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Hakmana, Witharana Sampath S. "Development of Cosmic Ray Simulation Program -- Earth Cosmic Ray Shower (ECRS)." Digital Archive @ GSU, 2007. http://digitalarchive.gsu.edu/phy_astr_diss/12.
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ECRS is a program for the detailed simulation of extensive air shower initiated by high energy cosmic ray particles. In this dissertation work, a Geant4 based ECRS simulation was designed and developed to study secondary cosmic ray particle showers in the full range of Earth's atmosphere. A proper atmospheric air density and geomagnetic field are implemented in order to correctly simulate the charged particles interactions in the Earth's atmosphere. The initial simulation was done for the Atlanta (33.460 N , 84.250 W) region. Four different types of primary proton energies (109, 1010, 1011 and 1012 eV) were considered to determine the secondary particle distribution at the Earth's surface. The geomagnetic field and atmospheric air density have considerable effects on the muon particle distribution at the Earth's surface. The muon charge ratio at the Earth's surface was studied with ECRS simulation for two different geomagnetic locations: Atlanta, Georgia, USA and Lynn Lake, Manitoba, Canada. The simulation results are shown in excellent agreement with the data from NMSU-WIZARD/CAPRICE and BESS experiments at Lynn Lake. At low momentum, ground level muon charge ratios show latitude dependent geomagnetic effects for both Atlanta and Lynn Lake from the simulation. The simulated charge ratio is 1.20 ± 0.05 (without geomagnetic field), 1.12 ± 0.05 (with geomagnetic field) for Atlanta and 1.22 ± 0.04 (with geomagnetic field) for Lynn Lake. These types of studies are very important for analyzing secondary cosmic ray muon flux distribution at the Earth's surface and can be used to study the atmospheric neutrino oscillations.
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張增 and Tsang Cheung. "Primary cosmic ray composition at 10 [to the power] 15--10 [to the power] 17eV studied from extensive air shower simulations." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1985. http://hub.hku.hk/bib/B31230593.
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Cheung, Tsang. "Primary cosmic ray composition at 10 [to the power] 15--10 [to the power] 17eV studied from extensive air shower simulations /." [Hong Kong : University of Hong Kong], 1985. http://sunzi.lib.hku.hk/hkuto/record.jsp?B12266176.
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Rol, Jan. "Characterization of monopole induced air showers using CORSIKA." Thesis, Uppsala universitet, Högenergifysik, 2017. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-328049.
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In this thesis a characterization of air showers induced by magnetic monopoles is presented. Monopoles are predicted to exist and be accelerated to relativistic velocities. High energy monopoles traversing earth’s atmosphere continuously deposit energy, inducing an air shower. These air showers have been described based on simulations run in CORSIKA. It was found that monopole air showers are continuous; they plateau after the shower maximum, and have a large electromagnetic component. As such,they can easily be distinguished from normal cosmic rays and most other air shower sources. Very high energy photons and muons could induce similar showers but do not produce identical signals in track-following detectors such as IceCube.
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Chen, Chuxing. "Local atmospheric electricity and its possible application in high-energy cosmic ray air shower detection." Diss., The University of Arizona, 1989. http://hdl.handle.net/10150/184799.
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We have conducted an extensive experimental study on the subject of near ground atmospheric electricity. The main objective was to gain more understanding of this particular aspect of atmospheric phenomena, while testing the possible application to cosmic ray research. The results in atmospheric electricity show that there are certain patterns in ion grouping such as the size and lifetime. The average lifetime of ion group is 0.7 seconds and the average size is about 10 meters at our experimental site. Ultrahigh energy cosmic ray air showers should create sizable slow atmospheric electric pulses according to our theoretical calculations. Preliminary studies on air showers with total particle number N equal or greater than 10⁵ (10¹⁵ eV) have yielded strong evidence that slow atmospheric current pulses are associated with air showers. The theory and the experiment agree with each other fairly well when we average over large numbers of events. With our current experimental arrangement, when the air shower exceeds a certain size, the system response saturates. Therefore it is extremely desirable in future research that the counter array be designed for a much higher threshold level, since this prototype experiment indicates that interesting data would be obtained. Another reason for further experimental research being directed toward ultrahigh energy, e.g., N ≥ 10⁷ (10¹⁷ eV) and higher, is to establish a calibration of the slow atmospheric electric signals generated by cosmic rays as a function of primary cosmic ray energy and core location. This type of slow atmospheric electric signal, if fully understood and calibrated, offers a new and potentially less expensive technique to observe ultrahigh energy cosmic ray events, which hold some fundamental keys to the knowledge of the universe on a large scale.
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Palmieri, Nunzia [Verfasser], and J. [Akademischer Betreuer] Blümer. "Determination of energy and mass of cosmic rays using air shower radio emission / Nunzia Palmieri. Betreuer: J. Blümer." Karlsruhe : KIT-Bibliothek, 2012. http://d-nb.info/1032946709/34.
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Maurel, Detlef [Verfasser], and J. [Akademischer Betreuer] Blümer. "Mass composition of ultra-high energy cosmic rays based on air shower universality / Detlef Maurel. Betreuer: J. Blümer." Karlsruhe : KIT-Bibliothek, 2013. http://d-nb.info/1044956178/34.
