All-optical time-resolved measurement techniques provide a powerful tool for investigating critical parameters that determine the performance of infrared photodetector and emitter semiconductor materials. Narrow-bandgap InAs/GaSb type-II superlattices (T2SLs) have shown great promise as next generation materials, due to superior intrinsic properties and versatility. Unfortunately, InAs/GaSb T2SLs are plagued by parasitic Shockley-Read-Hall recombination centers that shorten the carrier lifetime and limit device performance. Ultrafast pump-probe techniques and time-resolved differential-transmission measurements are used here to demonstrate that "Ga-free" InAs/InAs₁₋xSbx T2SLs and InAsSb alloys do not have this same limitation and thus have significantly longer carrier lifetimes. Measurements of unintentionally doped MWIR and LWIR InAs/InAs₁₋xSbx T2SLs demonstrate minority carrier (MC) lifetimes of 18.4 µs and 4.5 µs at 77 K, respectively. This represents a more than two order of magnitude increase compared to the 90 ns MC lifetime measured in a comparable MWIR and LWIR InAs/GaSb T2SL. Through temperature-dependent differential-transmission measurements, the various carrier recombination processes are differentiated and the dominant recombination mechanisms identified for InAs/InAs₁₋xSbx T2SLs. These results demonstrate that these Ga-free materials are viable options over InAs/GaSb T2SLs and potentially bulk Hg₁₋xCdxTe photodetectors. In addition to carrier lifetimes, the drift and diusion of excited charge carriers through the superlattice layers (i.e. in-plane transport) directly aects the performance of photo-detectors and emitters. All-optical ultrafast techniques were successfully used for a direct measure of in-plane diffusion coeffcients in MWIR InAs/InAsSb T2SLs using a photo-generated transient grating technique at various temperatures. Ambipolar diffusion coefficients of approximately 60 cm²/s were reported for MWIR InAs/InAs₁₋xSbxT2SLs at 293 K.

No description available.

No description available.

The depletion of more attractive thicker and easily accessible coal seams in the central Appalachia will direct attention towards the extraction of coal seams thinner than 28 in. This thesis investigates the feasibility of an integrated mining and backfilling system applicable to thin seams. Two conceptual mining systems, namely Auger mining and Self Advancing Miner, have been proposed for this purpose. Both these systems are designed to remotely mine coal from the seams. Several attempts were made in the past to mine coal in a similar fashion but were not very successful due to several problems inherent to thin seams. The lack of effective steering techniques, accurate coal/rock interface and pillar thickness detection techniques were the main shortcomings of the systems. These problems were addressed in the proposed conceptual mining systems. Several coal/rock interface and rib thickness detection techniques currently available in the market or in the prototype stage have been discussed. Recent developments in coal/rock interface detection and direction sensing techniques have good potential in alleviating the previously encountered problems. Sensitivity analyses have been performed to assess the of effect critical mining parameters on the production potential of these systems. The self advancing miner has been found to be more promising than auger mining. Conceptual panels and face layouts for both systems have been included. Two types of filling methods namely pneumatic and hydraulic are considered applicable under thin seam conditions. A backfilling technique using rubber hoses for fill placement can be applied with both methods. Sensitivity analysis have been performed to establish the relationship between face operation cost, filling cost per ton and development cost per foot. Resulting analyses indicate that panel cost per short ton of coal is more sensitive to filling cost than on development cost. / Master of Science

