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Journal articles on the topic "Auger, Pierre"
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Dova, Maria Teresa. "The Pierre Auger Observatory." Nuclear Physics B - Proceedings Supplements 122 (July 2003): 170–78. http://dx.doi.org/10.1016/s0920-5632(03)80373-0.
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Zavrtanik, D. "The Pierre Auger observatory." Nuclear Physics B - Proceedings Supplements 85, no. 1-3 (May 2000): 324–31. http://dx.doi.org/10.1016/s0920-5632(00)00525-9.
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Privitera, P. "The Pierre Auger Observatory." Nuclear Physics B - Proceedings Supplements 110 (July 2002): 487–90. http://dx.doi.org/10.1016/s0920-5632(02)01543-8.
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Privitera, P. "The Pierre Auger Observatory." Nuclear Physics B - Proceedings Supplements 110, no. 2 (July 2002): 487–90. http://dx.doi.org/10.1016/s0920-5632(02)80187-6.
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Marsella, Giovanni. "The Pierre Auger Observatory Upgrade." EPJ Web of Conferences 136 (2017): 02003. http://dx.doi.org/10.1051/epjconf/201713602003.
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Terrissol, Michel. "Pierre Auger and Monte Carlo." International Journal of Radiation Biology 92, no. 11 (November 1, 2016): 616. http://dx.doi.org/10.1080/09553002.2016.1233368.
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Castellina, Antonella. "Auger Highlights." Acta Polytechnica CTU Proceedings 1, no. 1 (December 4, 2014): 132–38. http://dx.doi.org/10.14311/app.2014.01.0132.
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The Pierre Auger Observatory has been designed to investigate the origin and nature of the ultra high energy cosmic rays using a hybrid detection technique. A review of selected results is presented, with the emphasis given to the measurement of energy spectrum, mass composition and arrival directions.
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Jejkal, Thomas. "Auger ACCESS—Remote Controlling and Monitoring the Pierre Auger Observatory." IEEE Transactions on Nuclear Science 60, no. 5 (October 2013): 3469–74. http://dx.doi.org/10.1109/tns.2013.2281816.
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Hardouin Duparc, Olivier. "Pierre Auger – Lise Meitner: Comparative contributions to the Auger effect." International Journal of Materials Research 100, no. 9 (September 2009): 1162–66. http://dx.doi.org/10.3139/146.110163.
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Escobar, Carlos O. "THE PIERRE AUGER COSMIC RAY OBSERVATORY." Radiation Physics and Chemistry 51, no. 4-6 (June 1998): 705–11. http://dx.doi.org/10.1016/s0969-806x(97)00243-0.
Full textDissertations / Theses on the topic "Auger, Pierre"
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Menezes, Márcio de [UNESP]. "Detecção de neutrinos no observatório Pierre Auger." Universidade Estadual Paulista (UNESP), 2003. http://hdl.handle.net/11449/91862.
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menezes_m_me_ift.pdf: 1408979 bytes, checksum: c49d46abc2dcaff209c0e561dfd6398a (MD5)Faz-se aqui o estudo da detecção de neutrinos (v) de altas energias ('E IND.v' > '10 POT.9' GeV) no Observatório Pierre Auger usando os detectores de fluorescência. Introduzimos todo o conhecimento experimental dos raios cósmicos, em conjunto com a fenomenologia das partículas elementares, para que o estudo da detecção possa ser entendido de forma bastante geral. Raios cósmicos de até '10 POT.15' eV vem de fontes em nossa galáxia; já as partículas acima de '10 POT.18' eV não são confinadas no campo magnético da galáxia. Portanto, acredita-se que estas partículas sejam de origem extra-galática. Porém, sua natureza continua completamente desconhecida. Existem vários modelos que resultam em diferentes fluxos de neutrinos de altíssimas energias. Independente do modelo, estes neutrinos vem de distâncias cosmológicas, estando sujeitos à oscilação do seu sabor. A oscilação de neutrinos traz como conseqüência uma igualdade entre os fluxos dos neutrinos de cada família. O método aqui utilizado para detecção de neutrinos consiste em considerar apenas aqueles que se propagam pelo interior terrestre, até chegarem a região de detecção. Estes neutrinos de altíssimas energias podem dar origem a léptons carregados após uma interação de corrente carregada com núcleos atômicos. Estes léptons carregados continuam se propagando na mesma direção do neutrino original, podendo sair da terra. Ao sair da Terra estes léptons carregados poderão ser detectados pelo Observatório Pierre Auger. Destes léptons, apenas o tau dará origem a um chuveiro eletromagnético que deverá ser detectado. Mostramos por fim que um número bastante pequeno de neutrinos atravessando a terra deverá ser observado. Entretando, mesmo a observação de um único evento em vários anos nos indicaria a existência de neutrinos. Além disso, seria o início de uma nova fase na detecção de raios cósmicos.
