Le milieu interstellaire (MIS) est un système extrêmement complexe. Il correspond à une échelle intermédiaire entre les étoiles et les galaxies. Le gaz interstellaire est présent dans toute la galaxie, remplissant l’espace entre les étoiles. Une grande diversité de processus couplés, comme la gravité, le champs magnétiques, la turbulence et la chimie, participe à son évolution, faisant de la modélisation du MIS un problème ardu. Une description correcte du MIS nécessite un bon traitement des équations de la magnetohydrodynamique (MHD), de la gravité, du bilan thermique et de l’évolution chimique à l’intérieur du nuage moléculaire.L’objectif de ce travail de thèse est une meilleure compréhension de la formation et de l’évolution des nuages moléculaires, et plus particulièrement de la transition du gaz atomique en gaz moléculaire. Nous avons réalisé des simulations numériques de la formation des nuages moléculaires et de la formation de l’hydrogène moléculaire sous l’influence de la gravité et de la turbulence MHD, en utilisant des estimations précises de l’écrantage par les poussières et de l’auto-écrantage par la molécule H2. Ceci a été calculé grâce à une méthode en arbre, à même de fournir une rapide estimation des densités de colonne.Nous avons trouvé que l’hydrogène moléculaire se forme plus rapidement que prévu par les estimations classiques du fait de l’augmentation de densité locale provoquée par les fluctuations turbulentes du gaz. L’hydrogène moléculaire, formé à des densités plus élevées, peut alors migrer vers les régions plus chaudes et moins denses.Les densités de colonne totale d’hydrogène moléculaire montrent que la transition HI-H2 se produit à des densités de colonne de quelques 10^20 cm−2. Nous avons calculé les populations des niveaux rotationnels de H2 à l’équilibre thermique et intégré le long de plusieurs lignes de visée. Ces résultats reproduisent bien les valeurs observées par Copernicus et FUSE, suggérant que la transition observée et les populations excitées pourraient être une conséquence de la structure multi-phasique des nuages moléculaires. Comme la formation de H2 précède la formation des autres molécules, le H2 chaud pourrait permettre le développement d’espèces endothermiques et éventuellement expliquer certains aspects de la richesse moléculaire observée dans l’ISM. / The interstellar medium (ISM) is a highly complex system. It corresponds to an intermediate scale between stars and galaxies. The interstellar gas is present throughout the galaxy, filling the volume between stars. A wide variety of coupled processes, such as gravity, magnetic fields, turbulence and chemistry, participate in its evolution, making the modeling of the ISM a challenging problem. A correct description of the ISM requires a good treatment of the magnetohydrodynamics (MHD) equations, gravity, thermal balance, and chemical evolution within the molecular clouds.This thesis work aims at a better understanding of the formation and evolution of molecular clouds, specially how they become "molecular", paying particular attention to the transition HI-to-H2. We have performed ideal MHD simulations of the formation of molecular clouds and the formation of molecular hydrogen under the influence of gravity and turbulence, using accurate estimates for the shielding effects from dust and the self-shielding for H2, calculated with a Tree-based method, able to provide fast estimates of column densities.We find that H2 is formed faster than predicted by the usual estimates due to local density enhancements created by the gas turbulent motions. Molecular hydrogen, formed at higher densities, could then migrate toward low density warmer regions.Total H2 column densities show that the HI-to-H2 transition occurs at total column densities of a few 10^20 cm−2. We have calculated the populations of rotational levels of H2 at thermal equilibrium, and integrated along several lines of sight. These two results reproduce quite well the values observed by Copernicus and FUSE, suggesting that the observed transition and the excited populations could arise as a consequence of the multi-phase structure of molecular clouds. As H2 formation is prior to further molecule formation, warm H2 could possibly allow the development of a warm chemistry, and eventually explain some aspects of the molecular richness observed in the ISM.

Im Rahmen einer Diplomarbeit an der TU Bergakademie Freiberg wurden in 2014 die Grundlagen für die Auswertung von 3D-Punktwolken zur automatisierten Nachtragung des Risswerks gelegt. Um die dafür notwendigen 3D-Punktwolken möglichst wirtschaftlich zu erstellen, laufen seit 2015 Untersuchungen und Testmessungen zur Machbarkeit des untertägigen Einsatzes von mobil messenden Laserscannern. Im Folgenden werden verschiedene technische Ansätze sowie die Ergebnisse der Testmessungen und die weiteren geplanten Schritte vorgestellt. / As part of a thesis at the Technical University of Freiberg, a basis for the analysis of 3D point clouds was set for refining the mine map automatically. Since 2015 studies and test measurements have been running to create the necessary 3D point clouds as economically as possible, by using an underground mobile scanning system. Below the different technical approaches will be presented as well as the results of the test measurements and the next planned steps.