O objetivo desta dissertação é a busca de anisotropias em grandes escalas angulares no fluxo de raios cósmicos acima de 4 × 10^{18} eV e o confronto dos resultados obtidos com as previsões dos principais modelos astrofísicos na região de ultra altas energias. Com esse propósito foram analisados os dados de chuveiros atmosféricos extensos registrados pelo Observatório Pierre Auger no período de 01 de janeiro de 2004 até 31 de agosto de 2016, compreendendo um total de 108 480 eventos detetados com ângulos zenitais entre 0 e 80 graus acima de 4 × 10^{18} eV. Efeitos sistemáticos locais como a influência da variação das condições atmosféricas e a influência do campo geomagnético nos estimadores de energia das cascatas atmosféricas foram corrigidos cuidadosamente para evitar a introdução de sinais espúrios de anisotropias na análise. Especial ênfase foi dedicada à construção de um mapa bidimensional na esfera celeste com os valores da exposição para cada direção no céu, calculado com uma precisão de 1% a partir da informação da área de coleção efetiva no Observatório Pierre Auger a cada minuto. Da mesma forma, a distribuição das direções de chegada dos eventos foi registrada em mapas bidimensionais na esfera celeste que, após corrigidos pela exposição, são transformados nos mapas de fluxo usados na análise quantitativa para a busca de anisotropias. Neste trabalho procurou-se padrões dipolares de anisotropias, os quais foram quantificados usando o método de expansão multipolar em harmônicos esféricos. Diferentemente do método bidimensional de Rayleigh usado na maioria dos estudos deste tipo, o método aqui utilizado fornece de maneira direta as três componentes cartesianas do dipolo, por meio das quais a reconstrução da amplitude e orientação espacial do dipolo é feita de maneira mais natural. A busca de anisotropias foi realizada em dois intervalos de energia independentes, assim foram analisados por separado os eventos com energias entre 4 × 10^{18} e 8 × 10^{18} eV e de energias maiores que 8 × 10^{18} eV. No primeiro intervalo não foi encontrado nenhum sinal de anisotropia estatisticamente significativo. No segundo intervalo foi encontrada uma anisotropia dipolar de amplitude d = (7.9 ± 1.1)% com coordenadas equatoriais (_d , _d ) = (103 ± 10 , 38 ± 7 ) graus e uma probabilidade de ocorrência ao acaso de 6.90 × 10^{8} , correspondendo a uma significância estatística acima do limiar de descoberta de 5 . Tal amplitude e direção são melhor explicadas assumindo-se uma origem extragaláctica para os raios cósmicos com energias acima de 8 × 10^{18} eV. / The aim of this dissertation is the search for large scale anisotropies in the cosmic ray flux above 4 × 10^{18} eV and the comparison of the results with the predictions of the main astrophysical models in the ultra high energy region. With this purpose we analyzed the data of extensive air showers detected by the Pierre Auger Observatory in the period of 1st January 2004 to 31st August 2016 comprising a total of 108 480 events with zenith angles between 0 and 80 degrees above the threshold of 4 × 10^{18} eV. Local systematic effects such as the influence of the variation of the atmospheric conditions and the effect of the geomagnetic field in the energy estimators were properly corrected to avoid the introduction of spurious anisotropy signals in the analysis. Special emphasis was placed on the construction of a two-dimensional map on the celestial sphere with the exposure values for each direction on the sky, calculated with an accuracy of 1% from the information of the effective collection area of the observatory at every minute. Likewise, the arrival directions distribution of the events was recorded in two-dimensional maps on the celestial sphere that after correcting by the exposure were transformed into the flux maps to be used in the quantitative analysis for the anisotropies search. In this work we search for dipolar-like anisotropy patterns, which were quantified by performing a spherical harmonics decomposition of the cosmic ray flux map. Unlike the traditional two-dimensional Rayleigh method used in the majority of the studies of this kind, the method used here directly provides the three cartesian components of the dipole, allowing the reconstruction of its amplitude and orientation in a more natural way. The anisotropy search was made in two independent energy bins, so the distributions of the events with energies between 4 × 10^{18} and 8 × 10^{18} eV and those with energies greater than 8 × 10^{18} eV were analyzed separately. In the first energy bin no statistically significant departure from isotropy was found. In the second energy bin a dipole anisotropy of amplitude d = (7.9 ± 1.1)% with equatorial coordinates (_d , _d ) = (103 ± 10 , 38 ± 7 ) degrees and a chance probability of 6.90 × 10^{8} was found, corresponding to a statistical significance above the discovery threshold of 5 . Such amplitude and direction for the reconstructed dipole is better explained if an extragalactic origin is assumed for the bulk of cosmic rays above 8 × 10^{18} eV.

