Investigating the potential magnetic origin of wind variability in OB stars

In this thesis, the origin of large-scale structures in hot star winds, believed to be responsible for the presence of discrete absorption components (DACs) in the absorption troughs of ultraviolet resonance lines, is constrained using both observations and numerical simulations. These structures are understood as arising from bright regions on the stellar surface, although their physical cause remains unknown. First, we use high quality circular spectropolarimetric observations of 13 well-studied OB stars to evaluate the potential role of dipolar magnetic fields in producing DACs. We perform longitudinal field measurements and place limits on the field strength using Bayesian inference, assuming that it is dipolar. No magnetic field was detected within this sample. The derived constraints statistically refute any significant dynamical influence from a magnetic dipole on the wind for all of these stars, ruling out such fields as a cause for DACs. Second, we perform numerical simulations using bright spots constrained by broadband optical photometric observations. We calculate hydrodynamical wind models using three sets of spot sizes and strengths. Co-rotating interaction regions are yielded in each model, and radiative transfer shows that the properties of the variations in the UV resonance lines synthesized from these models are consistent with those found in observed UV spectra, establishing the first consistent link between UV spectroscopic line profile variability and photometric variations and thus supporting the bright spot paradigm (BSP). Finally, we develop and apply a phenomenological model to quantify the measurable effects co-rotating bright spots would have on broadband optical photometry and on the profiles of photopheric lines in optical spectra. This model can be used to evaluate the existence of these spots, and, in the event of their detection, characterize them. Furthermore, a tentative spot evolution model is presented. A preliminary analysis of its output, compared to the observed photometric variations of xi Persei, suggests the possible existence of “active longitudes” on the surface of this star. Future work will expand the range of observational diagnostics that can be interpreted within the BSP, and link phenomenology (bright spots) to physical processes (magnetic spots or non-radial pulsations).

Testing quasar unification: radiative transfer in clumpy winds

Various unification schemes interpret the complex phenomenology of quasars and luminous active galactic nuclei (AGN) in terms of a simple picture involving a central black hole, an accretion disc and an associated outflow. Here, we continue our tests of this paradigm by comparing quasar spectra to synthetic spectra of biconical disc wind models, produced with our state-of-the-art Monte Carlo radiative transfer code. Previously, we have shown that we could produce synthetic spectra resembling those of observed broad absorption line (BAL) quasars, but only if the X-ray luminosity was limited to 1043 erg s-1. Here, we introduce a simple treatment of clumping, and find that a filling factor of ˜0.01 moderates the ionization state sufficiently for BAL features to form in the rest-frame UV at more realistic X-ray luminosities. Our fiducial model shows good agreement with AGN X-ray properties and the wind produces strong line emission in, e.g., Lyα and C IV 1550 Å at low inclinations. At high inclinations, the spectra possess prominent LoBAL features. Despite these successes, we cannot reproduce all emission lines seen in quasar spectra with the correct equivalent-width ratios, and we find an angular dependence of emission line equivalent width despite the similarities in the observed emission line properties of BAL and non-BAL quasars. Overall, our work suggests that biconical winds can reproduce much of the qualitative behaviour expected from a unified model, but we cannot yet provide quantitative matches with quasar properties at all viewing angles. Whether disc winds can successfully unify quasars is therefore still an open question.

The VLT-FLAMES Tarantula Survey XXI. Stellar spin rates of O-type spectroscopic binaries

Context: The initial distribution of spin rates of massive stars is a fingerprint of their elusive formation process. It also sets a key initial condition for stellar evolution and is thus an important ingredient in stellar population synthesis. So far, most studies have focused on single stars. Most O stars are, however, found in multiple systems. 

Aims: By establishing the spin-rate distribution of a sizeable sample of O-type spectroscopic binaries and by comparing the distributions of binary subpopulations with one another and with that of presumed-single stars in the same region, we aim to constrain the initial spin distribution of O stars in binaries, and to identify signatures of the physical mechanisms that affect the evolution of the spin rates of massive stars. 

Methods: We use ground-based optical spectroscopy obtained in the framework of the VLT-FLAMES Tarantula Survey (VFTS) to establish the projected equatorial rotational velocities (ν_esini) for components of 114 spectroscopic binaries in 30 Doradus. The ν_esini values are derived from the full width at half maximum (FWHM) of a set of spectral lines, using a FWHM vs. ν_esini calibration that we derive based on previous line analysis methods applied to single O-type stars in the VFTS sample. 

