The Wax Lake Delta (WLD) is a sandy, modern river delta prograding rapidly into Atchafalaya Bay. This dissertation uses field data to improve the understanding of channel kinematics that dictate river delta geometry and stratigraphy, while providing a framework for coastal restoration efforts. The studies presented here show that the distributary channel network of the WLD is erosional. In the first study, analyses of the feeder channel to the WLD and the channel network within the sub-aerially emergent delta show that the channel bed has incised into the consolidated muds that act as bedrock. The large (>62%) fraction of bedrock exposure found in multi-beam surveys is related to the under-saturation of suspended sand measured during the flood of 2009. The second study concerns the delta front beyond the emergent delta Distributary channels extend 2 – 6 km into the delta front. Four bathymetric surveys of one bifurcating distributary channel – Gadwall Pass – show that the majority of bed aggradation occurs during floods, but the majority of channel extension of each bifurcate channel occurs during low river discharge. In the third study, field measurements of fluid flow during a tidal cycle indicate that tidal augmentation of during periods of low river discharge is responsible for channel extension during low river discharges. Flow direction measured from streaklines present in aerial photomosaics is combined with bathymetric evolution data to quantify spatial velocity changes on the delta front. These data show that flow spreading is insufficient to prevent acceleration at channel margins, providing an explanation for observed erosion. Flow divergence is limited on the delta front by the proximity of neighboring channels, even though they are separated by 10-30 channel widths. The associated convergence of flow in inter-distributary bays occurs along “drainage troughs”. These channel-forms collect flow that has been dispensed from distributary channel network. Finally, ambient currents in Atchafalaya Bay (0.06 – 0.2 m/s) caused by tides and the proximity to the neighboring Atchafalaya Delta appear to alter flow patterns on the delta foreset, and are responsible for channel curvature on the delta front. / text

Produkte im Maschinenbau gewinnen durch immer weitreichendere Kundenanforderungen zunehmend an Komplexität. Davon angetrieben, werden auch die eingesetzten Softwarewerkzeuge kontinuierlich weiterentwickelt.CAD-Systeme werden beispielsweise heutzutage nicht mehr ausschließlich zur Konstruktion verwendet, sondern beinhalten meist auch weiterführende Module bspw.zur Simulation physikalischer Effekte (CAE) bis hin zur Arbeitsplanung (CAP) und werden in ganzen Softwaresuiten angeboten. Im vergangenen Jahrzehnt sind außerdem Mechanismus- und Bewegungsanalysen fester Bestandteil von CAD-Systemen geworden. Zusatzinformationen, wie bspw. Kinematikbeziehungen und / oder Animationen, die zur Verifikation der Funktionalität und Kollisionsfreiheit unabdingbar sind, können direkt in den CAD-Programen erstellt und überprüft werden. Die aktive Nutzung und Zugänglichkeit dieser CAD-Konstruktionssysteme durch konstruktionsferne Nutzergruppen ist nur bedingt durch so genannte Model-Viewer gegeben, wodurch bspw. die Fehlerbewertung (z.B. Design Review, FMEA) außerhalb der Entwicklungsabteilungen erschwert wird. Abhilfe bietet hier die Nutzung von High-EndTechniken, wie die immersive Darstellung mittels Virtual Reality (VR)-Technologie, im Prozess der Konstruktionsbewertung/Design Review. Dafür arbeiten wir mit der Chemnitzer Firma ARCsolutions GmbH an einer Lösung wie ein (teil-)automatisiert reduziertes Modell, unter Erhaltung im CAD definierter Animationen und Kinematischen Beziehungen automatisiert in die VR gebracht und dort genutzt werden kann.