Malgré des années de travaux théoriques et observationnels intensifs, nous sommes toujours loin d’une complète compréhension de l’univers proche, la Voie Lactée (MW) et ses galaxies voisines. Parmi les satellites de la MW, le Petit et le Grand Nuage de Magellan (LMC) sont particulièrement intéressants puisqu’ils forment le plus proche exemple de galaxies en interaction gravitationnelle et hydrodynamique, et partant, constituent un laboratoire unique pour étudier les effets des marées et l’échange de matière sur l’évolution chimique et l’histoire de la formation stellaire d’une galaxie. Le LMC est une galaxie de petite masse barrée à disque, prototype des galaxies riches en gaz que l’on pense jouer un rôle important dans la construction des grandes galaxies dans le cadre du ΛCDM. De plus, avec sa métallicité actuelle d’environ le tiers de la métallicité solaire, le chemin d’enrichissement chimique suivi par le LMC donne un grand poids aux yields des générations stellaires pauvres en métaux, ce qui fait du LMC un environnement idéal pour étudier la nucléosynthèse aux basses métallicités. Ce travail de doctorat vise à: 1) caractériser chimiquement la population de la barre du LMC, 2) comparer les tendances des éléments de la MW et du LMC et interpréter les différences ou ressemblance en termes d’évolution chimique et/ou de processus nucléosynthétiques (contraintes sur les sites et les processus nucléosynthétiques), 3) comparer l’évolution chimique de la barre et du disque interne du LMC et interpréter les différence ou ressemblance dans le contexte de la formation de la barre. Nos résultats montrent que l’histoire chimique du LMC a connu un forte contribution des supernovae de type I ainsi qu’un fort enrichissement en éléments s par les vents d’étoiles AGB pauvres en métaux. Par rapport à la MW, les étoiles massives ont eu une contribution plus petite à l’enrichissement chimique du LMC. Les différences observées entre la barre et le disque parlent en faveur d’un épisode de formation stellaire accrue il y a quelques Gyr, ayant lieu dans les zones centrales du LMC et conduisant à la formation de la barre. Ceci est en accord avec les histoires de la formation stellaire récemment dérivées. / Despite decades of intensive observational and theoretical work, we are still far from a complete and clear understanding of the nearby universe, the Milky Way (MW) and its neighbours. Among the satellites of the MW, the Small and Large Magellanic Cloud (LMC) are of particular interest since they form the closest example of galaxies in gravitational and hydrodynamical interaction, and therefore constitute a unique laboratory to study the effect of tides and matter exchange on the chemical evolution and star formation history of a galaxy. The LMC is a low-mass barred disc galaxy, prototypical of gas-rich galaxies that are thought to play an important role in the build-up of large galaxies in the ΛCDM framework. Furthermore, with its present day metallicity of only third of solar, the chemical enrichment path followed by the LMC gives a heavy weight to the yields of metal-poor stellar generations, which makes the LMC an ideal environment to study nucleosynthesis at low metallicities. This thesis work aims at: 1) chemically characterizing the LMC bar population, 2) comparing the elemental trends of the MW and the LMC and interpreting the differences or similarities in terms of chemical evolution and/or nucleosynthesis processes (constraints on the nucleosynthetic sites and processes), 3) comparing the chemical evolution of the LMC bar and inner disc and interpreting the differences or similarities between the LMC bar and inner disc in the context of the bar formation. Our results show that the chemical history of the LMC experienced a strong contribution from type Ia supernovae as well as a strong s-process enrichment from metal-poor AGB winds. Massive stars made a smaller contribution to the chemical enrichment compared to the MW. The observed differences between the bar and the disc speak in favour of an episode of enhanced star formation a few Gyr ago, occurring in the central parts of the LMC and leading to the formation of the bar. This is in agreement with recently derived star formation histories.

