A Fortran IV language computer program has been written by the author for the analysis of gamma-gamma directional correlations obtained using radioactive sources. In this program the multipole-mixing ratio parameter, A, for the mixed multipole transition in the cascade is varied and the theoretical correlation is calculated for one hundred fifty-seven values of the mixing ratio for each trial spin sequence. The normalized chi-square test, Q2, is used to compare the theoretical and experimental results.The study of the effect of the multipole-mixing ratio and the attenuation factors on gamma-gamma directional correlation shapes has been investigated forsequence sets. The study has been separated into two parts: first, the effect of the attenuation factors when the multipole-mixing ratio is fixed; second, the effect of the multipole-mixing ratio for fixed attenuation factors.The results show the smoothing effect of the attenuation factors on the correlation function and it is illustrated graphically. The effect of the multipole-mixing ratio on the correlation function, with is a quadratic function in S, is also shown graphically.Ball State UniversityMuncie, IN 47306

A multi-detector spectrometer was constructed to measure garmia-gamma angular correlations in 154Gd from the decay of 154Eu. Gamma-ray multipole mixing ratios were extracted from the data. A modified fast-slow coincidence electronics arrangement with selective routing of data was used. One Ge(Li) detector and three NaI detectors were used in the system for rapid data acquisition. "Real-plus-random" and "random" coincidences were accumulated simultaneously with detectors set at selected angles. Mixing ratios for the first transition in the cascades of 1274-123--keV (2--2+-0+), 1005-123-keV (3+-2+-0+), and 723-996-keV (2--2+-O+) were measured as '5(1274) = 0.02 0.02, '5(1005) = -28+10' '5(723) = 0.02 0.02.'The measured correlation for the 592-1005 keV cascade (2--3+-2+) was analyzed by searching a 157 by 157 array of values for '5(592) and 8(1005); agreement was tested using a Q2 criterion. The best agreement for the mixing ratio of the 592-keV transition was 8(592) = 0.08 0:22; for the 1005-keV transition 8(1005) = -9.5+7. The value 8(1005) _ -9.5+7 is taken to be the better value as a result of experimental considerations. The value for the 592-keV transition had not been previously measured.Ball State UniversityMuncie, IN 47306

The directional correlation of the 346-136 Kev gamma-gamma cascade in Ta¹⁸¹ was measured using the delayed coincidence method with a source of Hf¹⁸¹ in 27 N HF. The contributions to the composite delayed coincidence spectrum of the interfering 133-482 Kev and 133 - 346 Kev cascades were removed by the subtraction from this spectrum of appropriate 133-482 Kev pure delayed coincidence data. The extracted 346 -136 Kev coincidence data then yielded the correlation coefficients A₂₂ = o.190 土0.011 and A₄₄. = -0.025 土O. 024 that are consistent with the established spin sequence 5/ 2(E2)9 / 2(Ml +E2)7 / 2 and with an admixture of 16.20/0土1. 2% E2 radiation in the 136 Kev mixed transition. The results of the experiment are in excellent agreement with those obtained from conversion electron measurements and resolve the discrepancy apparent in earlier work on the 346-136 Kev cascade

