Esta dissertação objetiva investigar a evolução geomorfológica dos ambientes proglaciais (geleiras Ecology, Sphinx, Baranowski, Tower e Windy) da margem leste do campo de gelo Warszawa (62°12’0” S - 58°30’0” W) na Ilha Rei George, Antártica, entre 1956 - 2017. Dados obtidos por sensores remotos, como Aster GDEM2, imagens Sentinel-2 (2017) e WorldView-2 (2014), possibilitaram o mapeamento geomorfológico das formas de relevo de mesoescala proglaciais. A variação frontal e de área total das geleiras foi estimada e mapeada com dados de imagens de satélite (Sentinel-2 de 2017 e WorldView-2 de 2014) e vetores de variação frontal de 1956, 1979, 1988 e 2000. Evidenciou-se um contínuo processo de retração nas geleiras Ecology, Sphinx, Baranowski, Tower e Windy, com perda total de área de 33%, 25%, 37%, 71% e 30%, respectivamente, no período. A geleira Windy apresentou mudanças recentes em seu término de maré para terrestre, formando uma área proglacial com a exposição de formas de relevo deposicionais glaciais. Estimou-se um aumento das áreas livres de gelo de 6,3km² no período entre 1956-2017. Em resposta ao processo de retração glacial, há exposição de formas de relevo nos ambientes livres de gelo na área de estudo com a formação da rede de drenagem fluvioglacial e glaciolacustre e a formação de ambientes proglaciais com exposição de morainas laterais, frontais, latero-frontais e eskers. As áreas livres de gelo recentes são suscetíveis a processos de retrabalhamento por ação gravitacional, eólica e pluvial. Foram determinados três estágios de evolução do ambiente proglacial das geleiras associadas às feições geomorfológicas geradas em cada fase. Como mudança ambiental detectada está a sucessão de ambientes proglaciais, paraglaciais e periglaciais. / This dissertation aims to investigate the proglacial geomorphological evolution (Ecology, Sphinx, Baranowski, Tower and Windy glaciers) in the western sector of Warszawa Ice Cap (62°12’0” S 58° 30’ 0” W), Admiralty Bay coast, King George Island, Antarctica between 1956 and 2017. Data obtained by remote sensors, such as Aster GDEM2, Sentinel-2 (2017) and WorldView-2 (2014) images, were applied in geomorphological mapping of the proglacial mesoscale landforms. Glacial retreat and fluctuations of glaciers areas were estimated (using Sentinel-2 images, acquired in 2017, WorldView-2 data, acquired in 2014, and outline data of the 1956, 1979, 1988 and 2000). The results evidenced the continuous retreat processes in period for Ecology, Sphinx, Baranowski, Tower and Windy glaciers, with of 33%, 25%, 37%, 71% and 30% of the area lost, respectively. The Windy glacier changed of outlet glacier for land terminus conditions in latest decades, with a recent proglacial environment development. In response to glacial retreat processes there is a glacial landforms exposition in new ice-free environments in the study area. Was recorded an increase of the 6.3km² in ice-free land areas between 1956 and 2017 in in the western sector of Warszawa Ice Cap. As response the retreat processes there are the development of the glacio-fluvial drainage network, glacio-lacustrine landforms and the formation of proglacial ice marginal environments with lateral moraines, lateral-frontal moraines, frontal moraines, eskers. Recent ice-free areas are susceptible to gravitational, wind and pluvial reworking process. Three stages of evolution of the proglacial environments of the glaciers associated with the geomorphological features formed in each phase and environmental changes in response the glacier retreat was determined. Was detected the succession of proglacial for paraglacial and periglacial environments as evidence of the environmental change.

