Les piles à combustible sont des dispositifs qui permettent de transformer directement l’énergie chimique potentielle d’un carburant en énergie électrique. Elle sont presque toujours couplées à un convertisseur de puissance et l’ensemble est ici appellé « système à pile à combustible ». Le comportement de ces systèmes, les interactions entre ses composants, ainsi que leurs réponses aux stimulations extérieures ont été analysés, étudiés et mesurés. A cet effet, un système à pile à combustible complet a été modélisé. Des critères de dimensionnement pour cas où ni la pile à combustible ni le convertisseur de puissance sont à priori connus ont été identifiés et un prototype a été dimensionné et réalisé. D’autres aspects corrélatifs intéressants ont également été développés et étudiés, comme le fonctionnement du convertisseur à la limite entre les modes de conduction continu et discontinu, ainsi que son contrôle à fréquence de commutation variable. Des résultats expérimentaux et de simulation pour le système et pour les différentes parties dont il est composé sont présentés. / Fuel cells are devices in which a fuel’s chemical potential energy is directly converted into electrical energy. They are almost always coupled to a power converter and the ensemble is here called “fuel cell system.” The behaviour of such systems, the interactions between their components,and their responses to external stimulations have been analysed, studied and measured. For this purpose, a complete fuel cell system has been modelled. Sizing criteria for cases where neither the fuel cell nor the power converter are a priori known have been identified, and a prototype has been sized and built. Other interesting correlative aspects have also been developed and studied, like the operation of the power converter on the border between the discontinuousand continuous conduction modes, and its control with a variable switching frequency. Experimental and simulation results for the system and for the different parts that compose it are presented. / Le celle a combustibile sono dei dispositivi in cui l’energia chimica potenziale di un combustibile è direttamente convertita in energia elettrica. Quasi sempre le celle a combustibile sono accoppiate a un convertitore di potenza e l’insieme è qui chiamato «sistema a celle a combustibile». Il comportamento di questi sistemi, le interazioni tra i diversi componenti, nonché le loro risposte a stimoli esterni sono stati analizzati, studiati e misurati.A tal fine, un sistema completo a celle a combustibile è stato modellizzato. Sono stati identificati dei criteri di dimensionamento per casi in cui né la cella a combustibile, né il convertitore sono noti a priori, e un prototipo è stato dimensionato e realizzato. Altri interessantiaspetti correlatisonostati sviluppatie studiati,comeil funzionamento del convertitore di potenza al limite fra modo di conduzione discontinuo e continuo, e il suo controllo a frequenza di commutazione variabile. Risultati sperimentali e di simulazione per il sistema e le diverse parti che lo compongono sono presentati.

No description available.

This thesis presents the initiation of a multi-site photometric programme to examine the extraordinary behaviour displayed by 18 R Coronae Borealis (RCB) stars in the Magellanic Clouds (MCs). RCB stars exhibit a unique variability whereby they undergo rapid declines of up to several magnitudes. The decline may take several weeks, whereas the recovery to maximum light may take months or even years. The accepted wisdom for the cause of these enigmatic declines is a phenomenon whereby dust formed in the stellar environment reduces the brightness by as much as eight magnitudes (Clayton 1996). This is followed by the recovery phase during which the dust becomes homogeneously distributed in the stellar environment. The monitoring programme comprised the collection of UBVRI photometric data using five telescopes located at three different southern hemisphere longitudes (Las Campanas Observatory in Chile, Mount John University Observatory (MJUO) in New Zealand and the Southern African Large Telescope (SALT) in South Africa). The Optical Gravitational Lensing Experiment (OGLE), that operates at Las Campanas Observatory, provided the longest extent of data (December 1994 to February 2008). This was supplemented by data collected with telescopes at MJUO (September 2007 to January 2008) and SALTICAM on SALT (October 2007 to February 2008). Data calibration across the five instruments was a key element of the analysis, and entailed the use of F116 (an F region standard star) and other tertiary standards. Two important RCB characteristics, the enigmatic declines and the pulsational variability, form the bulk of the analysis presented in this thesis. Examination of the data acquired in the V and I filters resulted in the identification of a total of 18 RCB declines occurring in four stars (three stars in the Large Magellanic Cloud (LMC) and one in the Small Magellanic Cloud (SMC)). Construction of colour-magnitude diagrams (V −I vs V ), during the recovery to maximum light were undertaken in order to study the unique colour behaviour associated with the RCB declines. The combined recovery slope for the four stars was determined to be [(delta V)/(delta(V −I))] = 3.37 ± 0.24, which is similar to the value of [(delta V)/(delta(V −I))] = 3.1 ± 0.1 calculated for galactic RCB stars (Skuljan et al. 2003). In addition, the slopes calculated for the stars in the LMC ([(delta V)/(delta(V −I))]LMC = 3.34 ± 0.21) and SMC ([(delta V)/(delta((V −I))]SMC = 3.21 ± 0.22) alone, also agree to within their uncertainty. These results may imply that the nature of the dust (i.e. the particle size) is similar in both our Galaxy and the MCs. The pulsation analysis focused on the identification of pulsation periods in nine RCB stars in the MCs. Two different methods, Fourier analysis and dominant period subtraction, were employed for this purpose. Periodic variations are apparent in these stars, and for the majority, a period of around 40 days (common in RCB stars, Lawson et al. 1990, 1994) was detected using the second identification method. In the future, frequent data collection over several years, and more sophisticated pulsation identification techniques, will increase the probability of extracting individual periods from the complex RCB light curves.