Plus de 80% du Groenland est recouvert de glace. Sa fonte contribue à l’augmentation du niveau des océans. Cette fonte peut être accélérée ou ralentie par les nuages qui modulent le rayonnement qui atteint la surface. Dans cette thèse, nous avons utilisé les mesures du satellite CALIPSO (produit GOCCP) pour documenter les nuages au-dessus du Groenland et éclaircir leur rôle sur la fonte de surface.Comparer ces observations avec des mesures radar et lidar réalisées à la station sol de Summit, au centre du Groenland, a montré que dans GOCCP les nuages optiquement très fins (τ < 0.3) ne sont pas détectés. Nous avons ensuite étendu l’analyse sur l’ensemble du Groenland et mis en évidence que la région nord est moins recouverte de nuages que la région sud en hiver et qu’en été, Summit, est l’une des régions les plus nuageuses en nuages liquides notamment.Pour comprendre cette particularité et les conditions favorables à la formation de nuages, nous avons utilisé des classifications en régime de temps. Cependant cette étude n’a pas mis à jour de liens entre la variabilité des nuages et la circulation atmosphérique ce qui montre la complexité de ces interactions et la nécessité d’accumuler plus d’observations sur des périodes de temps longues.Enfin nous avons évalué la représentation des nuages dans des observations lidar synthétiques, simulées à partir des sorties de modèles de climat CMIP5. Plusieurs biais qui empêchent les modèles de reproduire l’influence des nuages sur la fonte ont été identifiés. Les modèles sous estiment les températures de surface et les couvertures nuageuses. Les nuages simulés sont soit trop opaques soit trop fins pour accélérer la fonte. / Over 80% of Greenland is covered by ice. Melting of this ice contributes to the sea level rise. By modulating the radiation reaching the surface, clouds can accelerate or slow down the melting. Through this thesis, we use CALIPSO satellite measurements (GOCCP product) to document clouds over Greenland, including their vertical structure, and understand their role in surface melting.We compare these observations with radar and lidar measurement taken from the Summit ground station in the middle of Greenland. The comparison shows that GOCCP does not include optically thin ice clouds (τ < 0.3). Extending this analysis over all Greenland shows that cloudiness follows different cloud annual cycles in North and South regions, and that Summit is one of the cloudiest regions of the Greenland especially for the liquid cloud cover.To understand the atmospheric conditions favorable to cloud formation, we follow two weather regime classification approaches. We do not find a clear relationship between cloud variability and atmospheric circulation. These results show the complexity of the interactions between clouds and synoptic circulation and highlight the need to accumulate more data over long time periods.Finally, we evaluate cloud representation over Greenland in simulated lidar profiles over output from CMIP5 climate models. We identify several biases that lead to models being unable to simulate surface melting. Models underestimate the surface temperature and the cloud cover. Also when clouds are simulated they are either too opaque or too thin to affect surface melting.

A detailed understanding of cloud microphysical processes is crucial for a large range of scientific disciplines that require knowledge of cloud particles for accurate climate and weather prediction. This thesis focuses on 3 measurement campaigns, encompassing both airborne and ground based measurements of the microphysical structures observed in cold, warm and occluded frontal systems around the United Kingdom, stratocumulus clouds in the Arctic and many different clouds observed over a 6 week period at a high-alpine site in the Swiss Alps. Particular attention was paid to the origin and distribution of both primary and secondary ice and the dominant features associated with ice phase processes. During investigation of cold, warm and occluded frontal systems associated with mid-latitude cyclones around the U.K., secondary ice was often found to dominate the number and mass concentrations of ice particles in all systems. The presence of large liquid droplets was sometimes observed in close proximity to regions of secondary ice production. The existence of these provides a possible mechanism by which rime-splintering is greatly enhanced through the creation of instant rimers as the large drops freeze. In-situ measurements during the cold frontal case were used to calculate rates of diabatic heating during a comparison between bin-resolved and bulk microphysics schemes. Observations in arctic stratocumulus clouds during spring and summer seasons revealed higher ice concentrations in the summer cases when compared to the spring season. This is attributed to secondary ice production actively enhancing ice concentrations in the summer, due to the higher temperature range the clouds spanned. At Jungfraujoch in the Swiss Alps, ground based measurements allowed us to obtain high spatial scale resolution measurements of cloud microphysics and we found transitions between high and low ice mass fractions that took place on differing temporal scales spanning seconds to hours. During the campaign measurements of aerosol properties at an out of cloud site, Schilthorn, were made. When analysing a Saharan Dust Event that took place a possible link between the number of U.V. fluorescent particles and the number of ice particles was found in the temperature range around -10 ºC.