Results: The overall ν_esini distribution of the primary stars resembles that of single O-type stars in the VFTS, featuring a low-velocity peak (at ν_esini<200 kms^-1) and a shoulder at intermediate velocities (200 <ν_esini<300 kms^-1). The distributions of binaries and single stars, however, differ in two ways. First, the main peak at ν_esini ~ 100kms^-1 is broader and slightly shifted towards higher spin rates in the binary distribution than that of the presumed-single stars. This shift is mostly due to short-period binaries (P_orb~<10 d). Second, the ν_esini distribution of primaries lacks a significant population of stars spinning faster than 300 kms^-1, while such a population is clearly present in the single-star sample. The ν_esini distribution of binaries with amplitudes of radial velocity variation in the range of 20 to 200 kms^-1 (mostly binaries with P_orb ~ 10-1000 d and/or with q<0.5) is similar to that of single O stars below ν_esini_~<170kms^-1. 

Conclusions: Our results are compatible with the assumption that binary components formed with the same spin distribution as single stars, and that this distribution contains few or no fast-spinning stars. The higher average spin rate of stars in short-period binaries may either be explained by spin-up through tides in such tight binary systems, or by spin-down of a fraction of the presumed-single stars and long-period binaries through magnetic braking (or by a combination of both mechanisms). Most primaries and secondaries of SB2 systems with P_orb~<10 d appear to have similar rotational velocities. This is in agreement with tidal locking in close binaries where the components have similar radii. The lack of very rapidly spinning stars among binary systems supports the idea that most stars with ν_esini_~> 300kms^-1 in the single-star sample are actually spun-up post-binary interaction products. Finally, the overall similarities (low-velocity peak and intermediate-velocity shoulder) of the spin distribution of binary and single stars argue for a massive star formation process in which the initial spin is set independently of whether stars are formed as single stars or as components of a binary system.

Energy levels and radiative rates for Cr-like Cu VI and Zn VII

Energy levels and radiative rates (. A-values) for transitions in Cr-like Cu VI and Zn VII are reported. These data are determined in the quasi-relativistic approach (QR), by employing a very large configuration interaction (CI) expansion which is highly important for these ions. No radiative rates are available in the literature to compare with our results, but our calculated energies are in close agreement with those compiled by NIST and other available theoretical data, for a majority of the levels. The A-values (and resultant lifetimes) are listed for all significantly contributing E1, E2 and M1 radiative transitions among the energetically lowest 322 levels of each ion.

Energy levels and radiative rates for transitions in Cr-like Co IV and Ni V

We report calculations of energy levels and radiative rates (A-values) for transitions in Cr-like Co IV and Ni V. The quasi-relativistic Hartree-Fock (QRHF) code is adopted for calculating the data although grasp (general-purpose relativistic atomic structure package) and flexible atomic code (fac) have also been employed for comparison purposes. No radiative rates are available in the literature to compare with our results, but our calculated energies are in close agreement with those compiled by NIST for a majority of the levels. However, there are discrepancies for a few levels of up to 3%. The A-values are listed for all significantly contributing E1, E2 and M1 transitions, and the corresponding lifetimes reported, although unfortunately no previous theoretical or experimental results exist to compare with our data.

Radiative rates for E1, E2, M1, and M2 transitions in S-like to F-like tungsten ions (W LIX to W LXVI)

Calculations of energy levels, radiative rates and lifetimes are reported for eight ions of tungsten, i.e. S-like (W LIX) to F-like (W LXVI). A large number of levels have been considered for each ion and extensive configuration interaction has been included among a range of configurations. For the calculations, the general-purpose relativistic atomic structure package (. grasp) has been adopted, and radiative rates (as well as oscillator strengths and line strengths) are listed for all E1, E2, M1, and M2 transitions of the ions. Comparisons have been made with earlier available experimental and theoretical energies, although these are limited to only a few levels for most ions. Therefore for additional accuracy assessments, particularly for energy levels, analogous calculations have been performed with the flexible atomic code (. fac).

Radiative rates for E1, E2, M1, and M2 transitions in Br-like ions with 43≤Z≤50

Energies and lifetimes are reported for the eight Br-like ions with 43≤Z≤50, namely Tc IX, Ru X, Rh XI, Pd XII, Ag XIII, Cd XIV, In XV, and Sn XVI. Results are listed for the lowest 375 levels, which mostly belong to the 4s²4p⁵, 4s²4p⁴4ℓ, 4s4p⁶,4s²4p⁴5ℓ, 4s²4p³4d², 4s4p⁵4ℓ, and 4s4p⁵5ℓ configurations. Extensive configuration interaction among 39 configurations (generating 3990 levels) has been considered and the general-purpose relativistic atomic structure package (grasp) has been adopted for the calculations. Radiative rates are listed for all E1, E2, M1, and M2 transitions involving the lowest 375 levels. Previous experimental and theoretical energies are available for only a few levels of three, namely Ru X, Rh XI and Pd XII. Differences with the measured energies are up to 4% but the present results are an improvement (by up to 0.3 Ryd) in comparison to other recently reported theoretical data. Similarly for radiative rates and lifetimes, prior results are limited to those involving only 31 levels of the 4s²4p⁵, 4s²4p⁴4d, and 4s4p⁶ configurations for the last four ions. Moreover, there are generally no discrepancies with our results, although the larger calculations reported here differ by up to two orders of magnitude for a few transitions.