Abstracts: Here we study the detection of the ultra high energy neutrinos in Pierre Auger Observatory using the fluorescence detectors. We introduce all the experimental knowledge of cosmic rays, together with the elementary particles phenomenology, so that the detection study can be understood in a very genral way. Cosmic rays with energies up to '10 POT.15' eV come from sources in our galaxy. But the particles above '10 POT.18' eV are not confined in the galactic magnetic field. So, it is believed that these particles are of extragalactic origin. But their nature is completely unknown. There are many models that result in different ultrahigh energy neutrino fluxes. Independent of the model, these neutrinos como from cosmological distances, being subject to flavor oscillation. The neutrino oscillation gives as a consequence the equality between the neutrino fluxes of each family. The method used for the neutrino detection is to consider only those that propagate through the earth, until they arrive to the detection area. These ultra high energy neutrinos can create charged leptons after a charged current interaction with atomic nuclei. These charged leptons keep the same direction of the original neutrino and they can exit the Earth. When they exit the Earth, they will be detected by the Pierre Auger Observatory. We show, finally, that very small number of neutrinos crossing the Earth will be detected. However, even the observation of one single event in many years will be an indication of the existence of a neutrino flux. Moreover, it would be the beginning of a new phase in the cosmic ray detection.
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Menezes, Márcio de. "Detecção de neutrinos no observatório Pierre Auger /." São Paulo : [s. n.], 2003. http://hdl.handle.net/11449/91862.
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Orientador: Rogério RosenfeldBanca: Marcelo Moraes Guzzo
Banca: Adriano Antônio Natale
Resumo: Faz-se aqui o estudo da detecção de neutrinos (v) de altas energias ('E IND.v' > '10 POT.9' GeV) no Observatório Pierre Auger usando os detectores de fluorescência. Introduzimos todo o conhecimento experimental dos raios cósmicos, em conjunto com a fenomenologia das partículas elementares, para que o estudo da detecção possa ser entendido de forma bastante geral. Raios cósmicos de até '10 POT.15' eV vem de fontes em nossa galáxia; já as partículas acima de '10 POT.18' eV não são confinadas no campo magnético da galáxia. Portanto, acredita-se que estas partículas sejam de origem extra-galática. Porém, sua natureza continua completamente desconhecida. Existem vários modelos que resultam em diferentes fluxos de neutrinos de altíssimas energias. Independente do modelo, estes neutrinos vem de distâncias cosmológicas, estando sujeitos à oscilação do seu sabor. A oscilação de neutrinos traz como conseqüência uma igualdade entre os fluxos dos neutrinos de cada família. O método aqui utilizado para detecção de neutrinos consiste em considerar apenas aqueles que se propagam pelo interior terrestre, até chegarem a região de detecção. Estes neutrinos de altíssimas energias podem dar origem a léptons carregados após uma interação de corrente carregada com núcleos atômicos. Estes léptons carregados continuam se propagando na mesma direção do neutrino original, podendo sair da terra. Ao sair da Terra estes léptons carregados poderão ser detectados pelo Observatório Pierre Auger. Destes léptons, apenas o tau dará origem a um chuveiro eletromagnético que deverá ser detectado. Mostramos por fim que um número bastante pequeno de neutrinos atravessando a terra deverá ser observado. Entretando, mesmo a observação de um único evento em vários anos nos indicaria a existência de neutrinos. Além disso, seria o início de uma nova fase na detecção de raios cósmicos.
Abstracts: Here we study the detection of the ultra high energy neutrinos in Pierre Auger Observatory using the fluorescence detectors. We introduce all the experimental knowledge of cosmic rays, together with the elementary particles phenomenology, so that the detection study can be understood in a very genral way. Cosmic rays with energies up to '10 POT.15' eV come from sources in our galaxy. But the particles above '10 POT.18' eV are not confined in the galactic magnetic field. So, it is believed that these particles are of extragalactic origin. But their nature is completely unknown. There are many models that result in different ultrahigh energy neutrino fluxes. Independent of the model, these neutrinos como from cosmological distances, being subject to flavor oscillation. The neutrino oscillation gives as a consequence the equality between the neutrino fluxes of each family. The method used for the neutrino detection is to consider only those that propagate through the earth, until they arrive to the detection area. These ultra high energy neutrinos can create charged leptons after a charged current interaction with atomic nuclei. These charged leptons keep the same direction of the original neutrino and they can exit the Earth. When they exit the Earth, they will be detected by the Pierre Auger Observatory. We show, finally, that very small number of neutrinos crossing the Earth will be detected. However, even the observation of one single event in many years will be an indication of the existence of a neutrino flux. Moreover, it would be the beginning of a new phase in the cosmic ray detection.
Mestre
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Le, Coz Sandra. "Radiodétection des gerbes atmosphériques à l'observatoire Pierre Auger." Thesis, Grenoble, 2014. http://www.theses.fr/2014GRENY073/document.
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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 attendusThe 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
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Niemietz, Lukas [Verfasser]. "Lightning Detection at the Pierre-Auger-Observatory / Lukas Niemietz." Wuppertal : Universitätsbibliothek Wuppertal, 2017. http://d-nb.info/1144397537/34.