Klimatförändringarna i Arktis sker i en snabbare takt än någon annanstans på jorden. I regionen är det framförallt havsisens utbredning som drabbas, vilken har minskat med 3.8 % av medelstorleken per decennium under åren 1979-2012. För att klimatmodellerna ska kunna göra så bra beräkningar som möjligt av det framtida klimatet behövs mer observationsdata och bättre förståelse av Arktis klimatsystem. Det arktiska klimatet är komplext, svåråtkomligt för observationer och därför mindre utforskat än klimatsystemen på resten av jorden. Detta gör att klimatmodellerna i nuläget har begränsningar för regionen. De arktiska molnen utgör en osäker faktor i sammanhanget. Molnen är en viktig del i strålningsbalansen och har en stark korrelation med havsisen. De arktiska molnen har en tydlig säsongsvariation med mer molnighet sommartid än under vinterhalvåret. Detta gör att molnen över Arktis till skillnad från i jordens övriga regioner har en totalt sett värmande effekt alla årstider förutom sommaren. Forskarna är även överens om att mer observationsdata och kunskap behövs inom området, vilket skulle förbättra klimatmodellerna och öka kunskapen kring korrelationen mellan molnen och den arktiska havsisen. / In the Arctic the climate changes faster than anywhere on the planet. It is especially the expansion of the sea ice that is affected. Over the years 1979-2012, the annual average extent of the Arctic sea ice has been reduced with 3.8 % per decade. In order for climate models to make the best possible calculations of the future climate, more observation data and better understanding of the Arctic climate system are needed. The Arctic climate is complex, difficult to reach for observations and therefore less explored than the climate systems in the rest of the world. This means that climate models currently have limitations for the region. The Arctic clouds constitute an uncertain factor in this context. Clouds are an important part of the radiation balance and have a strong correlation with the sea ice. The Arctic clouds have a clear seasonal variation with more cloudiness in summer than during the winter. This makes the Arctic clouds, unlike in the rest of the world, to have a total warming effect all seasons except during the summer. The researchers also agree that more observation data and knowledge are needed for the area. It would improve climate models and expand the science about the correlation between the clouds and the Arctic sea ice.

A Pequena Nuvem de Magalhães (PNM) é uma galáxia irregular e rica em gás, que juntamente com a Grande Nuvem de Magalhães (GNM) orbita a Via Láctea (VL). Elas formam um sistema triplo em constante interação. A PNM possui metalicidade baixa, e consequentemente seu meio interestelar (MI) apresenta propriedades particularmente diferentes das observadas para o MI da Galáxia. Mais do que isso, a importância do campo magnético em escalas galácticas vem sendo evidenciada cada vez mais. Então, o objetivo desta dissertação foi estudar a estrutura do campo magnético na PNM, e sua relação com componentes do MI desta galáxia. Para este fim, utilizamos dados de polarimetria no óptico, obtidos no Cerro Tololo Inter American Observatory. Construímos um catálogo polarimétrico que contém 7.207 estrelas em 28 campos distribuídos nas secções Nordeste e da Asa da PNM. Os mapas de polarização traçam o campo magnético no plano do céu diretamente, e pode-se obter sua intensidade utilizando o método de Chandrasekhar & Fermi. A partir do catálogo polarimétrico gerado neste trabalho, conseguimos observar que o campo magnético na PNM possui direção bastante irregular, porém é provável a existência de dois padrões em larga escala o primeiro alinhado com a Ponte pan-Magelânica e o segundo alinhado com a Barra da PNM. Obtivemos para o campo magnético regular Bcéu = (1,84 ± 0,11) uG e para o campo turbulento dB = (2,920 ± 0,098) uG. Esse resultado evidencia que na PNM o campo aleatório domina com relação ao de larga escala, justificando a observação de uma configuração tão irregular para os vetores de polarização. Correlacionando os mapas de polarização com estruturas presentes no MI da PNM, pudemos verificar a presença de diversos shells que podem possuir campos magnéticos da ordem de algumas dezenas de uG. Também foi possível observar ambientes onde o campo regular parece ter sido destruído pela turbulência e outros onde ele pode ainda não ter tido tempo de se formar. Derivamos a relação entre polarização e avermelhamento, e obtivemos como resultado que ela é da ordem de P/Av ~ 2, o que indica que na PNM a eficiência para polarização pode ser menor do que na Galáxia, talvez devido a alta turbulência e/ou ao fato de que nela o campo regular é muito baixo. Por fim, a partir da estimativa para as densidades de energia do campo magnético e para o movimento de rotação e de turbulência do gás, pudemos mostrar que o campo magnético possui importância dinâmica para PNM, sendo a componente turbulenta a maior responsável pela pressão magnética. / The Small Magellanic Cloud (SMC) is a gas rich irregular galaxy which, together with the Large