Radiative rates for E1, E2, M1, and M2 transitions in F-like ions with 37≤Z≤53

Calculations of energy levels, radiative rates and lifetimes are reported for 17 F-like ions with 37≤Z≤53. For brevity, results are only presented among the lowest 113 levels of the 2s²2p⁵, 2s2p⁶, 2s²2p⁴3ℓ, 2s2p⁵3ℓ, and 2p⁶3ℓ configurations, although the calculations have been performed for up to 501 levels in each ion. The general-purpose relativistic atomic structure package (grasp) has been adopted for the calculations, and radiative rates (along with oscillator strengths and line strengths) are listed for all E1, E2, M1, and M2 transitions of the ions. Comparisons are made with earlier available experimental and theoretical energies, although these are limited to only a few levels for most ions. Therefore for additional accuracy assessments, particularly for energy levels, analogous calculations have been performed with the Flexible Atomic Code (fac), for up to 72 259 levels. Limited previous results are available for radiative rates for comparison purposes, and no large discrepancy is observed for any transition and/or ion.

Three-dimensional simulations of gravitationally confined detonations compared to observations of SN 1991T

The gravitationally confined detonation (GCD) model has been proposed as a possible explosion mechanism for Type Ia supernovae in the single-degenerate evolution channel. It starts with ignition of a deflagration in a single off-centre bubble in a near-Chandrasekhar-mass white dwarf. Driven by buoyancy, the deflagration flame rises in a narrow cone towards the surface. For the most part, the main component of the flow of the expanding ashes remains radial, but upon reaching the outer, low-pressure layers of the white dwarf, an additional lateral component develops. This causes the deflagration ashes to converge again at the opposite side, where the compression heats fuel and a detonation may be launched. We first performed five three-dimensional hydrodynamic simulations of the deflagration phase in 1.4 M⊙ carbon/oxygen white dwarfs at intermediate-resolution (2563computational zones). We confirm that the closer the initial deflagration is ignited to the centre, the slower the buoyant rise and the longer the deflagration ashes takes to break out and close in on the opposite pole to collide. To test the GCD explosion model, we then performed a high-resolution (5123 computational zones) simulation for a model with an ignition spot offset near the upper limit of what is still justifiable, 200 km. This high-resolution simulation met our deliberately optimistic detonation criteria, and we initiated a detonation. The detonation burned through the white dwarf and led to its complete disruption. For this model, we determined detailed nucleosynthetic yields by post-processing 106 tracer particles with a 384 nuclide reaction network, and we present multi-band light curves and time-dependent optical spectra. We find that our synthetic observables show a prominent viewing-angle sensitivity in ultraviolet and blue wavelength bands, which contradicts observed SNe Ia. The strong dependence on the viewing angle is caused by the asymmetric distribution of the deflagration ashes in the outer ejecta layers. Finally, we compared our model to SN 1991T. The overall flux level of the model is slightly too low, and the model predicts pre-maximum light spectral features due to Ca, S, and Si that are too strong. Furthermore, the model chemical abundance stratification qualitatively disagrees with recent abundance tomography results in two key areas: our model lacks low-velocity stable Fe and instead has copious amounts of high-velocity 56Ni and stable Fe. We therefore do not find good agreement of the model with SN 1991T.