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Stapleton, James C. "Ultra-High Energy Cosmic Rays: Composition, Early Air Shower Interactions, and Xmax Skewness." The Ohio State University, 2015. http://rave.ohiolink.edu/etdc/view?acc_num=osu1431044195.
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Bridgeman, Ariel [Verfasser], and J. [Akademischer Betreuer] Blümer. "Determining the Mass Composition of Ultra-high Energy Cosmic Rays Using Air Shower Universality / Ariel Bridgeman ; Betreuer: J. Blümer." Karlsruhe : KIT-Bibliothek, 2018. http://d-nb.info/1166234266/34.
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Schoo, Sven [Verfasser], and J. [Akademischer Betreuer] Blümer. "Energy Spectrum and Mass Composition of Cosmic Rays and How to Publish Air-Shower Data / Sven Schoo. Betreuer: J. Blümer." Karlsruhe : KIT-Bibliothek, 2016. http://d-nb.info/110632997X/34.
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Smith, Benjamin Edward. "The mass composition of cosmic rays above 1 EeV inferred using the spread in arrival times of air shower particles." Thesis, University of Leeds, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.487779.
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The sources of ultra high energy cosmic rays (UHECRS) have remained undetected for over half a century. Identifying these sources could be made easier by measuring the charge and thus mass of UHECRs, as this would allow for corrections in their arrival directions due to deflections introduced by intervening magnetic fields to take place. The aim of this thesis is to derive a parameter which can be used as a surrogate for depth )f maximum in the data obtained using the surface array of the Auger Observatory for the measurement of the mass composition of UHECRs.
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Gottowik, Marvin [Verfasser]. "Radio Hybrid Reconstruction and Analysis of Inclined Air Showers with AERA of the Pierre Auger Observatory - Measuring the Hadronic Shower Development and Cosmic Ray Mass Composition / Marvin Gottowik." Wuppertal : Universitätsbibliothek Wuppertal, 2021. http://d-nb.info/1240426313/34.
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Prado, Raul Ribeiro. "Experimental studies of the muonic component of extensive air showers." Universidade de São Paulo, 2018. http://www.teses.usp.br/teses/disponiveis/76/76131/tde-21062018-150629/.
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Ultra-High Energy Cosmic Rays (UHECR) can only be measured by the detection of Extensive Air Showers (EAS) created by the interaction of the cosmic ray particle with an atmospheric nuclei. The inference of some of the properties of UHECR, like their mass composition, is only possible by the comparison of measurements of EAS observables to predictions from Monte Carlo simulations. The most important source of uncertainties on the description of EAS by the simulations is the modeling of hadronic interactions. For many years it has been known that the hadronic interaction models fail on predicting the EAS observables related to their muonic component. The most evident manifestation of that is called muon deficit problem due to the fact that the number of muons in EAS with energies above 1018 eV predicted by simulations is smaller than the observed ones. The aim of this thesis is to approach this problem in three distinct fronts. First, a method is developed to interpret measurements of number of muons in terms of cosmic rays composition in despite of the muon deficit problem. Second, an EAS observable which is sensitive to the muon energy spectrum at ground and, consequently, can be used to constrain hadronic interaction models is proposed and tested. Third and final, the muon production in air showers is studied through measurements of hadron production spectra in pion-carbon interactions.Raios Cósmicos Ultra Energéticos (Ultra-High Energy Cosmic Rays, UHECR) somente podem ser medidos através da detecção dos Chuveiros Atmosféricos Extensos (Extensive Air Showers, EAS) criados pela interação do raio cósmico primário com núcleos atmoféricos. A inferência de algumas propriedados dos UHECRs, como a composição de massa, é possível somente através da comparação entre medidas de observáveis dos EASs com predições geradas por simulações de Monte Carlo. A fonte de incerteza mais importante na descrição de EAS por simulações é a modelagem das interações hadrônicas. Por muitos anos é sabido que os modelos de interação hadrônica falham na predição de observáveis dos EASs relacionados a sua componente muônica. A manifestação mais evidente disso é chamada problema do déficit de múons devido ao fato que o número de múons em chuveiros com energias acima de 1018 eV predito por simulações é menor que os observados. O objetivo desta tese é abordar este problema através de três frentes. Primeiramente, um método é desenvolvido para interpretar as medidas do número de múons em termos de composição de raios cósmicos considerando o problema do déficit de múons. Segundo, a proposta e o teste de um observável que é sensível ao espectro de energia dos múons na superfície e, consequentemente, pode ser usado para discriminar entre os modelos de interação hadrônica. Por último, a produção de múons em chuveiros é estudada através de medidas do espectro de produção de hádrons em interações do tipo píon-carbono.
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Zong, Zizhao. "Study of cosmic rays by Auger and LHAASO : R&D and Data Analysis of AugerPrime and simulations for LHAASO." Thesis, Université Paris-Saclay (ComUE), 2017. http://www.theses.fr/2017SACLS366/document.