Thin-film solar cells based on an absorber layer of chalcogenide compounds (CIGS, CdTe) are today among the most promising photovoltaic technologies due to their long-term ability to gain a foothold in mass commercial production as an alternative to conventional Si solar cells. Despite this success, the physical origin of the defects present in the thin films are still insufficiently elucidated, especially in the compounds of the chalcopyrite family Cu(In_{1x},Ga_{x})(S_{y},Se_{1y})_{2}. The research focuses on the identification and analysis of microstructural defects responsible for the electrical instability of chalcopyrite-based thin-film solar cells with a typical heterostructure arrangement ZnO:Al/i-ZnO/CdS/Cu(In,Ga)Se_{2}/Mo. The non-uniform polycrystalline nature of semiconductor materials in this complex multilayer structure requires a comprehensive analysis of electro-optical, structural and compositional properties associated with the actual morphology at the macroscopic, microscopic or even nanoscopic level. The observed predominant ohmic or non-ohmic current conduction in the dark transport characteristics was also reflected in the slope deviations of the excessive noise fluctuations, which were in the spectral domain exclusively in the form of flicker noise with dependency S_{i} ~ f^{1}. Spatially resolved electroluminescence based on stimulated photon emission by charge carriers injecting into the depletion region, not only showed a significantly inhomogeneous distribution of intensity in planar heterojunction under forward bias, but also revealed light emitting local spots in reverse bias due to a trap-assisted radiative recombination through the high density of defect states. Microscopic examination of the defect-related light emitting spots revealed rather extensive defective complexes with many interruptions through the layers, especially at the heterojunction CdS/Cu(In,Ga)Se_{2} interface. Besides, the high leakage current via these defective complexes subsequently led to a considerable local overheating, which caused a clearly observable structural and morphological changes, such as deviations in absorber layer stoichiometry due to Cu–In–Ga–Se segregation, Cu-rich and Ga-rich grains formation with an occurrence of Se-poor or Cu_{x}Se_{y} secondary phases regions, material redeposition accompanied by evaporation of ZnO:Al/i-ZnO/CdS layers together with the formation of Se structures on the surface around the defects. Within the research, analytical modelling of transport characteristics was implemented with parameters extraction of individual transport mechanisms to understand the non-ohmic shunt behaviour due to leakage current. In addition to the proper current path along the main heterojunction, the proposed model contains parasitic current pathways as a consequence of recombination-dominated charge transport or current conduction facilitated by multi-step tunnelling via high density of mid-gap defect states in the depletion region, ohmic leakage current caused by pinholes or low-resistance paths along grain boundaries in Cu(In,Ga)Se_{2}, or space-charge limited current due to metals diffusion from the ZnO:Al layer and grid Ag contacts through disruptions in i-ZnO/CdS layers.