Stratégie d'amélioration de la résistance mécanique des zones de connecteurs

Le bois subit une demande croissante comme matériau de construction dans les bâtiments de grandes dimensions. Ses qualités de matériau renouvelable et esthétique le rendent attrayant pour les architectes. Lorsque comparé à des produits fonctionnellement équivalents, il apparait que le bois permet de réduire la consommation d’énergie non-renouvelable. Sa transformation nécessite une quantité d’énergie inférieure que l’acier et le béton. Par ailleurs, par son origine biologique, une structure en bois permet de stocker du carbone biogénique pour la durée de vie du bâtiment. Maintenant permis jusqu’à six étages de hauteur au Canada, les bâtiments de grande taille en bois relèvent des défis de conception. Lors du dimensionnement des structures, les zones des connecteurs sont souvent les points critiques. Effectivement, les contraintes y sont maximales. Les structures peuvent alors apparaitre massives et diminuer l’innovation architecturale. De nouvelles stratégies doivent donc être développées afin d’améliorer la résistance mécanique dans les zones de connecteurs. Différents travaux ont récemment porté sur la création ou l’amélioration de types d’assemblage. Dans cette étude, l’accent est mis sur le renforcement du bois utilisé dans la région de connexion. L’imprégnation a été choisie comme solution de renfort puisque la littérature démontre qu’il est possible d’augmenter la dureté du bois avec cette technique. L’utilisation de cette stratégie de renfort sur l’épinette noire (Picea Mariana (Mill.) BSP) pour une application structurale est l’élément de nouveauté dans cette recherche. À défaut d’effectuer une imprégnation jusqu’au coeur des pièces, l’essence peu perméable de bois employée favorise la création d’une mince couche en surface traitée sans avoir à utiliser une quantité importante de produits chimiques. L’agent d’imprégnation est composé de 1,6 hexanediol diacrylate, de triméthylopropane tricacrylate et d’un oligomère de polyester acrylate. Une deuxième formulation contenant des nanoparticules de SiO2 a permis de vérifier l’effet des nanoparticules sur l’augmentation de la résistance mécanique du bois. Ainsi, dans ce projet, un procédé d’imprégnation vide-pression a servi à modifier un nouveau matériau à base de bois permettant des assemblages plus résistants mécaniquement. Le test de portance locale à l’enfoncement parallèle au fil d’un connecteur de type tige a été réalisé afin de déterminer l’apport du traitement sur le bois utilisé comme élément de connexion. L’effet d’échelle a été observé par la réalisation du test avec trois diamètres de boulons différents (9,525 mm, 12,700 mm et 15,875 mm). En outre, le test a été effectué selon un chargement perpendiculaire au fil pour le boulon de moyen diamètre (12,700 mm). La corrélation d’images numériques a été utilisée comme outil d’analyse de la répartition des contraintes dans le bois. Les résultats ont démontré une portance du bois plus élevée suite au traitement. Par ailleurs, l’efficacité est croissante lorsque le diamètre du boulon diminue. C’est un produit avec une valeur caractéristique de la portance locale parallèle au fil de 79% supérieure qui a été créé dans le cas du test avec le boulon de 9,525 mm. La raideur du bois a subi une augmentation avoisinant les 30%. Suite au traitement, la présence d’une rupture par fissuration est moins fréquente. Les contraintes se distribuent plus largement autour de la région de connexion. Le traitement n’a pas produit d’effet significatif sur la résistance mécanique de l’assemblage dans le cas d’un enfoncement du boulon perpendiculairement au fil du bois. De même, l’effet des nanoparticules en solution n’est pas ressorti significatif. Malgré une pénétration très faible du liquide à l’intérieur du bois, la couche densifiée en surface créée suite au traitement est suffisante pour produire un nouveau matériau plus résistant dans les zones de connexion. Le renfort du bois dans la région des connecteurs doit influencer le dimensionnement des structures de grande taille. Avec des éléments de connexion renforcés, il sera possible d’allonger les portées des poutres, multipliant ainsi les possibilités architecturales. Le renfort pourra aussi permettre de réduire les sections des poutres et d’utiliser une quantité moindre de bois dans un bâtiment. Cela engendrera des coûts de transport et des coûts reliés au temps d’assemblage réduits. De plus, un connecteur plus résistant permettra d’être utilisé en moins grande quantité dans un assemblage. Les coûts d’approvisionnement en éléments métalliques et le temps de pose sur le site pourront être revus à la baisse. Les avantages d’un nouveau matériau à base de bois plus performant utilisé dans les connexions permettront de promouvoir le bois dans les constructions de grande taille et de réduire l’impact environnemental des bâtiments.