Magellanic Cloud (LMC), orbit the Milky Way (MW). They form a triple system in constant interaction. The SMC is a metal poor galaxy and, due to this, its interstellar medium (ISM) presents different properties from the Galaxy\'s ISM. In addition to that, the importance of magnetic fields on galactic scales is being recognized nowadays. Therefore, the aim of this project was to study the magnetic field structure of the SMC and its relationship with other components of SMC\'s ISM. For this purpose we have used starlight optical polarimetric data, obtained at Cerro Tololo Inter-American Observatory. We have constructed a polarization catalog containing a total of 7,207 stars in 28 fields in the Northeast/Wing sections of the SMC. The polarimetric vector maps trace the ISM magnetic field component in the plane of the sky and one can estimate its intensity towards a given region using the Chandrasekhar & Fermi method. Making use of the polarimetric catalog from this work, we have found that the magnetic field in the SMC, although varying from region to region, nevertheless shows two large scale patterns - the first one aligned with the Magellanic Bridge and a second one aligned with the SMC\'s Bar. We derived for the regular sky-projected magnetic field a value of Bsky = (1.84 ± 0.11) uG, and for the turbulent magnetic field dB = (2.920 ± 0.098) uG. These results evidence that in the SMC the random field prevails over the large scale field, which explains the irregular configuration of the polarization vectors often seen. Correlating the polarization maps with structures present on the SMC\'s ISM, we could identify the presence of several shells which may have magnetic fields up to a few tens uG. It was also possible to observe environments where the regular field seems to have been destroyed due to turbulence, and others where it seems that the large scale magnetic field has not enough time to be formed. Studying the relationship with polarization and reddening, we have obtained a value for P/Av ~ 2, which may indicate that the polarization efficiency in the SMC is smaller than in the Galaxy, perhaps due to a higher turbulence and/or because of a smaller regular magnetic field. Lastly, we have estimated the energy density for the magnetic field and for the rotation and turbulent gas motions. We showed that the magnetic field is dynamically important in the SMC\'s ISM, and that the turbulent component is the largest contributor to the magnetic pressure.

Cette thèse propose des modèles cartographiques à grande échelle d'environnements urbains et ruraux à l'aide de données en 3D acquises par plusieurs robots. La mémoire contribue de deux manières principales au domaine de recherche de la cartographie. La première contribution est la création d'une nouvelle structure, CoMapping, qui permet de générer des cartes 3D de façon collaborative. Cette structure s’applique aux environnements extérieurs en ayant une approche décentralisée. La fonctionnalité de CoMapping comprend les éléments suivants : Tout d’abord, chaque robot réalise la construction d'une carte de son environnement sous forme de nuage de points.Pour cela, le système de cartographie a été mis en place sur des ordinateurs dédiés à chaque voiture, en traitant les mesures de distance à partir d'un LiDAR 3D se déplaçant en six degrés de liberté (6-DOF). Ensuite, les robots partagent leurs cartes locales et fusionnent individuellement les nuages de points afin d'améliorer leur estimation de leur cartographie locale. La deuxième contribution clé est le groupe de métriques qui permettent d'analyser les processus de fusion et de partage de cartes entre les robots. Nous présentons des résultats expérimentaux en vue de valider la structure CoMapping et ses métriques. Tous les tests ont été réalisés dans des environnements extérieurs urbains du campus de l’École Centrale de Nantes ainsi que dans des milieux ruraux. / This thesis proposes large-scale mapping model of urban and rural environments using 3D data acquired by several robots. The work contributes in two main ways to the research field of mapping. The first contribution is the creation of a new framework, CoMapping, which allows to generate 3D maps in a cooperative way. This framework applies to outdoor environments with a decentralized approach. The CoMapping's functionality includes the following elements: First of all, each robot builds a map of its environment in point cloud format.To do this, the mapping system was set up on computers dedicated to each vehicle, processing distance measurements from a 3D LiDAR moving in six degrees of freedom (6-DOF). Then, the robots share their local maps and merge the point clouds individually to improve their local map estimation. The second key contribution is the group of metrics that allow to analyze the merging and card sharing processes between robots. We present experimental results to validate the CoMapping framework with their respective metrics. All tests were carried out in urban outdoor environments on the surrounding campus of the École Centrale de Nantes as well as in rural areas.