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Maller, Jennifer. "Caractérisation de signaux transitoires radio à l'observatoire Pierre Auger." Thesis, Nantes, Ecole des Mines, 2014. http://www.theses.fr/2014EMNA0186/document.
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Après plus d'un siècle d'études, l'origine des rayons cosmiques d’ultra-haute énergie reste mal comprise. En améliorant la connaissance de la composition des rayons cosmiques détectés sur Terre, il est possible de contraindre les modèles concernant leur origine, ainsi que leur mécanisme de production dans les sources astrophysiques. Les simulations montrent que le champ électrique émis par les gerbes est sensible à leur développement dans l'atmosphère. Ce champ électrique peut être mesuré avec un cycle utile élevé, faisant du signal radio une observable prometteuse pour identifier le rayon cosmique primaire. Le signal radio permet également de mesurer sa direction d'arrivée et son énergie. Depuis 2006, l'observatoire Pierre Auger accueille plusieurs réseaux de radio détection des rayons cosmiques. Des démonstrateurs équipés de quelques stations (RAuger,MAXIMA) ont permis une caractérisation efficace de l'environnement radio du site, ils ont également apporté des contraintes sur les mécanismes responsables de l'émission du champ électrique par les gerbes dans le domaine du MHz. Les prototypes ont mené à la construction d’AERA (Auger Engineering Radio Array) qui, avec 124 stations couvrant 6 km², est le premier réseau grande échelle de radio détection des gerbes dans le domaine du MHz. AERA est déployé dans l'extension basse énergie de l'observatoire afin de bénéficier d'une statistique plus importante. Le réseau permet d'intéressantes mesures hybrides ; son emplacement permet en effet de croiser les données obtenues par la radio avec celles provenant du réseau de surface (SD) et des télescopes à fluorescence (FD) proches du réseau. Cette thèse est dédiée à la caractérisation de signaux transitoires radio détectés par RAuger et AERA. Comme un des défis de la radio détection des gerbes atmosphériques est de supprimer les bruits de fond anthropiques causant des déclenchements accidentels, des méthodes de réjection du bruit de fond et de sélection des coïncidences SD-AERA ont été développées. Une étude de la corrélation entre le développement de la gerbe dans l'atmosphère (profil longitudinal) et le champ électrique mesuré par les stations radio est également présentée. Cette étude valide le lien direct entre le champ électrique et le développement de la gerbe dans l'atmosphère et confirme l’intérêt du signal radio pour l’estimation de la nature des rayons cosmiques d'ultra-haute énergieAfter more than a century of studies, one of the challenging questions related to ultra-high energy cosmic rays concerns their nature, which remains unclear. Improving the knowledge about the composition of cosmic rays will permit to constrain the models concerning their origins and the production mechanisms in the astrophysical sources. Simulations show that, the electric field emitted by the shower is sensitive to its development. This electric-field can be measured with a high duty cycle, and thus is apromising technique to identify an observable sensitive to the nature of the primary cosmic ray. The radio signal is also used to measure its arrival direction and its energy. Since 2006, the Pierre Auger Observatory hosts several radio detection arrays of cosmic rays, starting from small size prototypes (RAuger, MAXIMA) to achieve a large scale array of 124 radio stations: AERA, the Auger Engineering Radio Array covering 6 km². These different arrays allow the study of the radio emission during the development of the shower in the MHz domain. AERA is deployed in the low energy extension of the Pierre Auger Observatory in order to have a larger statistics. It enables interesting hybrid measurements, with the comparison of radio observable with those obtained with the surface detector (SD) and the fluorescence telescopes close to the array. This thesis is dedicated to the characterization of the radio transient signals detected by RAuger and AERA. As one of the challenges of the radio detection of air-shower is to remove the anthropic background causing accidental triggering, methods for background rejection and SD-AERA coincidences selection have been developed. A study of the correlation between the shower development in the atmosphere (longitudinal profile) and the electric-field measured by the radio stations is also presented. This study shows the relationship between the electric-field and the shower development in the atmosphere and confirms that the radio signal is a powerful tool to study the nature of the ultra-high energy cosmic rays
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Oliveira, Jaime Souza de. "Estudo em multirresolução de anisotropias nas direções de chegada dos raios cósmicos detectados no Observatório Pierre Auger." Niterói, 2017. https://app.uff.br/riuff/handle/1/2938.
