Un nouvel essai mécanique a été développé pour répondre à la demande d'analyse des propriétés mécaniques des revêtements et films d'épaisseur nanométrique par essai de gonflement. La méthode utilisée est l'application d'une différence de pression sur une membrane non supportée, usinée en utilisant les techniques standards de gravure microélectronique. Le banc d'essai permettra d'effectuer des essais à haute température (au dessus de 900°C). La principale difficulté rencontrée a été la mise au point d'une méthode de mesure de la déflection de la membrane qui perturbe celle ci aussi peu que possible. Deux techniques ont été utilisées : capteur ponctuel et capteur interférométrique 2D avec référence sphérique. La première technique, plus simple, s'est révélée difficilement praticable, en particulier dans le cas de flambage de la membrane. La mise en place de la deuxième a nécessité une description fine du comportement du système optique (distorsion des images, calcul des interférogrammes) aboutissant à une méthode de mesure simple, susceptible d'être intégrée en ligne au système de contrôle de l'interféromètre, et complétée par un traitement complet des données après essai.Afin de valider l'essai, deux types de revêtements ont été caractérisés. Tout d'abord des films fragiles de nitrure de silicium et de silicium pour mettre en évidence la fiabilité et la reproductibilité des essais. Puis des films minces d'or pour observer l'influence de la microstructure sur le début de la déformation plastique / A new mechanical testing device of free standing membranes by Bulge Test has been built at Institute Jean Lamour in order to investigate the mechanical properties of thin films of nanometric thickness. The Bulge Test measures the deflection of a free standing membrane to which a differential atmospheric pressure has been applied. (The specimens are prepared from film on substrate deposits by cutting a window within the substrate by standard microelectronic techniques.) We aim of achieve tests from room temperature to ~ 900°C. The main technical difficulty met during this work was to develop a non perturbating method of measurement of the film bulge. Two different techniques were tested: point measurement and 2D interferometry using a spherical reference. The first technique, however simple, was difficult to practice, especially in the case of buckling membranes. The second method required a detailed analysis of the whole optical system (image distorsion, calculation of interferograms) leading to a simple measurement method, suitable for integration in the acquisition and command chain of the device, followed by an off line full treatment.The operating method was used on two different sets of specimens: fragile silicon nitride and silicon membranes in order to test the reproducibility of the device. Polycrystalline gold thin films were then used to study the early stage of plastic strain

Os aglomerados globulares (GCs) são laboratórios essenciais no estudo da formação e evolução quimiodinâmica da Via Láctea, pois formaram-se durante os episódios iniciais de formação estelar das galáxias. Na última década, evidências observacionais fotométricas e espectroscópicas têm desafiado o paradigma clássico da formação dos GCs em um episódio único de formação estelar, dando origem ao debate sobre as múltiplas populações estelares. Com o objetivo de explorar esse fenômeno, o programa do Telescópio Espacial Hubble GO-13297 (UV Legacy Survey of Galactic Globular Clusters, PI G. Piotto) obteve fotometria para 57 GCs com os filtros UV/azul F275W, F336W e F438W (WFC3/UVIS), sensíveis às variações nas abundâncias de CNO e, portanto, capazes de distinguir múltiplas populações ao longo dos diagramas cor-magnitude. Combinados com fotometria anterior nos filtros do óptico F606W e F814W (programa GO-10775, PI A. Sarajedini), eles formam uma base de dados fotométricos sem precedentes para GCs. Este trabalho expõe a análise de sete desses aglomerados, sendo seis do Bojo Galáctico (NGC 6304, NGC 6624, NGC 6637, NGC 6652, NGC 6717 e