Ziel dieser Masterarbeit ist die Untersuchung neuartiger Prägeformkonzepte hinsichtlich ihres Prägeverhaltens. Die Konzepte weisen lokal unterschiedliche Materialeigenschaften auf, die zu einer verbesserten Ausprägung von Karton führen sollen. Die Konzepte sollen anhand der Prägeergebnisse und der Abformgenauigkeit evaluiert werden. Dabei ist ein weiteres Ziel der Arbeit, Methoden zur Quantifizierung der Abformgenauigkeit zu finden. Die Herstellung der Konzepte erfolgt mithilfe eines additiven Fertigungssystems, welches mehrere Materialien in einem Bauvorgang verarbeiten kann. Zur Datengewinnung werden Oberflächenscans der geprägten Kartonproben und Werkzeuge durchgeführt. Auf Grundlage dieser Scans werden drei Methoden zur Ermittlung der Abformgenauigkeit vorgeschlagen. Abschließend werden die Werkzeuge anhand der Prägeergebnisse und der ermittelten Abformgenauigkeit bewertet. Weiterhin werden die vorgeschlagenen Methoden miteinander verglichen und deren Vor- und Nachteile diskutiert. Dies gibt Auskunft darüber, unter welchen Bedingungen der Einsatz welcher Methode sinnvoll erscheint.:1. Einleitung 2. Theoretische Grundlagen 2.1 Umformprozesse 2.1.1 Prägen von Faserwerkstoffen 2.1.2 Einsatz von Niederhaltern beim Umformen von Blechen 2.1.2.1 Tiefenziehen 2.1.2.2 Tiefen 2.1.3 Einsatz von Niederhaltern beim Umformen von Karton 2.1.3.1 Ziehen und Pressformen 2.1.3.2 Hydroformen 2.2 Multi-Material-Verarbeitung in der additiven Fertigung 2.2.1 Materialextrusion 2.2.2 Badbasierte Photopolymerisation 2.2.3 Material Jetting 2.2.4 Pulverbettbasiertes Schmelzen 2.2.5 Workflow und Datenvorbereitung 2.3.6 Geeignete Dateiformate 2.3 Soll-Ist-Vergleich von 2.5D-Oberflächendaten 2.3.1 Berechnung von Flächeninhalten und Volumen 2.3.2 Registrierung und Abstandsberechnung von Punktwolken 3. Versuche und Messungen 3.1 Herstellung der Prägeformkonzepte 3.1.1 Beschreibung der Konzepte 3.1.2 Fertigungstechnologie und Materialwahl 3.1.3 Datenvorbereitung für die Polyjet-Fertigung 3.2 Prägeversuche und Datenverarbeitung 3.2.1 Prägeversuche 3.2.2 Oberflächenscan am Keyence 3D-Makroskop 3.3 Ermittlung der Abformgenauigkeit 3.3.1 Flächen- und Volumenberechnung in MatLab & CloudCompare 3.3.2 Abformgenauigkeit nach ICP-Algorithmus & Abstandsberechnung 4. Ergebnisse und Diskussion 4.1 Betrachtung der Prägewerkzeuge 4.2 Betrachtung der Kartonprägungen 4.2.1 Prägeergebnisse nach Flächeninhalt der Profilschnitte 4.2.2 Einfluss der Faserlaufrichtung auf Kartonprägungen 4.2.3 Prägeergebnisse nach Volumen der Punktwolken 4.3 Betrachtung der Abformgenauigkeit 4.3.1 Abformgenauigkeit nach Flächeninhalt & Volumen 4.3.2 Abformgenauigkeit nach ICP-Algorithmus & Abstandsberechnung 4.4 Bewertung der Methoden zur Ermittlung der Abformgenauigkeit 4.5 Beurteilung des Bedienereinflusses bei der Datenverarbeitung am Keyence 5. Zusammenfassung und Ausblick Literaturverzeichnis Eidesstattliche Erklärung / The aim of this master thesis is to investigate novel embossing die concepts with regard to their embossing behavior. The concepts have locally different material properties, which should lead to an improved embossing of cardboard. The concepts are to be evaluated on the basis of the embossing results and the impression accuracy. A further aim of the work is to find methods for quantifying the impression accuracy. The concepts will be manufactured using an additive manufacturing system that can process multiple materials in a single build process. Surface scans of the embossed cardboard samples and tools are performed to obtain data. Based on these scans, three methods are proposed to determine the impression