Abstract The Cassini/Huygens mission is a collaborative mission of NASA and ESA to study the Saturnian system. Cassini Plasma Spectrometer (CAPS)is one of the scientific investigations onboard the Cassini orbiter. It consists of three separate spectrometers: Electron Spectrometer (ELS), Ion Mass Spectrometer (IMS) and Ion Beam Spectrometer (IBS). The University of Oulu has a co-investigator status in the CAPS project, and been mainly involved in simulating the structure and scientific performance of the IBS instrument. IBS is a high resolution hemispherical electrostatic analyser aimed to study the solar wind ions. This thesis contains an Introduction and five original papers. Papers I–III contain a detailed description of the simulation process of the IBS instrument and related results. In Paper I the manufacturing tolerances were calculated in order to verify that the high resolution requirements can be achieved using available manufacturing processes. In Paper II the simulations have been further developed and the instrument properties have been studied in more detail. In Paper III the simulation model is used to help the analysis and interpretation of the laboratory calibrations of the IBS flight model. Papers IV and V study the long-term fluctuations in solar wind and interplanetary magnetic field in the period range of 1–2 years (so called mid-term quasi periodicities, MTQP), using the wavelet transformation method to produce dynamic power spectra. In paper IV the MTQP structure in solar wind speed at 1 AU was studied using the longest available series of geomagnetic activity. It was shown that the long-term occurrence MTQP fluctuations roughly follows the long-term solar activity, suggesting that MTQP fluctuations are closely connected with the solar dynamo activity. Moreover, it was also noted that MTQP activity may offer a possibility for a precursory signal which could be used to predict significant changes in long-term solar activity. While Paper IV presents the temporally longest study of MTQP fluctuations, Paper V gives the spatially widest treatment of the same phenomenon. Paper V studies MTQP fluctuations in solar wind and interplanetary magnetic field measured by four probes in the outer heliosphere. It is shown that two MTQP fluctuations of different periods (1.3 and 1.7 years)co existed during solar cycle 22, while during solar cycle 21 only the 1.7-year band existed. This suggests that the solar dynamo acts differently during even and odd cycles. It is also shown that the two MTQP fluctuations during solar cycle 22 are organized latitudinally. While the 1.3-year periodicity originates from equatorial regions, the 1.7-year fluctuations arise at mid-latitudes. / Original papers Original papers are not included in the electronic version of the dissertation. Vilppola, J. H., Keisala, J. T., Tanskanen, P. J., & Huomo, H. (1993). Optimization of hemispherical electrostatic analyzer manufacturing with respect to resolution requirements. Review of Scientific Instruments, 64(8), 2190–2194. https://doi.org/10.1063/1.1143958 Vilppola, J. H., Tanskanen, P. J., Huomo, H., & Barraclough, B. L. (1996). Simulations of the response function of a plasma ion beam spectrometer for the Cassini mission to Saturn. Review of Scientific Instruments, 67(4), 1494–1501. https://doi.org/10.1063/1.1146881 Vilppola, J. H., Tanskanen, P. J., Barraclough, B. L., & McComas, D. J. (2001). Comparison between simulations and calibrations of a high resolution electrostatic analyzer. Review of Scientific Instruments, 72(9), 3662–3669. https://doi.org/10.1063/1.1392337 Mursula, K., Zieger, B., & Vilppola, J. H. (2003). Mid-term quasi-periodicities in geomagnetic activity during last 15 solar cycles: Connection to solar dynamo strength. Solar Physics, 212(1), 201–207. https://doi.org/10.1023/a:1022980029618 Mursula, K., & Vilppola, J. H. (2004). Fluctuations of the Solar Dynamo Observed in the Solar Wind and Interplanetary Magnetic Field at 1 AU and in the Outer Heliosphere. Solar Physics, 221(2), 337–349. https://doi.org/10.1023/b:sola.0000035053.17913.26

For this project, a historical statistical analysis of the Amplitude of Mass Fluctuations ($\sigma_8$) and Hubble's Constant ($H_0$) parameters in the Standard Cosmological Model was carried out to determine whether or not the given error bars truly represent the dispersion of values. It was found through analysis of the Chi-Squared ($\chi^2$) values of the data that for $\sigma_8$ (60 data points and $\chi^2$ between 183.167 and 189.037) that the associated probability Q is extremely low, with $Q = 1.5597*10^{-15}$ for the weighted average and $Q = 1.2107*10^{-14}$ for the best fit of the data. This was also the case for the $\chi^2$ values (163 data points and $\chi^2$ between 484.3977 and 575.655) of $H_0$, where $Q = 4.2176*10^{-34}$ for the linear fit of the data and $Q = 1.0342*10^{-47}$ for the weighted average of the data. Through further analysis, it is shown in question, a linear fit is a better estimate of the data than the weighted average. The general conclusion is that the statistical error bars have been underestimated (in around 20\% of the measurements), or the systematic errors were not properly taken into account.

Forecasting demand is one of the processes which greatly influences the decision making within a company, and it is also one of the greatest sources of uncertainty. Inaccurate forecasts force companies to find ways to compensate for the uncertainty, often by building inventories. On the other hand, accurate forecasts help companies to achieve better customer service and lower inventory levels. Cytiva is a global life science leader who manufactures high-technology laboratory instruments at their site in Umeå. To make sure that their transportation and storage spaces are sufficient, their down-stream suppliers require information about the quantity of the final products beforehand. But as of today, the company has inconsistent outbound inventory volumes. Thus, there is a great demand for increased visibility and predictability at the Umeå site’s outbound logistics. Further, Cytiva in Umeå bases their forecasting on manually calculated estimations which is both inefficient and can create errors due to human factors. These intrinsic information inconsistencies related to the outbound logistics is prone to creating bottlenecks in their overall supply chain. The main goal of this project is to increase the accuracy of these forecasts by developing a model. The outcome will be better estimations and clearer connection between the site in Umeå and the 3PL in Rosersberg. Additionaly, a good model makes the supply chain more efficient by creating better preconditions for managing the transportation and inventory at the receiving 3PL. To make forecasts for Cytiva’s outbound inventory, we chose to focus on two of the most common families of univariate time series models, namely the ARIMA and the Exponential Smoothing family. Based on these two families we have implemented, evaluated and compared six forecasting models. Initially, the modeling was done using daily observations in order to examine whether the models could improve the company’s demand for short forecast horizons. However, except for modeling on daily observations, we also widened the time interval by merging the observations into weeks to extend the modeling perspective even further. The results showed that the use of models can noticeably improve the estimations of the inventory and transportation spaces. We conclude that, among our models, the Holt-Winters using additive seasonality is the most optimal model when the forecasts are made on a daily time frequency, while the SARIMA model performs better on the weekly data.