NGC 6723) e um localizado no Halo interno para referência (NGC 6362). A amostra é representativa dos dois picos na distribuição de metalicidades dos GCs do Bojo, em [Fe/H] ~ -0.5 e -1.0. Adotou-se métodos homogêneos para a separação das múltiplas populações nos diferentes estágios evolutivos e para o ajuste de isócronas, com o intuito de analisar comparativamente os dois grupos de metalicidade e verificar se ocorre alguma diferença de idades detectável entre as múltiplas populações. Algoritmos de classificação com aprendizado de máquina, e métodos utilizando estatística Bayesiana (máxima verossimilhança e MCMC) foram implementados e uma ferramenta em Python, nomeada SIRIUS, foi desenvolvida pelo grupo. Os resultados apontam para uma tendência de idades maiores (~ 13 Gyr) para os GCs mais pobres em metais com ramo horizontal azul, comparado com 12.0-12.5 Gyr para os outros GCs. Os resultados para as múltiplas populações indicam idades ligeiramente mais altas para a primeira geração em geral, mas com diferenças menores que 400 Myr comparado com a segunda geração. O resultado de 13.14 +0.25/-0.43 Gyr para o aglomerado NGC 6717 surpreende pois este é o aglomerado menos massivo da amostra, com maior fração de estrelas da primeira geração e com um ramo horizontal azul estendido: aspectos que o colocam como um dos objetos mais velhos da Galáxia. Esses resultados são bastante relevantes, com impactos diretos nos cenários de formação das partes centrais da Galáxia. / The globular clusters (GCs) are fundamental laboratories to study the formation and chemodynamical evolution of the Milky Way, as they formed during the initial episodes of star formation in galaxies. In the last decade, photometric and spectroscopic observational results have challenged the classical paradigm of GCs formation in a single star formation burst, giving rise to the debate about multiple stellar populations. With the purpose of better explore this phenomenon, the Hubble Space Telescope GO-13297 program (UV Legacy Survey of Galactic Globular Clusters, PI: G. Piotto) obtained photometry for 57 GCs with the UV/blue filters F275W, F336W and F438W (WFC3/UVIS), sensitive to variations in CNO abundances, and consequently able to distinguish multiple populations along the color-magnitude diagrams. Combined with previous photometry in the optical filters F606W and F814W (GO-10775 program, PI A. Sarajedini), they provide an unprecedented photometric database for GCs. This work presents the analysis of seven of these clusters, six of them from the Galactic Bulge (NGC 6304, NGC 6624, NGC 6637, NGC 6652, NGC 6717 and NGC 6723) and one located in the inner Halo for reference purposes (NGC 6362). This sample is representative of the two peaks in the metallicity distribution of Bulge GCs, with [Fe/H] ~ -0.5 and -1.0. We adopted homogeneous methods to the separation of multiple populations in the different evolutionary stages and to the isochrone fitting, with the purpose of analyze comparatively the two metallicity groups, and check whether there occurs any detectable age difference between the multiple populations. Classification algorithms with machine learning, and methods using Bayesian statistics (maximum likelihood and MCMC) were implemented and a Python tool, named SIRIUS, was developed by the group. The results point to a trend of larger ages (~ 13 Gyr) for the more metal-poor clusters with a blue horizontal branch, compared with 12.0-12.5 Gyr for the other GCs. The results for the multiple populations indicate slightly larger ages for the first generation in general, but with differences lower than 400 Myr compared with the second generation. The result of 13.14 +0.25/-0.43 Gyr for the cluster NGC 6717 is surprising because this is the least massive cluster of the sample, with the highest fraction of first generation stars and with a blue horizontal branch: features that place it as one of the oldest objects in the Galaxy. These results are quite relevant, with direct impacts on the formation scenarios of the innermost regions of the Galaxy.

