Sublimation experiments have been carried out to determine the effect of the mineral dust content of porous ices on the isotopic composition of the sublimate gas over medium (days to weeks) timescales. Whenever mineral dust of any kind was present, the D/H ratio of the sublimated gas was seen to decrease with time from the bulk ratio. Fractionations of up to 2.5 were observed for dust mixing ratios of 9 wt% and higher of JSC MARS-1 regolith simulant 1-10 mum crushed and sieved fraction. These favored the presence of the light isotope, H2O, in the gas phase. The more dust was added to the mixture, the more pronounced was this effect. Theoretical modeling of gas migration within the porous samples and adsorption on the excavated dust grains was undertaken to explain the results. Adsorption onto the dust grains is able to explain the low D/H ratios in the sublimate gas if adsorption favors retention of HDO over H2O. This leads to significant isotopic enrichment of HDO on the dust over time and depletion in the amount of HDO escaping the system as sublimate gas. This effect is significant for planetary bodies on which water moves mainly through the gas phase and a significant surface reservoir of dust may be found, such as on Comets and Mars. For each of these, inferences about the bulk water D/H ratio as inferred from gas phase measurements needs to be reassessed in light of the volatile cycling history of each body.PACS CODES:98.80.Ft Isotopes, abundances and evolution (astronomy)], 64.70.Hz Sublimation], 68.43.-h Adsorption at solid surfaces]

abstract: Jupiter’s moon Europa is an active target of research because of its unique geology and its potential for habitability. Europa’s icy chaos disrupts and transforms the previous terrain, suggesting melting is involved. Chaos occurs alongside several types of endogenic surface features. These microfeatures are under <100 km2 in area and include uplifts and domes, pits, spots, and hybrid features. The distribution of microfeatures is known in the ~10% of the Europa’s surface that are covered by the regional mosaics (“RegMaps”). The efforts to connect microfeature formation to any kind of heat transport in Europa are confounded because microfeatures are difficult to identify outside of RegMaps because of low image resolutions. Finding microfeatures outside of RegMaps would provide new observational constraints for microfeature formation models. First, I mapped microfeatures across four of Europa’s RegMaps and validated them against other mapping datasets. Microchaos features are the most numerous, followed by pits, domes, then hybrids. Spots are the least common features, and the smallest. Next, I mapped features in low-resolution images that covered the E15RegMap01 area to determine error rates and sources of omission or misclassification for features mapped in low-resolution images. Of all features originally mapped in the RegMap, pits and domes were the least likely to be re-mapped or positively identified (24.2% and 5%, respectively). Chaos, spots, and hybrids were accurately classified over 70% of the time. Quantitatively classifying these features using discriminant function analysis yielded comparable values of accuracy when compared to a human mapper. Finally, nearest-neighbor clustering analyses were used to show that pits are clustered in all regions, while chaos, domes, and hybrids vary in terms of their spatial clustering. This work suggests that the most likely processes for microfeature formations is either the evolution of liquid water sills within Europa’s ice shell or cryovolcanism. Future work extending to more areas outside of the RegMaps can further refine microfeature formation models. The detection of liquid water at or near the surface is a major goal of multiple upcoming Europa missions; this work provides predictions that can be directly tested by these missions to maximize their scientific return. / Dissertation/Thesis / Doctoral Dissertation Geological Sciences 2019

The solar wind interaction with an icy comet is studied through a model problem. A hybrid simulation is done of a box with evenly distributed water ions and protons, where initially the water ions are stationary, and protons move with the speed of the solar wind. The purpose of the thesis is to investigate the interaction between the two species through the convective electric field, and focus is on early acceleration of pick-up ions, and deflection of the solar wind. It is relevant to the cometary case, because it enables study of the physics of this interaction, without involving other mechanisms, such as bow shock, magnetic field pile-up and draping. The species are found to exchange kinetic energy similar to a damped oscillator, where the dampening is caused by kinetic energy being transferred to the magnetic field. At early times, i.e. times smaller than the gyration time for the water ions, the solar wind does not lose much speed when it is deflected. For comparable number densities, the solar wind can be deflected more than 90° at early times, and loses more speed, and water ions are picked up faster. The total kinetic energy of the system decreases when energy builds up in the magnetic field. The nature of the energy exchange is strongly dependent on the number density ratio between water ions and protons. A density instability with behaviour similar to a plasma beam instability forms as energy in the magnetic field increases, and limits the amount of time the simulation preserves total energy, for the particular hybrid solver used. There is a discussion on the structure of the density instability, and it is compared to cometary simulations.