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Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Coordenação de Aperfeiçoamento de Pessoal de Nível Superior
Conselho Nacional de Desenvolvimento Científico e Tecnológico
O início deste estudo de doutorado, em 2012, coincidiu com a celebração do primeiro centenário da descoberta da radiação cósmica. Embora nosso conhecimento sobre estas partículas tenha aumentando consideravelmente ao longo do último século, ainda há muitas questões que necessitam ser elucidadas, principalmente para aquelas com energias acima de 1018 eV, denominadas raios cósmicos de energia ultra alta. A razão para isso é que o fluxo destas partículas é extremamente pequeno, indo de uma partícula por km2 por ano, na faixa de energia de 1018 eV, a uma partícula por km2 por século, em energias ainda mais elevadas. Para compensar este baixo fluxo de partículas, foram construídos observatórios enormes nas últimas décadas, sendo o maior deles, o Observatório Pierre Auger, foco dos estudos realizados nesta tese. Embora o Observatório Auger, em operação desde 2004, venha realizando descobertas significativas com respeito aos raios cósmicos ultra-energéticos, ainda não se sabe, de maneira indubitável, quais são suas fontes, composição química, mecanismos de aceleração e propagação. Em especial, o estudo de anisotropias nas direções de chegada dos raios cósmicos à Terra é de fundamental importância para o entendimento destas questões. Assim, a principal contribuição desta tese trata de um estudo em multirresolução de anisotropias no fluxo dos raios cósmicos detectados no Observatório Auger, com energias acima de 4×1018 eV. Para isso, medidas do espectro de potência angular foram realizadas sob nossa responsabilidade, enquanto que uma análise complementar, utilizando needlets, foi empregada por um grupo de físicos da Universidade de Aachen, Alemanha. Ainda no contexto de anisotropia, destacamos um outro estudo realizado nesta tese, no qual mostramos não haver inconsistência entre resultados obtidos em duas análises distintas, uma usando somente dados da Colaboração Auger e outra usando também dados da Colaboração Telescope Array. Adicionalmente, também descrevemos um estudo relacionado ao aprimoramento dos detectores de superfície do Observatório Pierre Auger, no qual mostramos que os tanques de radiação Cherenkov podem ser calibrados e terem sua performance avaliada com a colocação de um detector de múons sob eles.
In 2012, the beginning of this Ph.D study coincided with the celebration of the first centenary of the cosmic radiation discovery. Although our knowledge these particles has increased considerably over the last century, there are still many issues to be clarified, particularly for those with energies above 1018 eV, called ultra high energy cosmic rays. The reason for this is that the flux of these particles is extremely low, from one particle per km2 per year at 1018 eV to one particle per km2 per century at even higher energies. In order to compensate this very low flux of particles, large observatories were built in recent decades. The largest one is the Pierre Auger Observatory, focus of the studies performed in this thesis. Although the Auger Observatory, in operation since 2004, has been reporting breakthroughs with regard to ultra-high energy cosmic rays, there is still no consensus related to their sources, chemical composition, acceleration and propagation mechanisms. Particularly, the study of anisotropies in the cosmic ray arrival directions is of fundamental importance for the understanding of these issues. Thus, the main contribution of this thesis is a multi-resolution anisotropy study of the cosmic ray flux detected in the Auger Observatory with energies above 4 × 1018 eV. To this goal, the angular power spectrum were performed under our responsibility, while one additional analysis, using needlets, was used by a group from Aachen University, Germany. Still within the context of anisotropy, we reported another study of this thesis, in which it was shown that there is no inconsistency between results obtained in two different analysis, one using only data obtained by the Auger Collaboration and another one using events from Auger and Telescope Array collaborations. In addition, we also described a different study related to the upgrade of the surface detectors of the Pierre Auger Observatory, in which we showed that the water Cherenkov tanks can be studied and calibrated by placing a muon detector under them.
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Souto, Bruno Fontes. "Anisotropia de raios cósmicos no âmbito do Observatório Pierre Auger." [s.n.], 2010. http://repositorio.unicamp.br/jspui/handle/REPOSIP/277498.
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Orientador: Carola Dobrigkeit ChinellatoDissertação (mestrado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin
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Resumo: O objetivo deste trabalho é aplicar umteste que visa determinar se as direções de chegada dos raios cósmicos de energias mais altas (> 1019 eV) observados pelo Observatório Pierre Auger seguem uma distribuição isotrópica. Sua principal vantagem é dispensar o uso de catálogos de objetos astrofísicos. Igualmente, procura-se uma correlação das direções de chegada com a região conhecida como Plano Supergaláctico. Dá-se ênfase na motivação, interpretação e na visão geral sobre anisotropia de raios cósmicos surgida nos últimos anos. O resultado obtido com os dados atuais neste trabalho é que de fato existe uma anisotropia nas direções de chegada, embora esta ainda seja difícil de caracterizar
Abstract: In this work, we apply a test designed to answer the question of whether the arrival directions of the highest energy (> 1019 eV) events observed by the Pierre Auger Observatory are consistent with being drawn from an isotropic distribution. Its main advantage is that the method does not rely on any catalogue of astrophysical objects. Furthermore, a correlation of the arrival directions with the region known as Supergalactic Plane is investigated. Emphasis is put on motivation, interpretation and on the global picture of cosmic ray anisotropy that has emerged during the last years. The result found so far from the current data in this work is that an anisotropy in the arrival directions indeed exists, even so it is still difficult to characterize
Mestrado
Raios Cósmicos
Mestre em Física
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Martins, Victor Barbosa. "RPCs design, development and tests for the Pierre Auger Observatory." Universidade de São Paulo, 2018. http://www.teses.usp.br/teses/disponiveis/76/76132/tde-26092018-083023/.