I have used blue near-infrared colours to select a group of UKIDSS T dwarfs with spectral types later than T4. From amongst these I identify two kinematic halo T-dwarf candi- dates. Blue near-infrared colours have been attributed to collisionally-induced hydrogen absorption, which is enhanced by either high surface gravity or low metallicity. Proper motions are measured and distances estimated, allowing the determination of tangential velocities. U and V components are estimated for our objects by assuming Vrad = 0. From this, ULAS J0926+0835 is found to have U = 62 kms−1 and V = −140 kms−1 and ULAS J1319+1209 is found to have U = 192 kms−1 and V = −92 kms−1. These values are consistent with potential halo membership. However, surprisingly, these are not the bluest objects in the selection. The bluest is ULAS J1233+1219, with J −K = −1.16±0.07, and surprisingly this object is found to have thin disc-like U and V . Our sample also contains Hip 73786B, which I find to be a companion to the star Hip 73786. Hip 73786 is a metal- poor star, with [Fe/H]= −0.3 ± 0.1 and is located at a distance of 19±0.7 pc. U, V,W space velocity components are calculated for Hip 73786A and B, finding that U = −48±7 kms−1, V = −75 ± 4 kms−1 and W = −44 ± 8 kms−1. From the properties of the pri- mary, Hip 73786B is found to be at least 1.6Gyr old. As a metal poor object, Hip 73786B represents an important addition to the sample of known T dwarf benchmarks. Using mid-infrared data from WISE, I also identify T dwarfs with abnormally-red H − W2 and consider possible causes for their extreme colours. In particular I exam- ine three prominent examples of this phenomenon, ULAS J1416+1348B, 2MASS J0939- 2448 and BD+01o 2920B. A plot of spectral type against MW2-magnitude suggests that ULAS J1416+1348B is potentially an unresolved binary, similar to 2MASS J0939-2448. However, the plot also indicates that BD+01o 2920B is not an unresolved binary. I also present new FIRE spectroscopy for ULAS J1416+1348B and 2MASS J0939-2448. These data show that ULAS J1416+1348B has a similar shape to the Y -band spectrum to that of BD+01o 2920B, thus suggesting that the two objects have a similar metallicity, whereas 2MASS J0939-2448 appears to be a more metal-rich object. Using a new parallactic dis- tance, I derive a luminosity of (6.9±0.7)×1020W for ULAS J1416+1348B. I also find a radial velocity of −39 ± 1 kms−1 for this object. The agreement between this and that of the L dwarf SDSS J1416+1348A confirms that these two objects are physically-associated. I also present a set of simulated unresolved binaries; the colours of these systems do not appear to redden significantly with the addition of cooler companions. From this, I suggest that the colours of ULAS J1416+1348B and BD+01o 2920B cannot be solely attributed to any possible unresolved companions; for these two objects, composition and/or surface gravity must be playing a substantial role. Consideration of model predictions provides extra evidence for this argument, showing as it does that high log g and low metallicity can redden H − W2 colours by as much as »0.5mag as compared to a high-metallicity and low log g object of the same effective temperature. I also present kinematics and photometry for several more new candidate low-metallicity T dwarfs. Spectra are also presented, where available. In addition I provide new follow-up JHK spectroscopy for ULAS J0926+0835, ULAS J1233+1219 and ULAS J1319+1209. These new spectra allow full JHK-based spectral typing for these objects.

Star formation in the Milky Way is confined to star-forming regions (OB association, HII regions, and open clusters) in the Galactic plane. It is usually assumed that these regions are found preferably along spiral arms, as is observed in other spiral galaxies. However, young early-type stars are often found at high Galactic latitudes, far away from their birthplaces in the Galactic disc. These stars are called runaway stars, and it is believed that they were ejected from their birth- places early in their lifetimes by one of two mechanisms: ejection from a binary system following the destruction of the massive companion in a supernova type II event (the binary ejection mechanism), or ejection from a dense cluster following a close gravitational encounter between two close binaries (the dynamical ejection mechanism). The aims of our study were: to improve the current understanding of the nature of high Galactic latitude runaway stars, in particular by investigating whether the theoretical ejection mechanisms could explain the more extreme cases; to show the feasibility of using high Galactic latitude stars as tracers of the spiral arms. The main technique used in this investigation was the tracing of stellar orbits back in time, given their present positions and velocities in 3D space. This technique allowed the determination of the ejection velocities, flight times and birthplaces of a sample of runaway stars. In order to obtain reasonable velocity estimates several recent catalogues of proper motion data were used. We found that the evolutionary ages of the vast majority of runaway stars is consistent with the disc ejection scenario. However, we identified three outliers which would need flight times much larger then their estimated ages in order to reach their present positions in the sky. Moreover, the ejection velocity distribution appears to be bimodal, showing evidence for two populations of runaway stars: a “low” velocity population (89 per cent of the sample), with a maximum ejection velocity of about 300 kms−1, and a “high” velocity population, with ejection velo- cities of 400 – 500 kms−1. We argue that the observed bimodality and maximum ejection velocity of 500 kms−1 can be interpreted as a natural consequence of a variation of the binary ejection mechanism. A possible connection between the “high” velocity population and the so-called hypervelocity stars is also explored, resulting in the conclusion that some stars previously identified as hypervelocity may be in fact runaway stars. The feasibility of using stars as tracers of the spiral arms was tested on a local sample, in order to obtain better quality data and larger numbers. We found that the spiral arms pattern speeds estimated from this sample (24.9±5.2 kms−1 kpc−1) and from a selected sample of runaways (22.8 ± 7.8 kms−1 kpc−1) are consistent within the errors and also consistent with other published estimates. We concluded that our estimates combined with the ones obtained in other studies suggest a value in the range 20 − 25 kms−1 kpc−1 for the pattern speed. Moreover, we concluded that an adequate representation of the spiral arms is obtained given the former pattern speed estimate, even when applied to the sample of runaway stars.

