The Evolution of Massive Young Stellar Objects in the Large Magellanic Cloud

This thesis presents an analysis of the largest catalog to date of infrared spectra of massive young stellar objects in the Large Magellanic Cloud. Evidenced by their very different spectral features, the luminous objects span a range of evolutionary states from those most embedded in their natal molecular material to those that have dissipated and ionized their surroundings to form compact HII regions and photodissociation regions. We quantify the contributions of the various spectral features using the statistical method of principal component analysis. Using this analysis, we classify the YSO spectra into several distinct groups based upon their dominant spectral features: silicate absorption (S Group), silicate absorption and fine-structure line emission (SE), polycyclic aromatic hydrocarbon (PAH) emission (P Group), PAH and fine-structure line emission (PE), and only fine-structure line emission (E). Based upon the relative numbers of sources in each category, we are able to estimate the amount of time massive YSOs spend in each evolutionary stage. We find that approximately 50% of the sources have ionic fine-structure lines, indicating that a compact HII region forms about half-way through the YSO lifetime probed in our study. Of the 277 YSOs we collected spectra for, 41 have ice absorption features, indicating they are surrounded by cold ice-bearing dust particles. We have decomposed the shape of the ice features to probe the composition and thermal history of the ice. We find that most the CO2 ice is embedded a polar ice matrix that has been thermally processed by the embedded YSO. The amount of thermal processing may be correlated with the luminosity of the YSO. Using the Australia Telescope Compact Array, we imaged the dense gas around a subsample of our sources in the HII complexes N44, N105, N113, and N159 using HCO+ and HCN as dense gas tracers. We find that the molecular material in star forming environments is highly clumpy, with clumps that range from subparsec to ~2 parsecs in size and with masses between 10^2 to 10^4 solar masses. We find that there are varying levels of star formation in the clumps, with the lower-mass clumps tending to be without massive YSOs. These YSO-less clumps could either represent an earlier stage of clump to the more massive YSO-bearing ones or clumps that will never form a massive star. Clumps with massive YSOs at their centers have masses larger than those with massive YSOs at their edges, and we suggest that the difference is evolutionary: edge YSO clumps are more advanced than those with YSOs at their centers. Clumps with YSOs at their edges may have had a significant fraction of their mass disrupted or destroyed by the forming massive star. We find that the strength of the silicate absorption seen in YSO IR spectra feature is well-correlated with the on-source HCO+ and HCN flux densities, such that the strength of the feature is indicative of the embeddedness of the YSO. We estimate that ~40% of the entire spectral sample has strong silicate absorption features, implying that the YSOs are embedded in circumstellar material for about 40% of the time probed in our study.

Desenvolvimento de um método para correção de curvas de desempenho em bombas centrífugas submersas operando com fluidos viscosos

Electrical Submersible Pump (ESP) is used as an artificial lift technique. However, pumping viscous oil is generally associated with low Reynolds number flows. This condition leads to a performance degradation respect to the performance expected from the regular operation with water that most of the centrifugal pumps are originally designed for. These issues are considered in this investigation through a numerical study of the flow in two different multistage, semi-axial type ESPs. This investigation is carried out numerically using a Computational Fluid Dynamics (CFD) package, where the transient RANS equations are solved numerically. The turbulence is modeled using the SST model. Head curves for several operating conditions are compared with manufacturer’s curves and experimental data for a three-stage ESP, showing good agreement for a wide range of fluid viscosities and rotational speeds. Dimensionless numbers (n, n, n e Re) are used to investigate performance degradation of the ESPs. In addition, flow phenomena through the impellers of the ESPs are investigated using flow field from numerical results. Results show that performance degradation is directly related to rotational Reynolds number, Re. In addition, it was verified that performance degradation occurs for constant normalized specific speedn, which shows that performance degradation occurs similarly for different centrifugal pumps. Moreover, experimental data and numerical results agreed with a correlation from literature between head and flow correction factors proposed by Stepanoff (1967). A definition of modified Reynolds number was proposed and relates the head correction factor to viscosity. A correlation between head correction factor and the modified Reynolds number was proposed, which agreed well with numerical and experimental data. Then, a method to predict performance degradation based on the previous correlations was proposed. This method was compared with others from literature. In general, results and conclusions from this work can also be useful to bring more information about the flow of highly viscous fluids in pumps, especially in semi-axial, multistage ESPs.