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The cosmic rays are the most energetic particles in the universe. Their production, propagation, and detection are objects of studies. Surface detectors aim to identify particles from extensive air showers (EAS) which the result from the cosmic-ray interactions with the atmosphere. Resistive Plate Chambers (RPCs) have shown to be a suitable muon detector to be integrated into the Pierre Auger Observatory. An instrumentation was developed to assembly RPCs in São Carlos (BRA). Data from RPCs already built by our collaborators in Coimbra (POR) were analyzed. The detector efficiency to muons was calculated and is approximately 88%, which is in good agreement with the values quoted in the literature. Direction maps were built to investigate the muon incoming direction and the quantity of matter traversed by the muons. The dependence of the muon flux on the zenith angle was calculated and compared with results from the simulation. A square cosine dependence is expected, though it is seen that the building structure has enough matter to block some of the incident muons and alter the dependence curve. The total muon flux was estimated based on the detector efficiencies and solid angle as 1.6.10−5. mm−2.sr−1. s−1 compared with the literature value of 7.1.10−5 mm−2.sr−1.s−1, which gives an absorption by the building of approximately 77%.Os raios cósmicos são as partículas mais energéticas do universo. Sua produção, propagação e detecção são objetos de estudos. Os detectores de superfície têm como objetivo identificar partículas dos chuveiros atmosféricos extensos (EAS), o qual é o resultado das interações do raio cósmico com a atmosfera. A Câmaras de Placas Resistivas (RPCs) demonstra ser um detector de múons adequado para ser integrado ao Observatório Pierre Auger. Foi desenvolvida em São Carlos (BRA) uma instrumentação para montagem de RPCs. Dados de RPCs já construídas por nossos colaboradores em Coimbra (POR) foram analisados. A eficiência dos detectores para múons foi calculada como sendo de aproximadamente 88%, o que está de acordo com os valores citados na literatura. Mapas de direção foram construídos para investigar a direção de chegada e a quantidade de matéria atravessada pelos múons. A dependência do fluxo de múons com o ângulo zenital foi comparada com os resultados da simulação. Embora uma dependência com o quadrado do cosseno é esperada, foi constatado que a estrutura do prédio tem matéria suficiente para bloquear parte dos múons incidentes e alterar a curva da dependência. O fluxo total de múons foi estimado baseado nas eficiências do detector e no ângulo sólido é de 1.6.10−5 mm−2.sr−1.s−1. Comparado com o valor da literatura de 7.1.10−5 mm−2.sr−1.s−1 resulta em uma absorção pelo prédio de aproximadamente 77% do fluxo de múons.
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Tartare, Mathieu. "Etude des neutrinos d'ultra-haute énergie à l'observatoire Pierre Auger." Thesis, Grenoble, 2013. http://www.theses.fr/2013GRENY038/document.
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Près d'un siècle après leur découverte, les rayons cosmiques sont encore sujets à de nombreuses interrogations. À ultra-haute énergie (UHE), leur nature, leur origine et leur mécanisme de production restent encore inconnus malgré les avancées expérimentales. L'observatoire Pierre Auger est actuellement l'expérience incontournable pour tenter de répondre à ces questions. Dans ce contexte, l'étude et la recherche de neutrinos à UHE sont susceptibles d'apporter des informations encore manquantes au puzzle des rayons cosmiques d'ultra-haute énergie, notamment quant à leur mécanisme de production ou leur origine. C'est dans ce cadre que s'inscrit cette thèse, centrée sur la recherche de neutrinos à UHE à l'observatoire Pierre Auger et plus particulièrement sur l'étude des neutrinos arrivant sous l'horizon (i.e. à incidence rasante) et interagissant dans la croûte terrestre. Dans une première partie, le contexte phénoménologique et expérimental dans lequel s'inscrit cette thèse est introduit. Dans une seconde partie, nous présenterons tout d'abord notre étude des incertitudes systématiques sur les modèles d'interactions à UHE des neutrinos et des leptons tau à travers une analyse revisitée des neutrinos tau à incidence rasante. Cette étude s'inscrit dans le cadre de la combinaison des résultats des différents canaux de détection de l'observatoire qui a permis de poser une limite compétitive sur les flux de neutrinos à UHE, au delà de la limite de Waxman et Bahcall. Nous présenterons ensuite notre travail effectué sur les neutrinos électroniques à incidence rasante. Ces derniers engendrent, en interagissant dans la croûte terrestre, des gerbes électromagnétiques souterraines soumises à l'effet LPM (Landau, Pomeranchuk et Migdal) qui entraîne un retard de leur développement et augmente leur probabilité de détection. Une chaîne complète de simulation de ce canal a été développée afin d'évaluer la sensibilité de l'observatoire à ces évènements. Enfin, dans le cadre de propositions d'améliorations de l'observatoire en vue d'accroître ses performances à partir de 2015, nous présentons l'étude que nous avons effectuée sur l'impact d'une nouvelle électronique d'acquisition et de nouveaux modes de déclenchements sur l'efficacité de détection des neutrinos à incidence rasante par les stations du réseau au solNearly one century after their discovery, cosmic rays are still subject to many questions. In particular at ultra-high energy (UHE) where their nature, origin and production mechanism are still unknown despite numerous experimental advances. The Pierre Auger observatory is currently the key experiment to try to answer these questions. In this context, the search for UHE neutrinos remains a major challenge for astroparticle physics. Their study is likely to bring informations that are still missing to the ultra-high energy cosmic ray puzzle regarding their origin and production mechanism. This thesis focuses on the search for UHE