Aims: The aim of this study was to investigate Core Stability Exercise (CSE) induced changes in trunk sagittal acceleration as a measure of performance in participants following an acute onset of non-specific low back pain (LBP). Methodology: A Lumbar Motion Monitor (LMM) was used to measure trunk sagittal acceleration. The LMM was demonstrated to be reliable [Intra-Class Correlation (ICC) for average sagittal acceleration (0.96, 95% CI 0.90-0.98) and peak sagittal acceleration (0.89, 95% CI 0.75-0.96) with a 95% limit of agreement for the repeated measure of between -100.64 and +59.84 Deg/s2 ]. Pain was measured using the Visual Analogue Scale (VAS) and disability was measured with the Roland Morris Disability Questionnaire (RMDQ). Results: Differences in mean trunk sagittal acceleration between control and experimental groups at time points were assessed using a regression analysis (ratio of geometric means [95%CI]) and demonstrated to be not statistically significant (3 weeks (20%) 1.2 [0.9 to 1.6], p=0.2; 6 weeks (10%) 1.1 [0.8 to 1.5], p=0.7; 3 months (20%) 1.2 [0.8 to 1.9], p=0.9). Similarly, differences in mean pain score (3 weeks (30%) 1.3 [0.8-2.2], p= 0.3); 6 weeks (20%) 1.2 [0.7-2.0], p=0.6; 3 months (0%) 1.0 [0.5-1.9], p=1.0) and difference in mean disability score (6 weeks (0%) 1.0 [0.7-1.5], p= 1.0, 3 months (30%) 1.3 [0.8-1.9], p= 0.3) between groups were also not statistically significant. Conclusions: This work does not infer that CSE are definitively effective in reducing pain, improving subjective disability and improving trunk performance after an onset acute of non-specific LBP. However, there is a suggestion of clinical importance and a possible mechanism by which they may work. Further investigation into this mechanism may provide future effective management strategies for intervention of acute non-specific low back pain with optimistic cost implications for healthcare delivery in general and Physiotherapy in particular.

Male crickets produce a species specific song to attract females which in response move towards the sound source. This behaviour, termed phonotaxis, has been the subject of many morphological, neurophysiological and behavioural studies making it one of the most well studied examples of acoustic communication in the animal kingdom. Despite this fact, the precise leg movements during this behaviour is unknown. This is of specific interest as the cricket’s ears are located on their front legs, meaning that the perception of the sound input might change as the insect moves. This dissertation describes a methodology and an analysis that fills this knowledge gap. I developed a semi-automated tracking system for insect motion based on commercially available high-speed video cameras and freely available software. I used it to collect detailed three dimensional kinematic information from female crickets performing free walking phonotaxis towards a calling song stimulus. I marked the insect’s joints with small dots of paint and recorded the movements from underneath with a pair of cameras following the insect as it walks on the transparent floor of an arena. Tracking is done offline, utilizing a kinematic model to constrain the processing. I obtained, for the first time, the positions and angles of all joints of all legs and six additional body joints, synchronised with stance-swing transitions and the sound pattern, at a 300 Hz frame rate. I then analysed this data based on four categories: The single leg motion analysis revealed the importance of the thoraco-coxal (ThC) and body joints in the movement of the insect. Furthermore the inside middle leg’s tibio-tarsal (TiTa) joint was the centre of the rotation during turning. Certain joints appear to be the most crucial ones for the transition from straight walking to turning. The leg coordination analysis revealed the patterns followed during straight walking and turning. Furthermore, some leg combinations cannot be explained by current coordination rules. The angles relative to the active speaker revealed the deviation of the crickets as they followed a meandering course towards it. The estimation of ears’ input revealed the differences between the two sides as the insect performed phonotaxis by using a simple algorithm. In general, the results reveal both similarities and differences with other cricket studies and other insects such as cockroaches and stick insects. The work presented herein advances the current knowledge on cricket phonotactic behaviour and will be used in the further development of models of neural control of phonotaxis.