Impacts d’une variabilité climatique changeante sur la morphologie de berges des chenaux du delta du Gange-Bramapoutre-Meghna et leurs conséquences en zones densément peuplées

Les changements climatiques, au niveau de la variabilité du climat, se font ressentir un peu partout à travers le globe que ce soit par le décalage des saisons, une variation des précipitations ou l’augmentation des températures. Certaines régions telles que le delta du Gange-Brahmapoutre-Meghna subissent au quotidien les impacts de ces variations. Quatre grandes perturbations environnementales chamboulent cette dynamique dans cette grande région du delta du GANGE-BRAHMAPOUTRE-MEGHNA : le changement du régime des précipitations, la fonte des glaciers causée par la hausse des températures moyennes annuelles, l’augmentation du niveau marin moyen et les perturbations climatiques extrêmes ponctuelles. Ces perturbations transforment le trait de côte, d’une manière directe ou indirecte. Cette fragilité des berges devient problématique dans un environnement urbain à forte densité. Nos résultats mettent en évidence que, dans un contexte de variabilité climatique changeant et de densité de population croissante, la région du delta du GANGE-BRAHMAPOUTRE-MEGHNA souffre d’une perte de terre viable entraînant des déplacements de populations. Certaines villes ont connu une augmentation de leur population allant au-delà de 1000% sur la période de 1921-2011. L’analyse de photographies aériennes sur la période 2001- 2013 montre un accroissement de l’étendue des zones urbaines, mais aussi du mouvement des berges. Sur une période plus récente, on constate même que de nouveaux quartiers ont été construits dans les zones inondées de 2004.

Factors influencing the radiative surface temperature of grey seal (Halichoerus grypus) pups during early and late lactation

The aim of this study was to examine the variation in body surface temperature of grey seal (Halichoerus grypus) pups throughout lactation in response to different environmental conditions. Radiative surface temperatures (T r, °C) of pups were measured on the Isle of May (56°11′N, 02°33′W), southeast Scotland from 29 October to 25 November 2003. Records were obtained from a total of 60 pups (32 female and 28 male) from three different pupping sites during early and late lactation. Pups were sheltered from high wind speeds but air temperature, humidity and solar radiation at pupping sites were similar to general meteorological conditions. The mean T r of all pups was 15.8°C (range 7.7–29.7°C) at an average air temperature of 10.2°C (range 6.5–13.8°C). There was no difference in the mean T r of pups between early and late lactation. However, the T r varied between different regions of the body with hind flippers on average 2–6°C warmer than all other areas measured. There was no difference in mean T r of male and female pups and pup body mass did not account for the variation in T r during early or late lactation. Throughout the day there was an increase in the T r of pups and this explained 20–28% of the variation in T r depending on stage of lactation. There was no difference in the mean T r of pups between pupping sites or associated with different substrate types. Wind speed and substrate temperature had no effect on the T r of pups. However, solar radiation, air temperature and relative humidity accounted for 48% of the variation in mean T r of pups during early lactation. During late lactation air temperature and solar radiation alone accounted for 43% of the variation in T r. These results indicate that environmental conditions explain only some of the variation in T r of grey seal pups in natural conditions. Differences in T r however indicate that the cost of thermoregulation for pups will vary throughout lactation. Further studies examining intrinsic factors such as blubber thickness and activity levels are necessary before developing reliable biophysical models for grey seals.

Les zones industrielles d’exportation : Le cas de la Tunisie

Ce mémoire compte deux parties distinctes, chacune étant toutefois rattachée à une étude du régime des entreprises entièrement exportatrices de la Tunisie, à laquelle nous avons participé. Ce régime instauré en 1972, avec des modifications depuis, avait pour but d'établir des conditions favorables à la venue d'investissements étrangers dans les secteurs d'exportation. Ce type de régime correspond, dans ses grandes lignes, à ce qu'il est convenu d'appeler les zones industrielles d'exportation. La première partie de ce mémoire est une revue de la littérature sur le sujet, une étude du pour et du contre autant d'un point de vue théorique que pratique. Nous tenterons par la suite d'en dégager des points de réflexion sur l'expérience tunisienne. Celle-ci a-t-elle rencontré des conditions qui favorisait sa réussite? Toujours dans le cadre de l'étude du régime tunisien, il a été nécessaire d'utiliser le concept de "taux de change de référence"(TCR), afin d'évaluer les avantages et les coûts de l'établissement de tels incitatifs. Il s'agit en quelque sorte de calculer le prix de référence (shadow price) des devises utilisées dans ce régime ou générées par lui. La seconde partie de ce mémoire consiste, dans un premier temps, à expliquer les bases théoriques du taux de change de référence, c'est-à-dire à en établir la définition selon deux différentes approches, et à en donner les formes d'évaluation. Dans un deuxième temps, nous tentons d'estimer le TCR de la Tunisie. Cet exercice avait déjà été tenté par l'Institut d'Économie Quantitative de la Tunisie en 1988 sur la base de la protection commerciale existante en 1983. Cependant, la fiabilité du résultat pouvait être améliorée en ce qui concerne l'estimation de l'élasticité des demandes d'importation. Nous avons refait ces estimations en utilisant un plus grand nombre de données. De plus nous avons basé nos calculs du TCR sur la base de la protection existante en 1990.