the UDS. Within the errors the passive fraction estimates in the UDS and VISTA VVDS D1 field are found to agree reasonably well. Finally, composite spectra are used to study the evolution of various different galaxy sub-samples as a function of redshift, age, stellar-mass and specific star-formation rate. This work produces an remarkably clean result, showing that the massive, absolute Kband bright, passively evolving ETGs are always the oldest population, with ages close to the age of the Universe at z ∼ 1.4. In contrast, the late-type, low-mass, star-forming galaxies are always found to be much younger systems. This result strongly supports the downsizing scenario, in which more massive systems complete their stellar-mass assembly before lower-mass counterparts.

This investigation undertakes to re-centre the figure of the film star and their film appearances in the field of star study. To this end it uses Charlton Heston as its focus in a re-appraisal of existing methods of accounting for the star phenomenon in cinema. It also concomitantly re-assesses existing accounts of the significance of Charlton Heston as a film star. This thesis posits a robust method for identifying the specificities of the star’s contribution to a film’s meanings and effects across the body of their work by drawing on Andrew Britton’s understanding of the ‘star enactment’. Present approaches through which to engage with the details of a star’s performance are considered in detail and the weaknesses of those that seek to impose external schemas onto such discussions are highlighted. The difficulties with approaches that attempt to account for the star as a signifying phenomenon through the concepts of acting and performance are also considered. Existing methods which may allow for a fruitful investigation into the significance of the star enactment, such as the commutation test, are re- formulated in this study and their benefits are demonstrated through their application to key Heston star enactments. These new understandings are also made possible through the application of an ‘ekphrastic’ method of rendering film moments. Previous readings of Heston’s star figure are also re- appraised, and their conclusions questioned, through closer reference to the evidence of details from films. The fruitfulness of this method for analysing and commenting on film is thus demonstrated and Heston’s relationship to genre and its effect on performance style is also considered in order to be able to confidently assert the specific features of the Heston aesthetic.