neutrinos at the Pierre Auger observatory and particularly on neutrinos arriving below the horizon (i.e. earth skimming) and interacting in the earth crust. In a first part, the phenomenological and experimental context is introduced. In a second part, we first present our study of systematic uncertainies on interactions models of UHE neutrinos and tau lepton through a revisited analysis of earth skimming tau neutrinos in the context of the combination of the results of the different observatory's detection channels. This combination allowed to put a competitive limit on the UHE neutrinos flux, beyond the Waxman and Bachal limit. We will then show our work on earth skimming electron neutrinos. They produce, by interacting in the earth crust, underground electromagnetic showers subject to the LPM (Landau, Pomeranchuk and Migdal) effet which causes a delay in their development and increaase their detection probability. A complete simulation chain of this channel was developed in order to estimate the sensitivity of the observatory to such events. Finally, in the context of proposals to upgrade the observatory in order to improve its performance beyond 2015, we present the study we have performed about the impact of a new acquisition electronic and new triggers on the earth skimming neutrinos detection efficiency by the stations of the ground array
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Almeida, Rogerio Menezes de. "Estudo de anisotropias de UHECR's em dados do Observatório Pierre Auger." [s.n.], 2009. http://repositorio.unicamp.br/jspui/handle/REPOSIP/277718.
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Orientador: Ernesto KempTese (doutorado) - Universidade Estadual de Campinas, Instituto de Fisica Gleb Wataghin
Made available in DSpace on 2018-08-14T11:18:31Z (GMT). No. of bitstreams: 1 Almeida_RogerioMenezesde_D.pdf: 29880310 bytes, checksum: a6d709505699fa646136930c8822d569 (MD5) Previous issue date: 2009
Resumo: Quase um século após o descobrimento da radiação cósmica, sua origem, composilção, mecanismos de aceleração e propagação pelo universo são ainda desconhecidos para a faixa de energia ultra-alta (E >~ 10 18 eV). O mistério torna-se ainda maior devido à supressão (corte GZK) no uxo dos raios cósmicos com energias E >~ 6 × 10 19 eV, devido à interação destas partículas com a radiação cósmica de fundo, previsto há cerca de 40 anos. Assim, espera-se que os raios cósmicos com energia acima deste limiar sejam provenientes de fontes distantes em até ~ 200 Mpc. Uma vez que nosso universo local é bastante heterogêneo e a rigidez magnética destas partículas é bastante elevada, espera-se que a distribuição das direções de chegada dos raios cósmicos de energia ultra-alta possa ser correlacionada com as direções de suas fontes, refletindo a anisotropia do universo local. Neste sentido, estudos de anisotropias nas direções de chegadas de tais partículas desempenham papel crucial na investigação da radiação cósmica e compreensão do universo. Este trabalho dedica-se ao estudo de anisotropias de pequena e larga escalas. No primeiro caso, procuramos UHECR¿s correlacionados com o surto gigante de radiação gama emitido pelo SGR 1806-20 em dezembro de 2004. Outro caso estudado é a análise de direções da esfera celeste com excessos de raios gama com significâncias estatísticas maiores que 4s, não associadas a fontes conhecidas, reportadas pela Colaboração JANZOS. Ainda com relação a anisotropias de pequena escala, são estudadas aplicações de filtros de wavelets para detecção de fontes pontuais. No contexto de anisotropias de larga escala, relacionadas a grandes distribuições de matéria, desenvolvemos um método de identificação de anisotropias independente de catálogos de objetos celestes, chamado MIIE. Testamos sua eficiência através de testes de hipóteses e o aplicamos a conjunto de eventos com energia extrema obtidos de dados do Observatório Pierre Auger
Abstract: Almost a century after the discovery of cosmic radiation, their origin, composition, acceleration and propagation mechanisms in the universe is still unknown for the ultra-high energy component ( > ~ 1018 eV). The mystery grows due to the suppression (GZK cutoff) in the ux of cosmic rays with energies E >~ 6 × 10 19 eV, caused by the interaction of these particles and the cosmic microwave background, predicted ~ 40 years ago. Thus, it is expected that cosmic rays with energy above this threshold are produced in sources within ~ 200 Mpc. Since our local universe is very inhomogeneous and the magnetic rigidity of these particles is very high, it is expected that the distribution of the arrival directions of ultra-high energy cosmic rays can be correlated with the directions of their sources, reflecting the anisotropy of our local universe. In this way, anisotropy studies play crucial role in the research of cosmic radiation and understanding of the universe. In this work, small-scale anisotropy, related to the study of point sources, are studied searching for UHECR¿s correlated with the giant are from SGR 1806-20 in December 2004. We have also analized directions with an excess of gamma rays with statistical significance S > 4s, not associated with any known sources, reported by the JANZOS Collaboration. Also, in this thesis wavelets are applied in the detection of point sources. In the context of anisotropy related to large distributions of matter, called large scale anisotropy, we propose a new anisotropy identification method independent of catalogs, so-called MIIE. We test its efficiency through hipothesis tests and apply it to events set obtained from the Pierre Auger data
Doutorado
Física das Particulas Elementares e Campos
Doutor em Ciências
Books on the topic "Auger, Pierre"
Book chapters on the topic "Auger, Pierre"
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Bluemer, Johannes. "Status and Perspectives of the Pierre Auger Observatory." In Beyond the Desert 2003, 801–18. Berlin, Heidelberg: Springer Berlin Heidelberg, 2004. http://dx.doi.org/10.1007/978-3-642-18534-2_53.