accuracy. Finally, the tools are evaluated based on the embossing results and the determined impression accuracy. Furthermore, the proposed methods are compared with each other and their advantages and disadvantages are discussed. This provides information on the conditions under which the use of which method appears to be sensible.:1. Einleitung 2. Theoretische Grundlagen 2.1 Umformprozesse 2.1.1 Prägen von Faserwerkstoffen 2.1.2 Einsatz von Niederhaltern beim Umformen von Blechen 2.1.2.1 Tiefenziehen 2.1.2.2 Tiefen 2.1.3 Einsatz von Niederhaltern beim Umformen von Karton 2.1.3.1 Ziehen und Pressformen 2.1.3.2 Hydroformen 2.2 Multi-Material-Verarbeitung in der additiven Fertigung 2.2.1 Materialextrusion 2.2.2 Badbasierte Photopolymerisation 2.2.3 Material Jetting 2.2.4 Pulverbettbasiertes Schmelzen 2.2.5 Workflow und Datenvorbereitung 2.3.6 Geeignete Dateiformate 2.3 Soll-Ist-Vergleich von 2.5D-Oberflächendaten 2.3.1 Berechnung von Flächeninhalten und Volumen 2.3.2 Registrierung und Abstandsberechnung von Punktwolken 3. Versuche und Messungen 3.1 Herstellung der Prägeformkonzepte 3.1.1 Beschreibung der Konzepte 3.1.2 Fertigungstechnologie und Materialwahl 3.1.3 Datenvorbereitung für die Polyjet-Fertigung 3.2 Prägeversuche und Datenverarbeitung 3.2.1 Prägeversuche 3.2.2 Oberflächenscan am Keyence 3D-Makroskop 3.3 Ermittlung der Abformgenauigkeit 3.3.1 Flächen- und Volumenberechnung in MatLab & CloudCompare 3.3.2 Abformgenauigkeit nach ICP-Algorithmus & Abstandsberechnung 4. Ergebnisse und Diskussion 4.1 Betrachtung der Prägewerkzeuge 4.2 Betrachtung der Kartonprägungen 4.2.1 Prägeergebnisse nach Flächeninhalt der Profilschnitte 4.2.2 Einfluss der Faserlaufrichtung auf Kartonprägungen 4.2.3 Prägeergebnisse nach Volumen der Punktwolken 4.3 Betrachtung der Abformgenauigkeit 4.3.1 Abformgenauigkeit nach Flächeninhalt & Volumen 4.3.2 Abformgenauigkeit nach ICP-Algorithmus & Abstandsberechnung 4.4 Bewertung der Methoden zur Ermittlung der Abformgenauigkeit 4.5 Beurteilung des Bedienereinflusses bei der Datenverarbeitung am Keyence 5. Zusammenfassung und Ausblick Literaturverzeichnis Eidesstattliche Erklärung

Die Eisbildung in Wolken wirkt sich auf die Niederschlagsbildung, die optischen Eigenschaften, und die Persistenz der Wolken aus und beeinflusst somit das Wetter und das Klima. Sogenannte eisnukleierende Partikel (ice nucleating particle; INP), katalysieren den Gefrierprozess von Wolkentröpfchen und tragen so zur primären Eisbildung in Wolken bei. In dieser Arbeit wurden die Häufigkeit und die Eigenschaften von INP in der Arktis untersucht. Hierzu wurde ein Vielzahl an Proben analysiert: Proben zweier Eisbohrkerne (aus Spitzbergen und Grönland); Filterproben von Aerosolpartikeln, die an Bord eines Flugzeuges über dem arktischen Ozean nordöstlich von Grönland gesammelt wurden; Filterproben von Aerosolpartikeln, die an Bord eines Schiffes in der Nähe von Spitzbergen gesammelt wurden. Zusätzlich wurden auch Meeresoberflächenfilm-, Meerwasser- und Nebelwasserproben gesammelt. Es wurde festgestellt, dass die INP-Konzentrationen in der Arktis im Allgemeinen niedriger sind als in den mittleren Breiten. Und obwohl die INP-Konzentrationen bei einer Temperatur von Probe zu Probe eine hohe Variabilität aufweisen, bewegen sie sich seit der Kleinen Eiszeit im 16. Jahrhundert auf einem ähnlichen Niveau und zeigen keinen langfristigen Trend. Außergewöhnlich eisaktive Proben zeichnen sich durch hohe INP-Konzentrationen bei wärmeren Temperaturen (ca. über -15°C) aus. Die in diesen Fällen aktiven INP können auf einen biogenen Ursprung zurückgeführt werden. Ferner wurden eindeutige