Submitted by Daniel Mathias Alves Pinto (poli372@hotmail.com) on 2015-01-13T16:50:47Z No. of bitstreams: 1 DESEMPENHO DOS FUNDOS DE INVESTIMENTO DE AÇÕES BRASILEIRO. UM ESTUDO DO PERÍODO DE 2000 a 2014.pdf: 2795101 bytes, checksum: ee7f73118bd8ebaf7cb32a2a7709b31e (MD5) / Approved for entry into archive by JOANA MARTORINI (joana.martorini@fgv.br) on 2015-01-13T17:13:56Z (GMT) No. of bitstreams: 1 DESEMPENHO DOS FUNDOS DE INVESTIMENTO DE AÇÕES BRASILEIRO. UM ESTUDO DO PERÍODO DE 2000 a 2014.pdf: 2795101 bytes, checksum: ee7f73118bd8ebaf7cb32a2a7709b31e (MD5) / Made available in DSpace on 2015-01-13T17:45:46Z (GMT). No. of bitstreams: 1 DESEMPENHO DOS FUNDOS DE INVESTIMENTO DE AÇÕES BRASILEIRO. UM ESTUDO DO PERÍODO DE 2000 a 2014.pdf: 2795101 bytes, checksum: ee7f73118bd8ebaf7cb32a2a7709b31e (MD5) Previous issue date: 2014-10-29 / The primary objective of this work is to answer if Brazilian equity funds were capable of creating value, as measured by Jensen’s alpha, during the selected period. After that it tried to identify the significate factors to value creation. Using the methodology developed by Jensen (1968), funds with significant alphas were separated from funds without them. The market portfolios used as benchmarks were Ibovespa and IBRx and the risk free rates were CDI, Selic and Account Savings (poupança). Regardless of the risk free rate or market portfolio, results obtained indicated that Brazilian equity mutual funds were not capable of generating alphas. Nevertheless, when compared with IBRx, mutual funds’ performance was even worse. After going through this process, a cross section regression was used to find the alpha generating significant variables, and the conclusion was that the larger the fund, the greatest the alpha it would generate. However, the older the fund and the higher the fees, the lower the alpha generated. Finally, for fund managers with positive significant alphas, risk was positively correlated with performance and for the ones with negative significant alphas, risk was negatively correlated with performance / O objetivo primário deste trabalho é verificar se os fundos de investimento em ações brasileiros criaram valor, medido pelo alpha de Jensen, dentro do período selecionado. Em seguida, busca-se identificar os fatores determinantes dessa criação de valor. Utilizando a metodologia desenvolvida por Jensen (1968), inicialmente foram separados os fundos que geram alphas significativos dos que não geram. Os benchmarks de mercado utilizados foram Ibovespa e IBRx e as taxas livres de risco foram Taxa Selic, CDI e Poupança. A conclusão foi que os fundos de ações brasileiros, nos períodos estudados, não foram capazes de gerar alpha, independentemente do benchmark ou da taxa livre de risco. No entanto, os resultados foram piores quando comparados com o IBRx. Após esse processo, foi utilizada uma regressão cross section para encontrar quais as variáveis significativas para geração de alpha. Concluiu-se que quanto maior o fundo, maior o alpha gerado. No entanto, quanto mais velho o fundo e quanto maior a taxa de administração menor será o alpha gerado. Por fim, para gestores que geram alphas positivos, cada unidade adicional de risco gera valor e, para gestores com alpha negativo, cada unidade adicional de risco destrói valor

abstract: The Jovian moon Europa's putative subsurface ocean offers one of the closest astrobiological targets for future exploration. It’s geologically young surface with a wide array of surface features aligned with distinct surface composition suggests past/present geophysical activity with implications for habitability. In this body of work, I propose a hypothesis for material transport from the ocean towards the surface via a convecting ice-shell. Geodynamical modeling is used to perform numerical experiments on a two-phase water-ice system to test the hypotheses. From these models, I conclude that it is possible for trace oceanic chemistry, entrapped into the newly forming ice at the ice-ocean phase interface, to reach near-surface. This new ice is advected across the ice-shell and towards the surface affirming a dynamical possibility for material transport across the ice-ocean system, of significance to astrobiological prospecting. Next, I use these self-consistent ice-ocean models to study the thickening of ice-shell over time. Europa is subject to the immense gravity field of Jupiter that generates tidal heating within the moon. Analysis of cases with uniform and localized internal tidal heating reveal that