We conducted a large spectroscopic survey of 336 red giants in the direction of the Leo II dwarf galaxy using Hectochelle on the Multiple Mirror Telescope, and we conclude that 175 of them are members based on their radial velocities and surface gravities. Of this set, 40 stars have never before been observed spectroscopically. The systemic velocity of the dwarf is 78.3 +/- 0.6 km s(-1) with a velocity dispersion of 7.4 +/- 0.4 km s(-1). We identify one star beyond the tidal radius of Leo II but find no signatures of uniform rotation, kinematic asymmetries, or streams. The stars show a strong metallicity gradient of -1.53 +/- 0.10 dex kpc(-1) and have a mean metallicity of -1.70 +/- 0.02 dex. There is also evidence of two different chemodynamic populations, but the signal is weak. A larger sample of stars would be necessary to verify this feature.

De nos jours la culbute est la technique de virage crawl unanimement employée par les nageurs de compétition. Elle se décompose en cinq phases principales : l’approche, le retournement, le contact avec le mur (composé du placement et de la poussée), la phase sous-marine (composée de la glisse et de la coulée) et la reprise de nage. Dans le cadre d’une première collaboration entre le Laboratoire de Mécanique Physique de Bordeaux et le service recherche de la Fédération Française de Natation, cette étude s’est appuyée sur un protocole complet d’analyse sous-marine 3D qui a permis d’évaluer l’ensemble des paramètres cinématiques et dynamiques de la performance. Une double analyse comparative a montré que le niveau d’expertise et le genre ont un effet sur la performance au virage. Les nageuses de niveaux différents se différencient entre-elles par des vitesses en approche et en fin de poussée plus élevées pour les expertes qui adoptent une position plus profilée tout au long du contact. À haut niveau, les nageurs se différencient des nageuses au début du retournement par une vitesse plus élevée puis lors de la poussée où ils produisent un pic de force horizontale plus élevé et obtiennent un gain de vitesse en conséquence.L’utilisation de la méthode Lasso a permis d’établir deux modèles experts de la performance au virage. Chez les nageuses expertes, le modèle a révélé l’importance de l’impulsion latérale pendant le placement, paramètre nouveau qui pourrait être représentatif de la vrille exécutée. Chez les nageurs experts, les meilleurs virages sont réalisés par anticipation du retournement. Le mur est impacté dans une position corporelle peu fléchie ce qui favorise une extension rapide mais crée peu de vitesse. Le trajet parcouru par les meilleurs est court et optimisé. Cette étude illustre l’intérêt d’une analyse 3D du virage culbute crawl : en dynamique d’une part, l’utilisation d’une plateforme de force 3D permettant de distinguer les phases de placement et de poussée et probablement aussi le mouvement de vrille ; en cinématique d’autre part, avec l’importance de la trajectoire parcourue sur la performance au virage des nageurs experts. Par delà cette étude du virage, la conception, la réalisation et l’utilisation de nouveaux outils dédiés à l’analyse du mouvement en natation permet aujourd’hui de proposer au sportif une aide à la performance en phase avec ses objectifs. De part un enrichissement de la connaissance des différentes techniques utilisées par les experts et les non-experts, cette étude devrait également permettre d’améliorer l’enseignement des virages de haut-niveau. / Nowadays the tumble turn is the turn technique embraced by all freestyle competitive swimmers. It consists of five main phases: the approach, the rotation, the wall contact (with braking and push-off sub phases), the underwater phase (with glide and underwater propulsion sub phases), and the resumption of swimming.Within the first collaboration between the Laboratoire de Mécanique Physique of Bordeaux and the research department of the Fédération Française de Natation, this study relied on a comprehensive protocol for 3D underwater analysis that allowed assessing all kinematic and dynamic variables of performance.A double comparative analysis showed that both the level of expertise and the gender have effects on the turn performance. Female swimmers of various levels differ by higher approach and push-off speeds for the experts who are more streamlined throughout the contact. At a high level, male swimmers differ from female swimmers first by higher speed at the beginning of the rotation and also by producing more horizontal force at the push-off peak, directly resulting in a higher speed.The use of the Lasso method made it possible to establish two models for the expert turn performance. For female swimmers, the model revealed the role of lateral momentum during the braking phase, a new parameter that could be representative of the twist executed. For male swimmers, the best turns are swum when the rotation is anticipated. The wall is reached with a slightly flexed posture that results in a fast extension but also creates a slow speed. The best swimmers’ trajectories are short and optimized.This study showed the importance of a 3D analysis of the crawl tumble turn: on one hand the dynamic analysis, with the use of a 3D force platform that makes easier the distinction between the braking and the push-off phases, and probably also gives insights into the twist movement; on the other hand the kinematic analysis, with the importance of the length of the swum path on the turn performance.Beyond this study of the turn, the design, the implementation and the use of new tools devoted to motion analysis in swimming can now offer athletes assistance in line with their objectives. By increasing the knowledge of different techniques used by experts and non-experts swimmers, this study should also improve the teaching of high-performance turns.