Analisi di mercato per pannelli fotovoltaici e cogeneratori

L'analisi di questa tesi si basa sui dati ottenuti contattando direttamente le aziende produttrici e/o di progettazione e riguarda due settori energetici: la cogenerazione e il solare fotovoltaico. Nel primo si sono studiate 60 unità complete di cogenerazione il cui studio si è basato sulla costruzione di grafici che mettono in relazione le potenze uscenti con il prezzo. Si è mostrato così la forte presenza di un fenomeno di economia di scala e la diversa ripartizione della potenza prodotta. Per unità di piccola-media potenza predomina la produzione di energia termica, la quale diminuisce la sua quota percentuale all’aumentare della taglia. Nel settore del solare fotovoltaico l’analisi è stata più diversificata e articolata. Si sono analizzati 70 pannelli di cui 35 monocristallini, 14 europei e 21 asiatici, e 35 policristallini, 26 europei e 9 asiatici, per i quali si sono graficati gli andamenti di resa, potenza specifica e costo specifico. I pannelli monocristallini, intrinsecamente più efficienti grazie al maggior grado di purezza, presentano un andamento crescente dei costi piuttosto ripido anche se non proporzionale con l’aumento delle prestazioni. Tra i pannelli policristallini invece si evidenzia l’assenza di un andamento nettamente crescente delle prestazioni all’aumentare dei costi. Confrontando i moduli divisi in base alla macro-regione di produzione si nota che l’Asia produce i pannelli al Si monocristallino più efficienti e più costosi mentre pannelli al Si policristallino più economici, ma con prestazioni in linea con quelli europei.Con i dati raccolti si è potuta svolgere anche una ristretta analisi sui pannelli al film sottile. Quelli che utilizzano il Si amorfo presentano prestazioni così basse da non permettere loro una vera affermazione sul mercato. Quest’ultima si presume che sarà invece possibile per pannelli basati su diversi materiali semiconduttori che presentano buoni livelli di prestazioni, ma prezzi ancora troppo elevati.

Quantizzazione in gauge di cono-luce di particelle e stringhe

In questa tesi si discute la formulazione di una teoria quantistica della dinamica libera di particelle e stringhe relativistiche. La dinamica relativistica viene costruita in entrambi i casi a partire dalla formulazione classica con invarianza di gauge della parametrizzazione di, rispettivamente, linee e fogli di mondo. Si scelgono poi condizioni di gauge-fixing dette di cono-luce. La teoria quantistica viene poi formulata usando le prescrizioni di quantizzazione canonica di Dirac.

Anioni: particelle identiche e topologia in meccanica quantistica

Si espone la teoria quantistica non relativistica dei sistemi di particelle identiche, costruendo un opportuno spazio delle configurazioni la cui struttura è coerente con la loro indistinguibilità. Si impiegano nozioni di topologia algebrica per la formulazione di una meccanica quantistica su tale spazio, mostrando che in due dimensioni spaziali esiste una continuità di statistiche quantistiche. Le particelle con queste statistiche intermedie tra bosoni e fermioni sono chiamate anioni. Si illustra l'importanza che hanno assunto nella spiegazione dell'effetto Hall quantistico e nell'attuale ricerca sulla possibilità di creare un computer quantistico topologico.

Modeling chemistry in massive star forming regions with internal PDRs

Over the past decades star formation has been a very attractive field because knowledge of star formation leads to a better understanding of the formation of planets and thus of our solar system but also of the evolution of galaxies. Conditions leading to the formation of high-mass stars are still under investigation but an evolutionary scenario has been proposed: As a cold pre-stellar core collapses under gravitational force, the medium warms up until it reaches a temperature of 100 K and enters the hot molecular core (HMC) phase. The forming central proto-star accretes materials, increasing its mass and luminosity and eventually it becomes sufficiently evolved to emit UV photons which irradiate the surrounding environment forming a hyper compact (HC) and then a ultracompact (UC) HII region. At this stage, a very dense and very thin internal photon-dominated region (PDR) forms between the HII region and the molecular core. Information on the chemistry allows to trace the physical processes occurring in these different phases of star formation. Formation and destruction routes of molecules are influenced by the environment as reaction rates depend on the temperature and radiation field. Therefore, chemistry also allows the determination of the evolutionary stage of astrophysical objects through the use of chemical models including the time evolution of the temperature and radiation field. Because HMCs host a very rich chemistry with high abundances of complex organic molecules (COMs), several astrochemical models have been developed to study the gas phase chemistry as well as grain chemistry in these regions. In addition to HMCs models, models of PDRs have also been developed to study in particular photo-chemistry. So far, few studies have investigated internal PDRs and only in the presence of outflows cavities. Thus, these unique regions around HC/UCHII regions remain to be examined thoroughly. My PhD thesis focuses on the spatio-temporal chemical evolution in HC/UC HII regions with internal PDRs as well as in HMCs. The purpose of this study is first to understand the impact and effects of the radiation field, usually very strong in these regions, on the chemistry. Secondly, the goal is to study the emission of various tracers of HC/UCHII regions and compare it with HMCs models, where the UV radiation field does not impact the region as it is immediately attenuated by the medium. Ultimately we want to determine the age of a given region using chemistry in combination with radiative transfer.