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Pimenta, M. "The Study of Ultra High Energy Cosmic Rays in the Pierre Auger Observatory." In NATO Science for Peace and Security Series B: Physics and Biophysics, 205–15. Dordrecht: Springer Netherlands, 2009. http://dx.doi.org/10.1007/978-90-481-2287-5_20.
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Courouau, Jean-François. "Le moi autobiographique dans la poésie languedocienne des XVIe et XVIIe siècles (Auger Gaillard, Pierre Godolin)." In Car c’est moy que je peins, 239–60. Presses universitaires du Midi, 2010. http://dx.doi.org/10.4000/books.pumi.39456.
Full textConference papers on the topic "Auger, Pierre"
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de Souza, Vitor. "Pierre Auger Observatory." In 4th School on Cosmic Rays and Astrophysics. Trieste, Italy: Sissa Medialab, 2011. http://dx.doi.org/10.22323/1.118.0026.
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Arteaga Velázquez, J. C. "The Pierre Auger Observatory." In INSTRUMENTATION IN ELEMENTARY PARTICLE PHYSICS. AIP, 2003. http://dx.doi.org/10.1063/1.1604092.
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Zepeda, Arnulfo. "The Pierre Auger observatory." In PARTICLES AND FIELDS: Seventh Mexican Workshop. American Institute of Physics, 2000. http://dx.doi.org/10.1063/1.1315049.
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Mantsch, Paul M. "The Pierre Auger project." In Workshops on particles and fields and phenomenology of fundamental interactions. AIP, 1996. http://dx.doi.org/10.1063/1.49731.
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Arteaga-Velázquez, J. C. "The Pierre Auger Observatory." In PARTICLES AND FIELDS: Tenth Mexican School on Particles and Fields. AIP, 2003. http://dx.doi.org/10.1063/1.1594374.
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Hojvat, Carlos. "The Pierre Auger Observatory." In First Latin American symposium on high energy physics and The VII Mexican School of Particles and Fields. AIP, 1997. http://dx.doi.org/10.1063/1.53255.
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Swain, John. "The Pierre Auger Observatory." In INTERSECTIONS OF PARTICLE AND NUCLEAR PHYSICS: 8th Conference CIPANP2003. AIP, 2004. http://dx.doi.org/10.1063/1.1664259.
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Giller, Maria. "The Pierre Auger Observatory." In ASTROPHYSICAL SOURCES OF HIGH ENERGY PARTICLES AND RADIATION. AIP, 2005. http://dx.doi.org/10.1063/1.2141837.
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Martello, Daniele. "The Pierre Auger Observatory Upgrade." In 35th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.0383.
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Caccianiga, Lorenzo. "The Pierre Auger Observatory highlights." In XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop. Trieste, Italy: Sissa Medialab, 2018. http://dx.doi.org/10.22323/1.306.0029.
Full textReports on the topic "Auger, Pierre"
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Mantsch, Paul M., and /Fermilab. Auger North: The Pierre Auger Observatory in the Northern Hemisphere. Office of Scientific and Technical Information (OSTI), January 2009. http://dx.doi.org/10.2172/993867.
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Aab, Alexander. The Pierre Auger Observatory Upgrade - Preliminary Design Report. Office of Scientific and Technical Information (OSTI), April 2016. http://dx.doi.org/10.2172/1250882.
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Gichaba, Justus Ogwoka. Measurements of TYVEK reflective properties for the Pierre Auger Project. Office of Scientific and Technical Information (OSTI), August 1998. http://dx.doi.org/10.2172/15017207.