Historically, studying the Martian ionosphere has been difficult due to the lack of dedicated instruments for electron density measurements in the orbit of Mars. However, since 2005, radio occultation measurements have been supplemented by Mars Express MARSIS remote sounder data and, more recently, by data from the MAVEN LPW Langmuir probe since 2014. The ionosphere of Mars is an interesting system, because Mars as one of the two solar system planetary bodies without an intrinsic magnetic field has highly localised crustal magnetic fields. The Chapman model describes the main layer of the ionosphere surprisingly well. Nevertheless, the crustal magnetic fields and other parameters potentially influence the ionosphere formation and topology. Combining the recent vast electron density data set, the Mars Global Surveyor crustal magnetic field map, and F10.7 solar radio flux measurements carried out at the Earth, a detailed study of the influence of these parameters can be conducted. To study the influence of these parameters as well as solar zenith angle on electron densities in the Martian ionosphere, we study magnitude of deviations from the established Chapman model. Furthermore, we use the Kolmogorov's 5/3 power law to investigate a possible dependence of its parameters characterising power and dissipation...

In the development of materials, the understanding of their properties is crucial. For magnetic materials, magnetism is an apparent property that needs to be accounted for. There are multiple factors explaining the phenomenon of magnetism, one being the effect of vibrations of the atoms on longitudinal spin fluctuations. This effect can be investigated by simulations, using density functional theory, and calculating energy landscapes. Through such simulations, the energy landscapes have been found to depend on the magnetic background and the positions of the atoms. However, when simulating a supercell of many atoms, to calculate energy landscapes for all atoms consumes many hours on the supercomputer. In this thesis, the possibility of using machine learning models to accelerate the approximation of energy landscapes is investigated. The material under investigation is body-centered cubic iron in the paramagnetic state at 1043 K. Machine learning enables statistical predictions to be made on new data based on patterns found in a previous set of data. Kernel ridge regression is used as the machine learning method. An important issue when training a machine learning model is the representation of the data in the so called descriptor (feature vector representation) or, more specific to this case, how the environment of an atom in a supercell is accounted for and represented properly. Four different descriptors are developed and compared to investigate which one yields the best result and why. Apart from comparing the descriptors, the results when using machine learning models are compared to when using other methods to approximate the energy landscapes. The machine learning models are also tested in a combined atomistic spin dynamics and ab initio molecular dynamics simulation (ASD-AIMD) where they were used to approximate energy landscapes and, from that, magnetic moment magnitudes at 1043 K. The results of these simulations are compared to the results from two other cases: one where the magnetic moment magnitudes are set to a constant value and one where they are set to their magnitudes at 0 K. From these investigations it is found that using machine learning methods to approximate the energy landscapes does, to a large degree, decrease the errors compared to the other approximation methods investigated. Some weaknesses of the respective descriptors were detected and if, in future work, these are accounted for, the errors have the potential of being lowered further.

京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第18060号 / 理博第3938号 / 新制||理||1567(附属図書館) / 30918 / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)教授 石田 憲二, 教授 前野 悦輝, 教授 松田 祐司 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DGAM

京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第20656号 / 理博第4321号 / 新制||理||1621(附属図書館) / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)教授 佐々木 節, 教授 田中 貴浩, 教授 川合 光 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第21247号 / 理博第4417号 / 新制||理||1634(附属図書館) / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)教授 石田 憲二, 教授 前野 悦輝, 教授 松田 祐司 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DGAM