Ο σκοπός της παρούσας διδακτορικής διατριβής ήταν η μελέτη δύο σημαντικών φαινομένων μεσοαστρική ύλης όπως είναι τα Πλανητικά Νεφελώμάτα (ΠΝ) και η ράβδος των σπειροειδών γαλαξιών. Πιο συγκεκριμένα, μελετήθηκαν 44 ΠΝ στην περιοχή του Γαλαξιακού σφαιροειδούς (Boumis et al. 2003; 2006) και προσδιορίστηκαν οι φυσικοί παράμετροι τους, όπως είναι η ενεργός θερμοκρασία και η λαμπρότητα του κεντρικού αστεριού, η πυκνότητα και η θερμοκρασία των ηλεκτρονίων, η αφθονία των Ηe, N, O, S κτλ., χρησιμοποιώντας το μοντέλο φωτο-ιονισμού Cloudy (Akras et al. 2010a). Επίσης, μελετήθηκε η ράβδος των γαλαξιών, χρησιμοποιώντας το μοντέλο διάδοσης ακτινοβολίας CRETE, με σκοπό να ερευνηθεί πώς η ύπαρξη της ράβδου επηρεάζει την μορφολογία των γαλαξιών και την σκόνη τους. Ταυτόχρονα, προσδιορίστηκαν οι παράμετροι της ράβδου, όπως το μήκος, το ύψος, η γωνία κλίσης και η γωνία θέσης της για 4 ραβδωτούς σπειροειδείς γαλαξίες (NGC 4013, UGC 2048, IC 2531 και το Γαλαξία μας). Στο πρώτο μέρος της μελέτης, διαχωρίστηκαν τα ΠΝ ανάλογα με την μορφολογία τους σε σφαιρικά, ελλειπτικά και διπολικά και βρέθηκε ότι η αφθονία του Ηe και του Ν είναι μεγαλύτερη στην τελευταία κατηγορία σε σχέση με τις υπόλοιπες. Επιπλέον, η χρήση του στατιστικού εργαλείου PCA, έδειξε ότι τα κυκλικά και τα ελλειπτικά ΠΝ διαχωρίζονται από τα διπολικά, βάσει της τιμής του λόγου log(Ν/Ο), ο οποίος παίρνει αρνητικές και θετικές τιμές για τα διπολικά, ενώ μόνο αρνητικές τιμές στις υπόλοιπες κατηγορίες. Η κρίσιμη τιμή βρέθηκε ίση με -0.18 dex και αντιστοιχεί σε μάζα προγενέστερου αστεριού ίση με 2.6 (Akras & Boumis 2007). Στο δεύτερο μέρος, περιγράφηκε η ράβδος των γαλαξιών χρησιμοποιώντας την συναρτησιακή ελλειψοειδής υπερβολής. Μεταβάλλοντας την γωνία κλίσης του γαλαξία, η δομή σχήματος «Χ», η οποία παρατηρείται στις ράβδους, μπορεί να παρατηρηθεί μόνο για γωνίες μεγαλύτερες από 60ο. Επιπρόσθετα, στην περίπτωση του Γαλαξία μας, βρέθηκε ότι η γωνία θέσης της ράβδου είναι γύρω στις 25ο και το μήκος της 3.75 kpc (Akras et al. 2010b). Λαμβάνοντας υπόψη ότι η μέση τιμή του μήκους της ράβδου στους γαλαξίες είναι μεταξύ 3.0 και 4.0 kpc, προκύπτει ότι για τον NGC 4013 η γωνία θέσης του είναι μεταξύ 5 και 10 μοίρες, για τον UGC 2048 μεταξύ 40 και 50 μοίρες, για τον IC 2531 35 και 45 μοίρες ενώ τέλος για το Γαλαξία μας υπολογίζεται μεταξύ 20 και 30 μοίρες (Akras et al. 2010b). / The aim of this PhD thesis was the study of two very important interstellar medium phenomena like the Planetary Nebulae (PNe) and the stellar bar in spiral galaxies. In particular, we studied 44 PNe in the Galactic bulge region and we determined their physical parameters, like the effective temperature and luminosity of the central star, the electron temperature and density, the abundance of He, N, O, S etc., using the photo-ionization model “Cloudy” (Akras et al. 2010a). It was also pursued to study the stellar bar component using the 3D radiative transfer model CRETE, in order to investigate the effects of a stellar bar component to the morphology of the galaxy and its dust content. In addition, the parameters of the bar component such as the length, the height, the inclination angle and the position angle were determined for four spiral galaxies (NGC 4013, UGC 2048, IC 2531 and our Galaxy). In the first part of the thesis, the PNe were separated according to their morphology (spherical, elliptical and bipolar shape) and we found that the He and N abundances are greater in bipolar PNe. Moreover, by using the statistical tool PCA, it was found that the circular and the elliptical PNe are different from the bipolar, since the log(O/N) takes negative values in the first two and positive or negative values in the bipolar PNe. The critical value was found at -0.18 dex, which corresponds to a stellar mass of 2.6 (Akras & Boumis 2007). In the second part, we managed to accurately describe the morphology of the bar component by using the function of hyperbolic ellipse. For different inclination angles of the observed galaxies, it was found that the “X-shape" feature can be seen only in the case where the inclination angle is greater than 60 degrees. In the case of Milky Way, it was found that the position angle of the bar is approximately 25 degrees and the length equals to 3.75 kpc (Akras et al. 2010b). Considering that the mean length of the bar component is equal to 3.0-4.0 kpc, it was determined that the position angle of a) NGC 4013 takes values between 5 and 10 degrees, b) UGC 2048 takes values between 40 and 50 degrees, c) IC 2531 takes values between 35 and 45 degrees, and our Galaxy takes values between 20 and 30 degrees (Akras et al. 2010b).