as the ice-shell grows from a warm initial ocean, there is an increase in the size of convection cells which causes a dramatic increase in the growth rate of the ice-shell. Addition of sufficient amount of heat also results in an ice-shell at an equilibrium thickness. Localization of tidal heating as a function of viscosity controls the equilibrium thickness. These models are then used to understand how compositional heterogeneity can be created in a growing ice-shell. Impurities (e.g. salts on the surface) that enter the ice-shell get trapped in the thickening ice-shell by freezing. I show the distribution pattern of heterogeneities that can form within the ice-shell at different times. This may be of potential application in identifying the longevity and mobility of brine pockets in Europa's ice-shell which are thought to be potential habitable niches. / Dissertation/Thesis / Doctoral Dissertation Geological Sciences 2017

This thesis presents an evaluation of the proposals and optimizing inventory management at ICE invest spol. s r.o. The theoretical part defines basic concepts regarding this issue, their classification and types of inventory control methods. It also describes the impact of each solution on the costs associated with them. The practical part analyzes the current state of inventory management in the company is also interested in the process of procuring, storing supplies and distribute them to individual branches. The aim of this analysis is to identify weaknesses and fix them with the best solutions that will lead to improvements in inventory management company.

La majeure partie de mon travail de thèse a porté sur l’étude de la composition chimique de la surface d’Europe. Afin d’apporter une plus-value par rapport aux résultats de l’instrument NIMS à bord de la sonde Galileo qui orbita dans le système jovien de 1995 à 2003, une campagne d’observations depuis le sol a été menée avec le spectromètre imageur infra-rouge SINFONI au VLT. Cinq observations en optique adaptative possédant une résolution spatiale d’environ 160 km et une résolution spectrale R=1500 dans le proche infra-rouge furent acquises. Une procédure complexe de réduction des données a été mise en place afin de construire un cube hyperspectral global en réflectance de la surface. La modélisation linéaire de chacun des spectres du cube a permis d’aboutir aux premières cartes d’abondances absolues jamais obtenues pour la surface d’Europe. Ces cartes confirment la présence des deux espèces majoritaires, la glace d’eau et l’acide sulfurique hydraté. La distribution de l’acide sulfurique est centrée sur l’hémisphère orbital arrière qui est préférentiellement impacté par un flux d’ions de soufre originaires du tore de plasma produit par l’activité volcanique d’Io. Cependant, deux résultats inattendus ont été obtenus. Le premier concerne la glace d’eau, dont la forme cristalline est près de deux fois plus abondante que la forme amorphe selon les résultats de la modélisation. Ce résultat, surprenant compte tenu du taux d’irradiation très élevé auquel la surface est soumise, pourrait s’expliquer par l’existence d’un fort gradient de cristallinité au sein de la couche de glace, mais aussi par l’existence d’une activité endogène relativement soutenue qui se traduit visuellement par une surface peu cratérisée, donc jeune. La corrélation entre la distribution des grains cristallins et la géomorphologie semble accréditer la seconde hypothèse. Le second résultat concerne la détection de sels chlorés à partir de la modélisation des spectres hautement résolus de SINFONI, et non de sulfates, remettant en cause les détections marginales annoncées par les observations de l’instrument NIMS/Galileo. La distribution des sels chlorés, tout comme celle de la glace d’eau cristalline, est corrélée à la géomorphologie, ce qui confirme le rôle important des apports endogènes. Des processus tectoniques et cryovolcaniques mis en évidence récemment pourraient être à l’origine de cette distribution. L’autre versant de ma thèse a été consacré aux caractéristiques physiques des grains cométaires de 67P/C-G. L’instrument COSIMA embarqué sur l’orbiter de la sonde Rosetta a permis la collecte, l'imagerie et l'analyse chimique élémentaire des grains présents dans l’environnement proche de 67P/C-G. Une approche automatisée de la détection des grains à partir des images prises par la caméra « COSISCOPE » a été mise en place et a permis de détecter environ 35000 grains ayant une surface de plus de 100 µm2 entre août 2014 et