No description available.

No description available.

We determine the optimal allocation of funds between the fixed and variable sub-accounts in a variable annuity with a GMDB (Guaranteed Minimum Death Benefit) clause featuring partial withdrawals by using a utility-based approach. In section two, the Merton method is applied by assuming that individuals allocate funds optimally in order to maximize the expected utility of lifetime consumption. It also reflects bequest motives by including the recipient's utility in terms of the policyholder's guaranteed death benefits. We derive the optimal transfer choice by the insured, and furthermore price the GMDB through maximizing the discounted expected utility of the policyholders and beneficiaries by investing dynamically in the fixed account and the variable fund and withdrawing optimally. In section three, we add fixed and stochastic income to the model and find that both human capital and the GMDB will influence the insured's allocation and withdrawal decisions. Section four explores the GMDB effects if there is also a term life policy available in the market. Our work suggests that if term life insurance is available and is continuously adjustable, fairly priced GMDBs may not be useful investments and the existence of GMDBs does not affect term life policy demand significantly.

Dissertation : Sciences : Chicago : 1913. / Astrophysical journal, Vol. XXXVIII, no. 3.

This study is about some of the variables that influence a correct using of the prepositions por and para in the Spanish language and in which type of clauses it is more difficult to separate the two prepositions, according to Swedish students at university level.                                                                                               The purpose of this essay is to investigate in which type of clauses it is more difficult to differentiate por and para. The study also intends to determinate some of the variables that influence on the correct/incorrect use of the two prepositions.                                                                                                     This study is carried out with 56 students from two Swedish universities that are currently studying Spanish at the first, second or third level. This investigation withholds a questionnaire that is divided into two parts. The first part has a sociological character with questions about date and place of birth, sex and native language of the informant and his or her parents. It also includes questions about the informant´s grades in Spanish, the own estimation of his or her competence in Spanish and the own perception of one´s acquired Spanish. The second part contains exercises in which the informants had to choose between por and para and translate the complete sentence into Swedish so that it is clear if they have guessed or if they know the true value of the chosen preposition. The answers of the questionnaire were used to find out in which type of clauses it is more difficult to separate the two prepositions and which factors were most significant for the application of the correct preposition.                                                                    The results of the investigation show that the clauses formed by spatial location were regarded the hardest ones by the students. They also show that the most significant variable that influences on the use of the correct preposition is the own perception of one´s competence regarding Spanish.

This thesis presents the initiation of a multi-site photometric programme to examine the extraordinary behaviour displayed by 18 R Coronae Borealis (RCB) stars in the Magellanic Clouds (MCs). RCB stars exhibit a unique variability whereby they undergo rapid declines of up to several magnitudes. The decline may take several weeks, whereas the recovery to maximum light may take months or even years. The accepted wisdom for the cause of these enigmatic declines is a phenomenon whereby dust formed in the stellar environment reduces the brightness by as much as eight magnitudes (Clayton 1996). This is followed by the recovery phase during which the dust becomes homogeneously distributed in the stellar environment. The monitoring programme comprised the collection of UBVRI photometric data using five telescopes located at three different southern hemisphere longitudes (Las Campanas Observatory in Chile, Mount John University Observatory (MJUO) in New Zealand and the Southern African Large Telescope (SALT) in South Africa). The Optical Gravitational Lensing Experiment (OGLE), that operates at Las Campanas Observatory, provided the longest extent of data (December 1994 to February 2008). This was supplemented by data collected with telescopes at MJUO (September 2007 to January 2008) and SALTICAM on SALT (October 2007 to February 2008). Data calibration across the five instruments was a key element of the analysis, and entailed the use of F116 (an F region standard star) and other tertiary standards. Two important RCB characteristics, the enigmatic declines and the pulsational variability, form the bulk of the analysis presented in this thesis. Examination of the data acquired in the V and I filters resulted in the identification of a total of 18 RCB declines occurring in four stars (three stars in the Large Magellanic Cloud (LMC) and one in the Small Magellanic Cloud (SMC)). Construction of colour-magnitude diagrams (V −I vs V ), during the recovery to maximum light were undertaken in order to study the unique colour behaviour associated with the RCB declines. The combined recovery slope for the four stars was determined to be [(delta V)/(delta(V −I))] = 3.37 ± 0.24, which is similar to the value of [(delta V)/(delta(V −I))] = 3.1 ± 0.1 calculated for galactic RCB stars (Skuljan et al. 2003). In addition, the slopes calculated for the stars in the LMC ([(delta V)/(delta(V −I))]LMC = 3.34 ± 0.21) and SMC ([(delta V)/(delta((V −I))]SMC = 3.21 ± 0.22) alone, also agree to within their uncertainty. These results may imply that the nature of the dust (i.e. the particle size) is similar in both our Galaxy and the MCs. The pulsation analysis focused on the identification of pulsation periods in nine RCB stars in the MCs. Two different methods, Fourier analysis and dominant period subtraction, were employed for this purpose. Periodic variations are apparent in these stars, and for the majority, a period of around 40 days (common in RCB stars, Lawson et al. 1990, 1994) was detected using the second identification method. In the future, frequent data collection over several years, and more sophisticated pulsation identification techniques, will increase the probability of extracting individual periods from the complex RCB light curves.

Thesis (Ph. D.)--Faculty of Science, University of Sydney, 2005. / Bibliography: leaves 217-229.