Absolute K-shell x-ray cross sections and Auger-electron cross sections are measured for carbon for 0.6 to 2.0 MeV proton incident on CH₄, n-C₄H₁₀ (n-Butane), i-C₄H₁₀ (isobutane), C₆H₆ (Benzene), C₂H₂ (Acetylene), CO and CO₂. Carbon K-shell fluorescence yields are calculated from the measurements of x-ray and Auger-electron cross sections. X-ray cross sections are measured using a variable geometry end window proportional counter. An alternate method is described for the measurement of the transmission of the proportional counter window. Auger electrons are detected by using a constant transmission energy Π/4 parallel pi ate electrostatic analyzer. Absolute carbon K-shell x-ray cross sections for CH₄ are compared to the known results of Khan et al. (1965). Auger-electron cross sections for proton impact on CH₄ are compared to the known experimental values of RΦdbro et al. (1979), and to the theoretical predictions of the first Born and ECPSSR. The data is in good agreement with both the first Born and ECPSSR, and within our experimental uncertainties with the measurements of RΦdbro et al. The x-ray cross sections, Auger-electron cross sections and fluorescence yields are plotted as a function of the Pauling charge, and show significant variations. These changes in the x-ray cross sections are compared to a model based on the number of electrons present in the 2s and 2p sub shells of these carbon based molecules. The changes in the Auger-electron cross sections are compared to the calculations of Matthews and Hopkins. The variation in the fluorescence yield is explained on the basis of the multiconfiguration Dirac-Fock model.

Röntgen Freie Elektronen Laser ermöglichen es Doppel-K-Schalen Löchern in Molekülen in aufeinanderfolgenden mehrfachen Ionisationsschritten in bedeutender Anzahl zu erzeugen. Die Eigenschaften dieser zweifach ionisierten Zustände ist insbesondere relevant für die Strahlungsschäden bei Beugungsexperimenten mit kohärenter Röntgenstrahlung zur Bildgebung einzelner Moleküle. In dieser Arbeit wird der Auger Zerfall doppelt K-Schalen ionisierter Moleküle mittels quantenchemischer ab-initio Methoden untersucht. Zur Beschreibung des emittierten Auger Elektrons im kontinuierlichen Energiespektrum wird dabei die Ein-Zentrums Methode verwendet, in der die elektronische Wellenfunktion auf einem radialen Gitter beschrieben wird unter Verwendung von sphärischen Harmonischen. Wie anhand desWassermoleküls gezeigt wird, ergeben sich durch die Doppel-K-Loch induzierte Protonendynamik in dem Auger Spektrum ausgeprägte Flanken im höherenergetischen Teil jeder Spektralspitze. Die Lebensdauer von Doppel-K-Schalen Löchern in Molekülen ist deutlich verringert im Vergleich zu einfachen K-Löchern durch die K-Loch induzierten Abschirmeffekte der Valenzelektronen. Dieser Mechanismus wird durch ein einfaches Modell erklärt aus dem eine Beziehung zwischen Zerfallsrate und Valenzelektronenpopulation abgeleitet. Mögliche Konsequenzen dieser Ergebnisse für Röntgenbeugungsexperimente sind: Erstens, auch für Röntgenpulse kürzer als 10fs wird das Beugungsbild durch die K-Loch induzierten Umstrukturierungen der Valenzelektronen beeinflußt. Zweitens, die Gesamt-Ionisationsrate ist erhöht aufgrund der schnelleren Neubesetzung der K-Löcher.