This thesis offers an account of children's lived experiences in Rwanda (1930s-2016) in four key domains: kinship, education, economic transitions, and marriage. Based on historical and ethnographic fieldwork in rural and urban Rwanda from 2012 to 2014, this work explores how three generations of young people have experienced and navigated childhood and coming of age at the interface of 'traditional' and 'modern' institutional systems. Rather than focusing narrowly on 'crisis' childhoods, individual agency, or exogenous forces, as studies of young Africans and social change tend to, this work examines young people's 'everyday' actions - intentional and unintentional, individual and collective, compliant and non-compliant - and locates them within their broader historical, relational, and institutional environment. By focusing on the intensely reproductive period of childhood and coming of age, on Rwanda's unexceptional majority rather than its exceptionally vulnerable minority, and on children's everyday actions rather than the strategic actions of elites, this thesis shows us how children shape the institutions of childhood and marriage and, in so doing, influence how society is reproduced and changed. Theoretically, this thesis explains how children and their institutional environment are mutually constituting: it examines how and why young people experience rapid change and structural violence differently and it traces how they reproduce and change these structural conditions as they engage with institutional mechanisms in (un)intended ways. The research reveals that children in central Rwanda navigate constraints and opportunities by drawing on established kinship relationships and institutions while also opportunistically engaging with modern institutions and their actors. However, in this context of 'institutional multiplicity', traditional and modern institutional systems each need Rwanda's young majority to reproduce their institutions over others', and as intended, to achieve their power-distributional goals. This makes children's actions particularly consequential and demands that we redefine what political action - and political actors - look like.

Le bulbe Galactique, est cruciale pour comprendre les processus physiques responsables de la formationde la galaxie. L'étude spectroscopique des étoiles vieilles de faible masse permettre de caractériser endétail la chimie et la cinématique du bulbe. Dans cette thèse, nous avons utilisé des données provenantdu Gaia-ESO survey pour mener une étude détaillée du système du disque ainsi que du bulbeGalactique. La distribution de métallicité du bulbe est bimodale. La population riche en métaux montreune cinématique typique de la barre. Elle présente une caractéristique de double RC et recouvre laséquence du disque mince à haute métallicité dans le plan [Mg/Fe] vs. [Fe/H]. Nous associons cesétoiles avec celles de la barre formée à la suite de l'évolution séculaire du disque mince primordial.D'autre part, la population pauvre en métaux présente une cinématique chaude et ne participe pas à laforme en X du bulbe. Ces étoiles semblent imiter la distribution de celles du disque épais dans le plan[Mg/Fe] vs. [Fe/H]. Quand nous comparons la position en métallicité du genou de cette distribution,qui se trouve à [Fe/H]=-0.37+/-0.09 dex, elle est plus élevée de 0.6 dex par rapport au disque épais. Unmodèle d'évolution chimique permet de bien ajuster cette distribution pour les étoiles du bulbe ensupposant un épisode de formation stellaire rapide (<1 Gyr) et intense. L'origine du bulbe pauvre enmétaux reste encore relativement incomprise, mais divers projets futurs devraient permettre de faire ladistinction entre les processus violents ou ceux liés à une évolution séculaire qui ont pu contribuer à saformation / The Galactic bulge, as a massive and old Galactic component, is key to understand the physicalprocesses responsibles for the formation of the Galaxy. The spectroscopic study of long lived low massstars represents an opportunity to characterize the detailed chemical and kinematical patterns of theeventual mix of stellar populations building up the bulge. In this thesis we made use of data comingfrom the Gaia-ESO survey to conduct a detailed analysis of the disk system as well as bulge stellarpopulations. The bulge metallicity distribution function is bimodal. The metal-rich population exhibitsbar-like