Orientador: Carola Dobrigkeit Chinellato / Dissertação (mestrado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin / Made available in DSpace on 2018-08-22T13:08:19Z (GMT). No. of bitstreams: 1 Castilho_CamileMendes_M.pdf: 4872331 bytes, checksum: 59af4c2607b071fd467957e83946bcf8 (MD5) Previous issue date: 2013 / Resumo: Duas questões importantes no estudo da física de raios cósmicos são quais são as fontes astrofísicas dessas partículas e como é o campo magnético por elas atravessado. O Observatório Pierre Auger, localizado na província de Mendoza, na Argentina, é um experimento que tem como objetivo estudar raios cósmicos de altas energias (superior a 1 EeV). Entre os objetivos do observatório, está buscar possíveis fontes desses raios cósmicos e estudar o campo magnético por eles atravessado. Considerando que partículas ultra-energéticas sofrem deflexões em campos magnéticos que são inversamente proporcionais _as suas energias, espera-se que aquelas provenientes de uma mesma fonte cheguem á Terra com suas direções alinhadas sobre a esfera celeste e com desvios angulares satisfazendo essa dependência com a energia. Um grupo de raios cósmicos com suas direções e energias satisfazendo essas características é chamado de multipleto. Nesta dissertação, foram analisados 2196 raios cósmicos com energias acima de 20 EeV, detectados pelo Observatório Pierre Auger entre 1o de janeiro de 2004 e 22 de novembro de 2012, a _m de realizar uma busca por multipletos. Para encontrar estes multipletos, foi utilizado o Método da _Arvore de Extensão Mínima. Este método é utilizado para separar o conjunto de raios cósmicos em subconjuntos. Uma vez encontrados esses subconjuntos, foi verificado se as direções dos raios cósmicos do subconjunto satisfazem a correlação esperada entre as suas direções e os inversos de suas energias. Para isso foi calculado o coeficiente de correlação e a dispersão angular nas coordenadas dos raios cósmicos de cada subconjunto em um plano tangente _a esfera celeste no ponto correspondente _a direção média. Se o coeficiente de correlação for superior a um valor mínimo e a dispersão angular for menor do que um valor máximo pré-estabelecidos, o multipleto em questão é considerado um multipleto correlacionado. Após identificarmos estes multipletos, foi possível encontrar as posições das possíveis fontes dos raios cósmicos que o compõem e obter informação sobre o poder de deflexão do campo magnético por eles atravessado nas direções das respectivas fontes. Para o período em questão foram encontrados três multipletos correlacionados com um número de eventos igual ou superior a doze. Para estes três multipletos foram procuradas posições de possíveis fontes. Realizando uma comparação entre as posições encontradas e um catalogo de objetos astrofísicos, foram encontrados objetos próximos ás direções das fontes encontradas / Abstract: Two important questions in the study of ultra-high-energy cosmic rays are related to the astrophysical sources of these particles and the characteristics of the magnetic field they have traversed in their way from the sources to Earth. The Pierre Auger Observatory was designed and built in Argentina in order to address these and other questions about ultra-high energy cosmic rays. Its design goals included being able to measure ultra-high energy cosmic rays (above 1 EeV) with unprecedented statistics. Considering that the trajectories of ultra-high energy particles are defected by the magnetic fields traversed and that the defection is inversely proportional to their energies, it can be expected that particles having different energies and coming from a single source will arrive at Earth with their directions aligned on the celestial sphere and with angular deviations satisfying that dependence with the energy. A group of cosmic rays with their directions and energies satisfying those characteristics is called a multiplet. In this work, we search for multiplets in a data sample of 2196 cosmic rays with energies above 20 EeV recorded by the Pierre Auger Observatory between 1st January 2004 and 22nd November 2012. We applied the method of the minimum spanning tree to separate the whole data set into subsets and then analyzed the subsets, checking whether the directions of the cosmic rays in each subset satisfy the expected correlation with the inverse of their energies. After identifying multiplets which satisfy the correlation, it is possible to find theposition of the sources of the cosmic rays and estimate the defection power of the magnetic field these particles must have traversed in the corresponding directions of the sources. In the period covered by our analysis we have found three multiplets with twelve or more events. For each multiplet we have found the direction of the possible source and the defection power of the magnetic field and looked for nearby astrophysical objects in a catalog / Mestrado / Física / Mestra em Física

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Contexte : La chromodynamique quantique (CDQ), théorie de l’interaction forte, prédit un nouvel état de la matière, le plasma de quarks et de gluons (PQG) dont les degrés de liberté fondamentale, les quarks et les gluons, peuvent bouger quasi-librement. Les hautes températures et densités de particules, qui sont nécessaires, sont supposées être les conditions de l’univers dans ses premiers moments ou dans les étoiles à neutrons. Récemment elles ont été recrées par des collisions de noyaux d’ions lourdes à hautes énergies. Ces expériences étudient le PQG par la détection des particules de hautes énergies qui traversent le milieu, notamment, les quarks lourds. Les mécanismes de leur perte d’énergie dans le PQG ne sont pas compris complètement. Particulièrement, ils sont attribués aux processus soit de radiation induite par le milieu, soit de collisions de particules de type 2 vers 2, ou des combinaisons.Méthodes : Afin de trouver de nouvelles observables pour pouvoir distinguer les mécanismes de la perte d’énergie, on a implémenté un algorithme Monte-Carlo, qui simule la formation des cascades des particules à partir d’une particule initiale. Pour traiter le milieu, on a introduit des interactions PQG-jets, qui correspondent aux processus collisionnels et radiatifs. Les corrélations entre deux particules finales des cascades, dont une représente un quark trigger, ont été examinées comme moyen pour distinguer les modèles.Résultats : La dépendance de l’ouverture angulaire pour des corrélations entre deux particules en fonction des énergies des particules peut servir comme moyen pour séparer les mécanismes collisionnels et radiatifs de la perte d’énergie dans le milieu. / Context: Quantum chromodynamics (QCD), the theory of the strong interactions, predicts a new state of matter, the quark-gluon plasma (QGP), where its fundamental degrees of freedom, the quarks and gluons, behave quasi-freely. The required high temperatures and/orparticle densities can be expected for the early stages of the universe and in neutron stars, but have lately become accessible by highly energetic collisions of heavy ion cores. Commonly, these experiments study the QGP by the detection of hard probes, i.e. highly energetic particles, most notably heavy quarks, that pass the medium. The mechanisms of their energy-loss in the QGP are not yet completely understood. In particular, they are attributed to processes of either additional, medium induced radiation or 2 to 2 particle scattering, or combinations thereof.Methods: In a theoretical, phenomenological approach to search for new observables that allow discriminating between these collisional and radiative energy-loss mechanisms a Monte-Carlo algorithm that simulates the formation of particle cascades from an initial particle was implemented. For the medium, different types of QGP-jet interactions, corresponding to collisional and/orradiative energy loss, were introduced. Correlations between pairs of final cascade particles, where one represents a heavy trigger quark, were investigated as a means to differentiate between these models.Findings: The dependence of angular opening for two particle correlations as a function of particle energy may provide a means to disentangle collisional and radiative mechanisms of in-medium energy loss.