mai 2016. La résolution de 13.7 µm/pixel a rendu possible la caractérisation en détail de la forme et de la structure des grains, et le nombre important de détections a permis d’obtenir des statistiques robustes concernant la distribution en taille et l’évolution de celle-ci au cours du temps. Deux grandes familles de grains ont été identifiées : les grains compacts, qui ne représentent qu’une faible minorité des grains et qui ont été majoritairement collectés en début de mission, et les agrégats, qui ont une structure très poreuse similaire à celle des IDPs et des micrométéorites collectées en Antarctique. La distribution en taille obtenue suit une loi de puissance intégrale en r-2.66. La comparaison avec des lois obtenues à des échelles différentes par d’autres instruments met en évidence des différences qui peuvent être interprétées par des mécanismes d’éjection dépendant de la taille associés à un biais du processus de collecte en orbite. / The major part of my work focused on the study of the chemical composition of Europa’s surface. In order to provide additional insights in comparison to the results of the NIMS instrument onboard the Galileo spacecraft that orbited in the Jovian system from 1995 to 2003, a ground-based observations campaign was conducted with the infrared imaging spectrometer SINFONI on the VLT. Several observations using adaptive optics with a spatial resolution of about 160 km and a spectral resolution R = 1500 in the near-infrared were acquired and then combined. A specific data reduction pipeline was developed to build a global hyperspectral cube in surface reflectance. The linear modeling of each spectra of this cube leads to the first global abundance maps ever obtained for the surface of Europa. These maps confirm the presence of the two major species, namely water ice and hydrated sulfuric acid. The distribution of the hydrated sulfuric acid is centered on the trailing orbital hemisphere preferentially affected by a sulfur ion flux coming from the plasma torus produced by Io volcanic activity. Two surprising results were obtained. The first one concerns water ice, which crystalline form is about twice more abundant than the amorphous form according to the modeling results. This result, unexpected given the very high radiation rate on the surface, could be explained by a strong crystallinity gradient through the ice slab. However, it could also point out an endogenous activity possibly strong as first suggested by its poorly well-known cratered surface. The correlation between the crystalline grains distribution and the geomorphology seems in favor to the second hypothesis. The second result is related to the detection of chlorinated salts from the modeling of highly resolved spectra from SINFONI. Sulfates, first reported by several analyses of NIMS observations are marginal in the modeled composition, hence challenging their presence on the surface of Europa. The chloride distribution, as well as the one of the crystalline water ice, is correlated to geomorphology, potentially confirming significant endogenous contributions as the result of tectonic and cryovolcanic processes recently highlighted. The second part of my PhD was dedicated to the physical characteristics of the 67P/C-G’s cometary grains. The COSIMA instrument onboard the Rosetta orbiter allowed the collection, imaging and elemental chemical analysis of grains present in the immediate environment of 67P/C-G. An automated approach of the grains detection based on images taken by the camera "COSISCOPE" was set up and able to detect about 35.000 grains having an area of more than 100 µm² between August 2014 and May 2016. The resolution of 13.7 µm/pixel allowed to perform a detailed characterization of the shape and the structure of the grains, and the large number of detections permitted to obtain significant statistics on the size distribution and its evolution over the time. Two large families of grains have been identified: the compact grains, which represent only a small minority of grains mostly collected at the beginning of the mission, and aggregates, which have a very porous structure similar to those of IDPs and micrometeorites collected in Antarctica. The size distribution obtained follows an integrated power law in r-2.66. The comparison with the laws obtained at different scales by other instruments highlights differences that can be interpreted by ejection mechanisms depending on the size associated with a selection bias during the collection process in orbit.