Les connaissances sur les rayons cosmiques d'ultra haute énergie (E>10^{18} eV) ont progressé durant la dernière décennie, en particulier grâce aux résultats remarquables de l'Observatoire Pierre Auger. La question de la composition du flux de rayons cosmiques à ces énergies reste cependant ouverte. Le projet EASIER (Extensive Air Shower Identification using Electron Radiometer) de détection radio des gerbes atmosphériques recherche de nouvelles observables liées à la nature du rayonnement cosmique primaire, complémentaires de celles déjà mise en oeuvre à l'Observatoire Pierre Auger. Ce dispositif est constitué d'un réseau d'antennes radio fonctionnant aux fréquences MHz et GHz et installées en mode esclave sur une soixantaine de détecteurs de particules du réseau de surface de l'Observatoire. Après étude de la réponse des détecteurs et analyse des données, les caractéristiques des signaux détectés aux fréquences MHz se sont révélées compatibles avec une origine géomagnétique de l'émission radio des gerbes. Aux fréquences GHz, seuls quelques signaux ont été détectés en coïncidence avec des gerbes atmosphériques. Un programme de simulation a été réalisé dans le but d'identifier l'origine de cette émission micro-ondes. Il inclut le développement de la gerbe dans l'atmosphère et différents mécanismes d'émission aux fréquences GHz : l'effet Cerenkov et le bremsstrahlung moléculaire. La propagation du rayonnement dans l'atmosphère et la réponse de l'antenne réceptrice sont également simulés, ce qui permet une comparaison directe des signaux détectés avec les signaux attendus. / The understanding on the ultra high cosmic rays (E>10^{18} eV) issue has been improved over the last decade, especially through the noteworthy results of the Pierre Auger Observatory. The composition of cosmic rays at those energies is still an open matter. The EASIER project (Extensive Air Shower Identification using Electron Radiometer) on radio detection of extensive air showers is looking for new observables related to the nature of primary cosmic rays, complementary to those already implemented at the Pierre Auger Observatory. This prototype consists of an array of MHz and GHz antennas, set up on a slave mode on about sixty tanks of the surface detector of the Observatory. Further to a study of the antenna response and a data analysis, the features of the detected signals at MHz frequencies have turned out to be compatible with a geomagnetic origin of the shower radio emission. At GHz frequencies, only a few signals have been detected in coincidence with extensive air showers. A simulation program has been created, aiming to identify the origin of this micro wave emission. It includes the air shower development in the atmosphere and different emission mechanisms at GHz frenquencies : the Cerenkov radiation and the molecular bremsstrahlung. The radiation propagation through the atmosphere and the receiving antenna response are simulated as well, allowing to directly compare the detected signals to the predicted ones.

O objetivo desta dissertação é a busca de anisotropias em grandes escalas angulares no fluxo de raios cósmicos acima de 4 × 10^{18} eV e o confronto dos resultados obtidos com as previsões dos principais modelos astrofísicos na região de ultra altas energias. Com esse propósito foram analisados os dados de chuveiros atmosféricos extensos registrados pelo Observatório Pierre Auger no período de 01 de janeiro de 2004 até 31 de agosto de 2016, compreendendo um total de 108 480 eventos detetados com ângulos zenitais entre 0 e 80 graus acima de 4 × 10^{18} eV. Efeitos sistemáticos locais como a influência da variação das condições atmosféricas e a influência do campo geomagnético nos estimadores de energia das cascatas atmosféricas foram corrigidos cuidadosamente para evitar a introdução de sinais espúrios de anisotropias na análise. Especial ênfase foi dedicada à construção de um mapa bidimensional na esfera celeste com os valores da exposição para cada direção no céu, calculado com uma precisão de 1% a partir da informação da área de coleção efetiva no Observatório Pierre Auger a cada minuto. Da mesma forma, a distribuição das direções de chegada dos eventos foi registrada em mapas bidimensionais na esfera celeste que, após corrigidos pela exposição, são transformados nos mapas de fluxo usados na análise quantitativa para a busca de anisotropias. Neste trabalho procurou-se padrões dipolares de anisotropias, os quais foram quantificados usando o método de expansão multipolar em harmônicos esféricos. Diferentemente do método bidimensional de Rayleigh usado na maioria dos estudos deste tipo, o método aqui utilizado fornece de maneira direta as três componentes cartesianas do dipolo, por meio das quais a reconstrução da amplitude e orientação espacial do dipolo é feita de maneira mais natural. A busca de anisotropias foi realizada em dois intervalos de energia independentes, assim foram analisados por separado os eventos com energias entre 4 × 10^{18} e 8 × 10^{18} eV e de energias maiores que 8 × 10^{18} eV. No primeiro intervalo não foi encontrado nenhum sinal de anisotropia estatisticamente significativo. No segundo intervalo foi encontrada uma anisotropia dipolar de amplitude d = (7.9 ± 1.1)% com coordenadas equatoriais (_d , _d ) = (103 ± 10 , 38 ± 7 ) graus e uma probabilidade de ocorrência ao acaso de 6.90 × 10^{8} , correspondendo a uma significância estatística acima do limiar de descoberta de 5 . Tal amplitude e direção são melhor explicadas assumindo-se uma origem extragaláctica para os raios cósmicos com energias acima de 8 × 10^{18} eV. / The aim of this dissertation is the search for large scale anisotropies in the cosmic ray flux above 4 × 10^{18} eV and the comparison of the results with the predictions of the main astrophysical models in the ultra high energy region. With this purpose we analyzed the data of extensive air showers detected by the Pierre Auger Observatory in the period of 1st January 2004 to 31st August 2016 comprising a total of 108 480 events with zenith angles between 0 and 80 degrees above the threshold of 4 × 10^{18} eV. Local systematic effects such as the influence of the variation of the atmospheric conditions and the effect of the geomagnetic field in the energy estimators were properly corrected to avoid the introduction of spurious anisotropy signals in the analysis. Special emphasis was placed on the construction of a two-dimensional map on the celestial sphere with the exposure values for each direction on the sky, calculated with an accuracy of 1% from the information of the effective collection area of the observatory at every minute. Likewise, the arrival directions distribution of the events was recorded in two-dimensional maps on the celestial sphere that after correcting by the exposure were transformed into the flux maps to be used in the quantitative analysis for the anisotropies search. In this work we search for dipolar-like anisotropy patterns, which were quantified by performing a spherical harmonics decomposition of the cosmic ray flux map. Unlike the traditional two-dimensional Rayleigh method used in the majority of the studies of this kind, the method used here directly provides the three cartesian components of the dipole, allowing the reconstruction of its amplitude and orientation in a more natural way. The anisotropy search was made in two independent energy bins, so the distributions of the events with energies between 4 × 10^{18} and 8 × 10^{18} eV and those with energies greater than 8 × 10^{18} eV were analyzed separately. In the first energy bin no statistically significant departure from isotropy was found. In the second energy bin a dipole anisotropy of amplitude d = (7.9 ± 1.1)% with equatorial coordinates (_d , _d ) = (103 ± 10 , 38 ± 7 ) degrees and a chance probability of 6.90 × 10^{8} was found, corresponding to a statistical significance above the discovery threshold of 5 . Such amplitude and direction for the reconstructed dipole is better explained if an extragalactic origin is assumed for the bulk of cosmic rays above 8 × 10^{18} eV.