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Molina Bueno, Laura. Measurement of the Muon Atmospheric Production Depth with the Water Cherenkov Detectors of the Pierre Auger Observatory. Office of Scientific and Technical Information (OSTI), September 2015. http://dx.doi.org/10.2172/1248227.
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Collica, Laura. Mass composition studies of Ultra High Energy cosmic rays through the measurement of the Muon Production Depths at the Pierre Auger Observatory. Office of Scientific and Technical Information (OSTI), January 2014. http://dx.doi.org/10.2172/1249492.
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Döring, Thomas, and Birgit Aigner-Walder. Verkehrs-, umwelt- und raumbezogene Aspekte der Elektromobilität unter Berücksichtigung entscheidungstheoretischer Überlegungen zum Nutzerverhalten. Sonderforschungsgruppe Institutionenanalyse, 2015. http://dx.doi.org/10.46850/sofia.9783941627468.
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Zweifelsohne wirken sich neue Technologien auf die Alltagsmobilität einschließlich der Wahl verfügbarer Verkehrsmitteln aus und implizieren damit verkehrs- umwelt- und raumbezogene Folgen. Der massenhafte Anstieg der individuellen Pkw-Nutzung der zurückliegenden Jahrzehnte wird weitestgehend auf strukturelle Veränderungen zurückgeführt, die sich aus dem Zusammenwirken von technologischer Möglichkeit (hier: der Option „Pkw“) und allgemeinen ökonomischen und sozialen Entwicklungstrends in modernen Industriegesellschaften ergeben (vgl. exemplarisch Kutter 2001; Kutter/Stein 1998). Insbesondere bezogen auf die soziale Akzeptanz von technischen Neuerungen – ökonomisch gesprochen: die Substitutionsbereitschaft zwischen bestehenden und neuen Technologien – muss jedoch die Perspektive des Akteurs und sein individuelles Entscheidungsverhalten stärker in den Blick genommen werden, um die für Verkehr, Umwelt und Raum sich ergebenden Folgen besser abschätzen zu können. Entsprechende Studien, die das individuelle Entscheidungsverhalten im Umgang mit technologischen Neuerungen ins Zentrum der Untersuchung stellen, sind jedoch nach wie vor nur in geringer Zahl vorhanden. So steht beispielsweise außer Frage, dass Neuerungen im Bereich von IuK-Technologien die physische Mobilität nachhaltig beeinträchtigen werden. Gleichwohl sind die vorhandenen theoretischen wie empirischen Befunde der Mobilitätsforschung, wie die Entwicklung von IuK-Technologien die individuelle Mobilitätsnachfrage verändern wird, jedoch unklar oder widersprüchlich. Entsprechend stellt etwa Bamberg (2010) fest: „Die Dynamik dieser Entwicklung ist z.Z. kaum prognostizierbar“. Vor diesem Hintergrund hat unter anderen das Institut für Mobilitätsforschung (ifmo) in Kooperation mit dem Imperial College London jüngst eine Grundlagenstudie gestartet, um den Stand des Wissens zum Einfluss von IuK-Technologien auf das Mobilitätsverhalten aufzuarbeiten. Ein ähnlicher Erkenntnisstand lässt sich für andere verkehrs- und mobilitätsrelevante Technologiebereiche diagnostizieren. Eine der wenigen Ausnahmen hiervon bilden Analysen des Nutzerverhaltens bezogen auf die Akzeptanz neuer Antriebstechnologien im Bereich des motorisierten Individualverkehrs und hier speziell mit Blick auf die Nutzung elektrisch betriebener Fahrzeuge (vgl. stellvertretend Bongard 2014; Fazel 2014; Peters et al. 2013; Haugrund 2013; Pieper et al. 2013; Paternoga et al. 2013; Dudenhöffer et al. 2012; Döring/Aigner 2012; Döring 2012; Ahrend et al. 2011; Peters/Hoffmann 2011; Döring/Aigner 2011). Zu den Elektrofahrzeugen zählen dabeiterminologisch nicht alllein reine batterieelektrisch betriebene Fahrzeuge (BEV), sondern auch solche Elektrofahrzeuge, die entweder über einen Verbrennungsmotor zur Reichweitenverlängerung verfügen (REEV) oder bei denen sowohl ein E-Motor als auch ein Verbrennungsmotor für den Antrieb sorgt, wie dies bei den am Stromnetz aufladbaren Plugin-Hybridfahrzeugen (PHEV) der Fall ist. Schließlich werden zudem Brennstoffzellenfahrzeuge (FCEV), welche die benötigte Energie direkt an Bord des Fahrzeugs erzeugen (z.B. in Form von Wasserstoffbrennstoffzellen), zu den Elektrofahrzeugen gezählt. In Anbetracht dessen sollen nachfolgend exemplarisch die vorhandenen Einsichten zum Nutzerverhalten im Umgang mit der Elektromobilität zusammenfassend dargestellt sowie – wenngleich nur ansatzweise und damit in lediglich rudimentärer Form – einige sich daraus ergebende verkehrs-, umwelt- und raumbezogene Implikationen aufgezeigt werden.