The Kittlitz's murrelet (Brachyramphus brevirostris) is a species of conservation concern over the entirety of its known range, which spans coastal Alaska and northeastern Russia. Concerns about the status of the species have been raised due to evidence of population declines in key breeding areas, low reproductive output, and perceived threats to adult survival. A general lack of information related to vital rates and natural history for this species has hampered efforts to address potential threats and drivers of population decline. This thesis addresses the hypothesis that foraging conditions and nutritional stress may be related to the observed low reproductive output and apparent population declines. I used stable isotope analysis of Kittlitz's murrelet feathers and blood to assess foraging habits during four separate periods across the annual cycle. I also used stable isotope signatures (δ¹⁵N and δ¹³C) in feathers from museum specimens collected in southeastern Alaska during 1907–1984 to investigate potential long-term trends in food habits and foraging ecology. I found that δ¹⁵N progressively increased by 5‰ between the vernal pre-alternate molt and the autumnal pre-basic molt, equivalent to an increase of 1.5 trophic levels for assimilated prey, whereas seasonal patterns in δ¹³C suggest shifts in foraging habitat between breeding and non-breeding periods. These results indicate that the pre-breeding diet was comprised primarily of low trophic level prey from offshore habitats, such as macrozooplankton and/or larval fish. During the summer breeding season, Kittlitz's murrelets gradually switched to consuming higher proportions of planktivorous fish from nearshore habitats. By the post-breeding period, during the pre-basic molt, the diet was comprised almost exclusively of higher trophic level prey, presumably forage fish, from offshore habitats. Based on stable isotope signatures of murrelet feathers from museum specimens, these seasonal patterns were evident during the past century (1907-2009). δ¹³C in feathers grown during pre- and post-breeding (pre-alternate and pre-basic molts, respectively) became significantly more depleted over the last century, however, suggesting either a gradual change in diet and/or foraging habitat or a long-term shift in the isotopic composition of prey. I investigated potential energy constraints on reproduction in Kittlitz's murrelets by constructing a bioenergetics model to estimate energy budgets for breeding adult Kittlitz's murrelets under different scenarios of prey energy content and commuting distance between foraging areas and nest sites. Estimated field metabolic rate (FMR) of breeding Kittlitz's murrelets during the chick-rearing period exceeded the hypothetical maximum sustainable working capacity (MSWC; 4 times basal metabolic rate [BMR]) under empirically derived scenarios of prey energy content and commuting distance. This suggests that, under conditions of low energy content in available prey and/or long commuting distances to inland nest sites, Kittlitz's murrelets would be required to expend energy at a rate that, if maintained over an extended period, could be detrimental to subsequent adult survival and overall fitness. In addition, energy expenditure rates at the high end of the estimated range may exceed the rate at which food energy can be assimilated by adult murrelets. Metabolism of fat reserves, as indicated by mass loss during the breeding season, may be a partial, although limited, solution to periods of high energy demand for breeding adults. This thesis research is the first to indicate that Kittlitz's murrelets rely on distinctly different prey resources during different periods of the annual cycle. The previously unappreciated seasonal complexity of Kittlitz's murrelet foraging ecology offers a new perspective on potential factors limiting survival and reproduction in this species of conservation concern. In addition, my research suggests an adaptive explanation for the low breeding frequency and low reproductive output of Kittlitz's murrelets that is related to the exceptionally high energy expenditure rates required to raise young at nest sites as much as 70 km inland from the coast and up to 2,500 m above sea level. Because of their high level of reproductive effort, Kittlitz's murrelets may be more dependent on the high availability of high-lipid marine prey than other seabirds. / Graduation date: 2012