Orientador: Marcelo Moraes Guzzo / Tese (doutorado) - Universidade Estadual de Campinas, Instituto de Fisica Gleb Wataghin / Made available in DSpace on 2018-08-07T11:07:30Z (GMT). No. of bitstreams: 1 MouraJunior_CelioAdregade_D.pdf: 3776986 bytes, checksum: 07c139c8c30b32426082bda432e718e0 (MD5) Previous issue date: 2006 / Resumo: Fazemos uma estimativa do número de Chuveiros Atmosféricos Extensos originados por neutrinos do tau em Detetores de Fluorescência como os do Observatório Pierre Auger. Consideramos modelos de produção de neutrinos do elétron e do múon de altíssimas energias em objetos extra galácticos e Defeitos Topológicos, assim como mudança de sabor na propagação dos neutrinos da fonte até a Terra. Para a seção de choque dos neutrinos utilizamos um modelo que extrapola os parâmetros do Modelo Padrão até energias da ordem de 1021 e V. Porém esses parâmetros foram comprovados até a ordem de 1012 e V. gerando incertezas nos números obtidos para altíssimas energias. Concluímos que, dependendo da relação entre fluxo e seção de choque, existe uma região restrita de energia dos neutrinos do tau que pode gerar eventos com chuveiros atmosféricos duplos detectáveis em Detetores de Fluorescência. A energia dos neutrinos do tau deve ser de aproximadamente 1018 e V e o número de eventos pode variar algumas ordens de magnitude em torno de um evento por ano, dependendo dos modelos propostos e das caracteristicas do detetor / Abstract: We calculate the possible number of Extensive Air Showers originated by tau neutrinos in Fluorescence Detectors like the ones of the Pierre Auger Observatory. We consider models of production of electron and muon neutrinos in extra galactic objects and Topological Defects, as well as the possibility of neutrino flavor change in the propagation of the neutrinos between the source and the Earth. The neutrino cross section was calculated by the extrapolation of the standard model parton distribution functions until energies of the order of 1021 e V. However, due to uncertainties in the extrapolation for energies higher than 1012 e V the results are not robust. We conclude that, depending on the relation between flux and cross section, there is a strict range of energy for the tau neutrinos to generate double extensive air showers detectable in Fluorescence Detectors. The tau neutrino energy must be approximately 1018 e V and the event rate can vary some orders of magnitude around one event per year , depending on the flux-cross section relation and detector characteristics / Doutorado / Física das Particulas Elementares e Campos / Doutor em Ciências