kinematics, displays the double RC feature and overlaps the metal-rich end of the thin disksequence in the [Mg/Fe] vs. [Fe/H] plane. We associate these stars with the bar X-shape bulge formedas the product of secular evolution of the early thin disk. On the other hand, the metal-poor populationpresents isotropic hot kinematics and does not participate in the X-shaped bulge. When compared to thethick disk, bulge stars seem to mimic their distribution in the [Mg/Fe] vs. [Fe/H] plane. Whencomparing the metallicity position of the so called ``knee'', that of the bulge is found to be at [Fe/H]=-0.37+/-0.09 dex, being 0.6 dex higher than that of the thick disk. A chemical evolution model suitablyfits the whole bulge sequence by assuming a fast (<1 Gyr) intense burst of star formation taking place atearly epochs. The origin of the metal-poor bulge still remains unconstrained, but further research shouldallow to distinguish between violent processes or secular evolution for its origin

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Les modèles numériques personnalisables d'organes du corps humain offrent un formidable potentiel pour évaluer le risque lésionnel dans les domaines de la sécurité des transports, du médical ou du sport. Suivant les applications, différents niveaux de détails peuvent être nécessaires. En particulier, lorsque le comportement mécanique des tissus biologiques doit être finement reproduit, les modèles de comportement doivent intégrer des considérations sur la structure du tissu, et simuler les mécanismes suivant lesquels il réagit à un chargement mécanique. Le travail de thèse présenté ici s'est focalisé sur la capsule de foie, notamment sur ses propriétés microstructurales et mécaniques, afin d'identifier les hypothèses importantes à intégrer dans la construction d'un modèle constitutif de tissu fibreux basé sur la microstructure. La méthodologie expérimentale a été mise en place afin de caractériser le comportement mécanique de ce tissu, en lien avec l'organisation de sa microstructure. Des essais de traction uniaxiale et de gonflement sous microscope confocal biphotonique ont été développés, pour observer l'évolution de la microstructure sous chargement. Des déformations macroscopiques ont été mesurées, et une méthode de mesure de champs de déformations locaux a été développée pour quantifier l'état de déformation du réseau de fibres. La réorganisation du réseau de fibre de collagène a également été quantifiée. L'analyse des liens existant entre les grandeurs mesurées à l'échelle macroscopique et ces phénomènes microscopiques est proposée, pour préciser les hypothèses à adopter dans les modèles permettant de passer de l'échelle des fibres au comportement global du tissu / Customized human body models offer a great potential to assess the injury risks in the fields of transport safety, surgery or sport. Various detail levels can then be needed, according to the targeted application. In particular, when the mechanical behavior of biological tissues needs to be accurately reproduced, numerical models have to include information about the structure of the tissue, and model the mechanisms of the response to mechanical loading. The work presented here focuses on the microstructural and mechanical characterization of the human liver capsule, in order to identify the important hypotheses that need to be included in a fibrous tissue constitutive model, based on microstructure. Thus, an experimental methodology has been developed to identify the mechanical behavior of this particular tissue, related with its microstructural organization. Uniaxial tensile tests, as well as bulge tests under a multiphoton confocal microscope have been performed, to observe the microstructure evolution during loading. Macroscopic strain has been assessed, and a method to measure local strain fields has been developed, to quantify the strain state of the fibrous network. The reorganization of the collagen fibers network has also been quantified. An analysis of the links between the measured macroscopic parameters and the microscopic phenomena is given. Therefore, the hypotheses that need to be included in constitutive models are highlighted, with particular consideration given to the affine transformation hypothesis which allows to link the fibers behavior to the global response of the tissue

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