As an orbiter cruising to Jupiter will encounter different plasma environments, variety of spacecraft surface charging is expected. This surface potential can lead to inaccurate and wrong in-situ plasma measurements of on-board sensors, which explain the interest in simulating the charging.In this thesis the spacecraft-plasma interactions for a future mission to Jupiter are modelled with the help of the Spacecraft Plasma Interaction System, taking the case of a Jupiter Ganymede Orbiter (JGO) and a Jupiter Europa Orbiter (JEO) as an archetype for a future mission.It is shown that in solar wind at Earth and Jupiter, spacecraft potentials of about 8 V for the JEO, and 10 V to 11 V for the JGO are expected. Furthermore, at a distance of 15 Jupiter radii from Jupiter, the JGO is expected to charge to an electric potential of 2 V, except in the planetary shadow, where it will charge to a high negative potential of -40 V. Moreover, close to the orbit of Callisto, JGO will charge to 12 V in the sun and to 4.6 V in eclipse, due to a high secondary electron emission yield. / <p>Validerat; 20120115 (anonymous)</p>

The evolving science of astrobiology for the search for life beyond Earth has put focus on the possibility of subsurface bodies of liquid water beneath the surface of icy moons within our Solar System. Specifically, the Jovian moon of Europa and the Saturnian moon of Enceladus show telling characteristics of endogenous heating through their complex tidal resonances with their parent planets – suggesting the presence of oceans of liquid water and therefore a potential for astrobiology. Today, the planning of upcoming satellite missions to guarantee the identification of completely unknown, possibly habitable environments has become an intriguing task for space agencies worldwide. A method of guidance, ground-truthing, debugging and testing of the viability of planned satellite missions is to utilize relatively accessible analogue environments on the Earth. Fortunately, the research of Antarctic subglacial water environments has been acknowledged as the most suitable analogues to the environments of Europa and Enceladus. Given its recorded motions of ice dynamics, erosion, complex thermal systems, and occasions of sampled microbes within – these sensitive, exotic environments beneath the Antarctic ice bed are currently assessed for their suitability as habitats for extremophilic microorganisms, which may provide important insights into the potential existence of habitats, perhaps even life, on icy moons. Ultimately, viable lessons can be drawn from the research of Antarctic subglacial environments given the uncovering of reliable sanitary methodologies that are going to be required during future approaches and sampling of natural systems of extraterrestrial subglacial environments in order to minimize irreparable anthropogenic disturbances on any potential astrobiology. Regardless of the question if the future investigation of Europa’s and Enceladus environments is going to reveal astrobiology within beneath their icy surfaces; this investigation is going to be of invaluable information for the improving familiarity of physical systems beyond Earth. / Sedan länge har forskare vetat att flytande/rinnande vatten är en av de viktigaste förutsättningar för allt liv på Jorden. Under de senaste decennierna har frågan om liv på Jupiters måne Europa, och Saturnus måne Enceladus aktualiserats, efter upptäckten av frusna islager på deras månytor. Evidens från respektive månars omloppsbanor, gör att forskare idag tror att månarnas djupa islager hettas upp inifrån av en aktiv, inre geologi, vilket i sin tur kan tyda på större mängder av flytande vatten. I och med omvandlingen av is till flytande vatten, får detta forskare att tro att cirkulationen av vatten, ihop med den aktiva geologin, möjligtvis har skapat och upprätthåller beboliga förutsättningar för mikroskopiskt liv. I dagsläget planeras ett flertal satelliter skjutas upp till månarna med uppdrag att bekräfta fallet om flytande vatten och beboliga miljöer på månarna, och därmed även undersöka frågan om månarna möjligtvis bär på liv. På den frusna kontinenten Antarktis har ett flertal motsvarande subglaciala miljöer undersökts för att fastställa deras kvalifikationer att upprätthålla liv under extrema levnadsförhållanden. Under dessa undersökningar har ett flertal mikroorganismer påträffats i prover från iskärnor från två subglaciala sjöar (Vostoksjön och Whillanssjön), varav några blivit omstritt påstådda som inhemska extremofiler. Ifall detta stämmer, betyder det att de två subglaciala sjöarna underhålls av ett unikt samspel av drivande faktorer som upprätthåller de nödvändigaste levnadsförutsättningarna för att mikroorganismer kan överleva, även frodas i uppenbart extrema miljöförhållanden. Med forskningen av Antarktis subglaciala sjöar som rapporterar ett unikt samspel mellan is, vatten och underliggande geologi; kan den fortsatta fastställningen av detta fysiska samspel, samt vidare identifikationer av inhemska mikroorganismer att bli en viktig lärdom för framtida satelliters datainsamling av subglaciala vattenmiljöer på Europa och Enceladus. För att underlätta och effektivisera sökandet efter potentiella livsmiljöer, samt möjligtvis hitta utomjordiskt liv på isiga månar bör framtidens satellituppdrag dra stor lärdom och väga in de erfarenheter och resultat som gjorts på subglaciala sjöar i Antarktis.