Shallow sea tidal friction and sediment transport

The dissertation addresses one aspect of the hydrodynamic and bottom topography interactions within a shallow sea. We investigate causes for the surprising lack of overall motion of the linear sand ridges that lie within the energetic wind-wave and tidal regime of the Southern Bight. There are many problems associated with the accurate estimation of ocean fluid velocity. However, it was found that this was the only significant parameter that could be collected and analysed with the accuracy required for a scientific investigation. No detailed measurements were taken of the sea-bed features or of the suspended and bed-load sediment concentrations. The particular linear sand ridge investigated was the South Falls bank. The tidal flow was measured using current meter rigs on and off the bank. Analytical and numerical modelling of the hydrodynamic equations was compared with these current meter values for the fluid velocity field. It was found that a simple two-dimensional model that agreed well with observations of fluid velocity implies that, locally the tidal friction is insensitive to change of depth. A Seasat synthetic aperture radar image of the Southern Bight showed grey-scale variation strongly related to the bottom topography, with increased brightness on the western flank of the sandbanks and sand waves of the region. A tidal surface velocity field was generated, for the time of the image, by reference to the measured velocities over the bank. It was estimated that the wave-current interaction, due to radiation stress effects, would have produced changes in the surface roughness over the bank that relate well to the image brightness variation. The flow over a rough strip of the sea-bed within a constant depth region or a core of relict beach material are each sufficient for bank generation. The relation of the present flow regime over South Falls bank to that of the flow over a rough strip suggests that the cross-sectional area of the central portion of the bank is stable. The South Falls cross-section shape may be a result of wave blocking rather than a westward sediment transport. Secondary flow acts to give a frictional bottom flow everywhere within the Southern Bight. This must change at the bank and may integrate to helical vortices

Through Thick and Thin: Kinematic and Chemical Components in the Solar Neighbourhood

We search for the existence of chemically-distinct stellar components in the solar neighbourhood using published data. Extending earlier work, we show that when the abundances of Fe, alpha elements, and the r-process element Eu are considered, stars separate neatly into two groups that delineate the traditional thin and thick disk of the Milky Way. The group akin to the thin disk is traced by stars with [Fe/H]>-0.7 and alpha/Fe<0.2. The thick disk-like group overlaps the thin disk in [Fe/H] but has higher abundances of alpha elements and Eu. Stars in the range -1.5<[Fe/H]<-0.7 with low [alpha/Fe] ratios, however, seem to belong to a separate, dynamically-cold, non-rotating component that we associate with tidal debris. The kinematically-hot stellar halo dominates the sample for [Fe/H]<-1.5. These results suggest that it may be possible to define the main dynamical components of the solar neighbourhood using only their chemistry, an approach with a number of interesting consequences. The kinematics of thin disk stars is then independent of metallicity: their average rotation speed remains roughly constant in the range -0.7<[Fe/H]<+0.4, a result that argues against radial migration having played a substantial role in the evolution of the thin disk. The velocity dispersion of stars assigned to the thin disk is also independent of [Fe/H], implying that the familiar increase in velocity dispersion with decreasing metallicity is the result of the increased prevalence of the thick disk at lower metallicities, rather than of the sustained operation of a dynamical heating mechanism. The substantial overlap in [Fe/H] and, probably, stellar age, of the various components might affect other reported trends in the properties of stars in the solar neighbourhood.Comment: 8 pages, 5 figures, some clarifications after referee report. Conclusions unchange

The early days of the Sculptor dwarf spheroidal galaxy

We present the high resolution spectroscopic study of five -3.9<=[Fe/H]<=-2.5 stars in the Local Group dwarf spheroidal, Sculptor, thereby doubling the number of stars with comparable observations in this metallicity range. We carry out a detailed analysis of the chemical abundances of alpha, iron peak, light and heavy elements, and draw comparisons with the Milky Way halo and the ultra faint dwarf stellar populations. We show that the bulk of the Sculptor metal-poor stars follows the same trends in abundance ratios versus metallicity as the Milky Way stars. This suggests similar early conditions of star formation and a high degree of homogeneity of the interstellar medium. We find an outlier to this main regime, which seems to miss the products of the most massive of the TypeII supernovae. In addition to its value to help refining galaxy formation models, this star provides clues to the production of cobalt and zinc. Two of our sample stars have low odd-to-even barium isotope abundance ratios, suggestive of a fair proportion of s-process; we discuss the implication for the nucleosynthetic origin of the neutron capture elements.Comment: Replacement after language editio

A physically based calving model applied to marine outlet glaciers and implications for the glacier dynamics

This is the published version, also available here: http://dx.doi.org/10.3189/002214310794457344.We present results from numerical ice-flow models that include calving criteria based on penetration of surface and basal crevasses, which in turn is a function of longitudinal strain rates near the glacier front. The position of the calving front is defined as the point where either (1) surface crevasses reach the waterline (model CDw), or (2) surface and basal crevasses penetrate the full thickness of the glacier (model CD). For comparison with previous studies, results are also presented for a height-above-buoyancy calving model. Qualitatively, both models CDw and CD produce similar behaviour. Unlike previous models for calving, the new calving criteria are applicable to both grounded termini and floating ice shelves and tongues. The numerical ice-flow model is applied to an idealized geometry characteristic of marine outlet glaciers. Results indicate that grounding-line dynamics are less sensitive to basal topography than previously suggested. Stable grounding-line positions can be obtained even on a reverse bed slope with or without floating termini. The proposed calving criteria also allow calving losses to be linked to surface melt and therefore climate. In contrast to previous studies in which calving rate or position of the terminus is linked to local water depth, the new calving criterion is able to produce seasonal cycles of retreat and advance as observed for Greenland marine outlet glaciers. The contrasting dynamical behaviour and stability found for different calving models suggests that a realistic parameterization for the process of calving is crucial for any predictions of marine outlet glacier change

The Evolution of Oxygen and Magnesium in the Bulge and Disk of the Milky Way

We show that the Galactic bulge and disk share a similar, strong, decline in [O/Mg] ratio with [Mg/H]. The similarity of the [O/Mg] trend in these two, markedly different, populations suggests a metallicity-dependent modulation of the stellar yields from massive stars, by mass loss from winds, and related to the Wolf-Rayet phenomenon, as proposed by McWilliam & Rich (2004). We have modified existing models for the chemical evolution of the Galactic bulge and the solar neighborhood with the inclusion of metallicity-dependent oxygen yields from theoretical predictions for massive stars that include mass loss by stellar winds. Our results significantly improve the agreement between predicted and observed [O/Mg] ratios in the bulge and disk above solar metallicity; however, a small zero-point normalization problem remains to be resolved. The zero-point shift indicates that either the semi-empirical yields of Francois et al. (2004) need adjustment, or that the bulge IMF is not quite as flat as found by Ballero et al. (2007); the former explanation is preferred. Our result removes a previous inconsistency between the interpretation of [O/Fe] and [Mg/Fe] ratios in the bulge, and confirms the conclusion that the bulge formed more rapidly than the disk, based on the over-abundances of elements produced by massive stars. We also provide an explanation for the long-standing difference between [Mg/Fe] and [O/Fe] trends among disk stars more metal-rich than the sun.Comment: 22 pages including 5 figures. Submitted to the Astronomical Journa