Hinweise auf das Vorhandensein lokaler mariner INP-Quellen gefunden in der Arktis gefunden. Dies ist ein interessantes Ergebnis, da auch gezeigt wurde, dass ohne signifikante Anreicherung während des Transfers vom Ozean in die Aerosolphase, die vorhandenen INP im Meerwasser die INP-Konzentration in der Luft nicht erklären können. Die INP-Konzentrationen Temperaturbereich unterhalb von -26°C, hingegen scheinen eher durch Ferntransport von Staub aus den mittleren Breiten und/oder terrestrischer Quellen in der Arktis bestimmt zu sein.:1 Introduction 2 Experimental 2.1 Campaign Overviews 2.1.1 Arctic Ice Cores 2.1.2 PAMARCMiP 2.1.3 PASCAL 2.2 Instrumentation 2.2.1 Droplet Freezing Assays 2.2.2 HERA 2.2.3 Low Volume Filter Sampler 2.2.4 SPIN 2.2.5 Sea and fog water sampling 2.2.6 Other Aerosol Instrumentation 2.3 Data analysis 2.3.1 INP concentration 2.3.2 Back trajectories 2.3.3 Sea ice fraction and thickness 2.3.4 Transmission Electron Microscopy 3 Results 3.1 INP measurements on Arctic ice core samples 3.1.1 Results & Discussion 3.1.2 Summary 3.2 Airborne INP measurements during PAMARCMiP 3.2.1 Results & Discussion 3.2.2 Summary 3.3 Ship-borne INP measurements during PASCAL 3.3.1 Results & Discussion 3.3.2 Summary 4 Summary and Conclusion / Ice formation in clouds impacts precipitation initiation, cloud optical properties, and cloud persistence, and hence influences weather and climate. At the base of the primary ice formation in clouds stands the ice nucleating particle (INP), which catalyzes the freezing process of cloud droplets. In this thesis, the abundance and properties of Arctic INP were investigated in samples from two ice cores (Svalbard and Greenland), in samples of aerosol particles collected on an aircraft over the Arctic ocean northeast of Greenland, and in ship-borne aerosol filter samples, as well as sea surface microlayer, bulk sea water and fog water samples collected in the vicinity of Svalbard. It was found that INP concentrations in Arctic are generally lower than in mid-latitudes. And while they show a high inter-sample variability, INP concentrations have been on similar levels since the Little Ice Age in the 16th century and show no long-term trend. Exceptionally ice-active samples are characterized by high INP concentrations at warmer temperatures (approximately above -15°C). The INP active in these cases were attributed to a biogenic origin. Furthermore, clear evidence for the presence of local marine INP sources was found in the Arctic. This is an interesting finding as it was also shown that without significant enrichment during the transfer from the ocean to the aerosol phase, the INP in the sea water can not explain the INP concentration in the air. INP concentrations temperature range below -26°C, on the other hand, appear to be determined more by long-range transport of dust from mid-latitudes and/or terrestrial sources in the Arctic.:1 Introduction 2 Experimental 2.1 Campaign Overviews 2.1.1 Arctic Ice Cores 2.1.2 PAMARCMiP 2.1.3 PASCAL 2.2 Instrumentation 2.2.1 Droplet Freezing Assays 2.2.2 HERA 2.2.3 Low Volume Filter Sampler 2.2.4 SPIN 2.2.5 Sea and fog water sampling 2.2.6 Other Aerosol Instrumentation 2.3 Data analysis 2.3.1 INP concentration 2.3.2 Back trajectories 2.3.3 Sea ice fraction and thickness 2.3.4 Transmission Electron Microscopy 3 Results 3.1 INP measurements on Arctic ice core samples 3.1.1 Results & Discussion 3.1.2 Summary 3.2 Airborne INP measurements during PAMARCMiP 3.2.1 Results & Discussion 3.2.2 Summary 3.3 Ship-borne INP measurements during PASCAL 3.3.1 Results & Discussion 3.3.2 Summary 4 Summary and Conclusion