We present a chemodynamical analysis of the Leo V dwarf galaxy, based on the Keck II DEIMOS spectra of eight member stars. We find a systemic velocity for the system of nu(r) = 170.9(+2.1) (-1.9) km s(-1) and barely resolve a velocity dispersion for the system, with sigma nu(r) = 2.3(+3.2) (-1.6) km s(-1), consistent with previous studies of Leo V. The poorly resolved dispersion means we are unable to adequately constrain the dark-matter content of Leo V. We find an average metallicity for the dwarf of [ Fe/ H] =-2.48 +/- 0.21 and measure a significant spread in the iron abundance of its member stars, with -3.1 <= [ Fe/ H] <=-1.9 dex, which clearly identifies Leo V as a dwarf galaxy that has been able to self-enrich its stellar population through extended star formation. Owing to the tentative photometric evidence for the tidal substructure around Leo V, we also investigate whether there is any evidence for tidal stripping or shocking of the system within its dynamics. We measure a significant velocity gradient across the system, of dv d chi = -4.1(+2.8) (-2.6) km s(-1) arcmin(-1) ( or d nu/d chi=-71.9(vertical bar 50.8) (-45.6) km s(-1) kpc(-1)), which points almost directly towards the Galactic Centre. We argue that Leo V is likely a dwarf on the brink of dissolution, having just barely survived a past encounter with the centre of the Milky Way.

We present results from MMT/Hectochelle spectroscopy of 390 red giant candidate stars along the line of sight to the recently discovered Galactic satellite Crater 2. Modeling the joint distribution of stellar positions, velocities, and metallicities as a mixture of Crater 2 and Galactic foreground populations, we identify similar to 62 members of Crater 2, for which we resolve a line-of-sight velocity dispersion of sigma(nu los) = 2.7(-0.3)(+0.3) km s(-1) and a. mean velocity of <nu(los)> = 87.5(-0.4)(+0.4) km s(-1) (solar rest frame). We also resolve a metallicity dispersion of sigma([Fe/H]) = 0.22(-0.03)(+0.04) dex and a mean of <[Fe/H]> = 1.98(-0.1)(+0.1) dex that is 0.28 +/- 0.14 dex poorer than estimated from photometry. Despite Crater 2's relatively large size (projected halflight radius R-h similar to 1 kpc) and intermediate luminosity (M-V similar to -8), its velocity dispersion is the coldest that has been resolved for any dwarf galaxy. These properties make Crater 2 the most extreme low-density outlier in dynamical as well as structural scaling relations among the Milky Way's dwarf spheroidals. Even so, under assumptions of dynamical equilibrium and negligible contamination by unresolved binary stars, the observed velocity distribution implies a gravitationally dominant dark matter halo, with a dynamical mass of. 4.4(-0.9)(+1.2) x 10(6) M-circle dot and a mass-to-light ratio of 53(-11)(+15) M-circle dot/L-V,L-circle dot enclosed within a radius of similar to 1 kpc, where the equivalent circular velocity is 4.3(-0.5)(+0.5) km s(-1).