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Les rayons cosmiques sont des particules chargées, ainsi que des coproduits comme les photons et les neutrinos, issus de sources de rayons cosmiques galactiques ou extragalactiques. Ils arrivent au sommet de l'atmosphère terrestre avec des énergies primaires allant jusqu'à quelques 10 EeV. Lorsque les rayons cosmiques entrent dans l'atmosphère, ils interagissent avec les molécules de l'air et produisent un grand nombre de particules secondaires, créant une gerbe atmosphérique (extensive air shower, EAS). Accompagné des particules secondaires, une émission de la lumière Cherenkov et de la lumière fluorescence est induite par le passage des particules dans l'atmosphère. L'Observatoire Pierre Auger et Large High Altitude Air Shower Observatory (LHAASO) sont des observatoires dédiés à la détection des gerbes atmosphériques dans le but de répondre aux questions ouvertes concernant les rayons cosmiques, mais se concentrant sur différentes gammes d'énergie, les plus hautes énergies et les énergies autour de quelques PeV. Après plus de 10 ans d'exploitation de l'Observatoire Pierre Auger, la collaboration Auger a proposé une amélioration des détecteurs de son réseau de surface, appelée "AugerPrime". Le but est d'augmenter la sensibilité à la masse des particules primaires en ajoutant un détecteur scintillateur sur le détecteur Cherenkov à eau. Les deux observatoires sont dits «hybrides» car composés de télescopes optiques observant le développement longitudinal des gerbes et des réseaux de détecteurs de surface échantillonnant leurs profils latéraux. Dans cette thèse, une série d'études contribuant aux projets AugerPrime et LHAASO sont présentées. En ce qui concerne le projet AugerPrime, la présente étude comprend le travail de recherche & développement des scintillateurs et l'analyse de données du réseau de tester. Pour le projet LHAASO, des simulations de télescopes Cherenkov et une analyse multivariée des observations hybrides pour l'identification des masses primaires sont présentéesCosmic rays are charged particles, as well as coproducts like photons and neutrinos, originated in cosmic-ray sources inside or outside the Galaxy. They arrive at the top of the Earth's atmosphere with primary energies of up to a few 10 EeV. When the cosmic rays enter the atmosphere, they interact with the molecules in the air and produce a large number of secondary particles, creating an extensive air shower (EAS). The ground-based observation of the EAS can be used to deduce the energy, the arrival direction, and the mass composition of cosmic rays. The Pierre Auger Observatory and the Large High Altitude Air Shower Observatory (LHAASO) are both EAS observatories aiming at solving open questions of cosmic-ray studies but focusing on different energy ranges, the highest-energy and the so-called knee (around few PeV) regions. Based on the experience gained during the operation of the Pierre Auger Observatory for more than 10 years, the Auger collaboration has proposed an upgrade project, called ''AugerPrime'', with the aim of increasing the sensitivity of the surface detector array to the primary mass of cosmic rays. Both observatories employ the so-called ''hybrid detector arrays'' composed of optical telescopes overlooking the longitudinal development and ground detector arrays sampling the signal densities in the lateral direction of the EAS. The ground detector arrays of both observatories are being constructed or upgraded to have various types of particle detectors (scintillator and water-Cherenkov detectors), which allow us to decompose the electromagnetic and muonic components of the EAS. In this thesis, a series of studies contributing to the AugerPrime and LHAASO projects are presented. Concerning the AugerPrime project, the present study includes R&D work of the scintillator detector and data analysis of the engineering array. For the LHAASO project, simulations of the wide field of view Cherenkov telescope array and a multivariate analysis of LHAASO-hybrid observations for the primary mass identification are presented
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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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Madani, Jamal Hamzah. "Extensive air showers." Thesis, Durham University, 1987. http://etheses.dur.ac.uk/6877/.
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A computerised 8-channel data acquisition unit constructed by the Durham University Microprocessor Unit is described and the calibration of this unit is given in chapter 2. A test for the data acquisition unit using a Geiger-Mul1er cosmic ray telescope is described in Chapter 3. In Chapter 4 the main experiment is described. Two plastic scintillation counters each of 0.4 area and 5cm thick in coincidence were used in this experiment to measure the density spectrum of electrons at sea level in the range 20 - 600 electrons per m(^2). The microcomputer data acquisition system is employed to record the scintillator pulse heights. The measured integral density spectrum has been used to calculate the integral size spectrum at sea level. A brief description of the theory of electron-photon cascades and the formation of extensive are showers is give in Chapter 5.A FORTRAN program which uses Monte Carlo method to simulate extensive air showers generated by high energy protons with a given energy is described in Chapter 6. Using the relation between primary energy and average number of electrons arriving at sea level found by Monte Carlo calculation in Chapter 6 an estimate has been made of the integral primary energy spectrum in the range lO(^14)-lQ(^16)eV, and the result is given in Chapter 7.
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Escudie, Antony. "From the observation of UHECR signal in [1-200] MHz to the composition with the CODALEMA and EXTASIS experiments." Thesis, Ecole nationale supérieure Mines-Télécom Atlantique Bretagne Pays de la Loire, 2019. http://www.theses.fr/2019IMTA0145/document.
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Malgré la découverte des rayons cosmiques il y a plus de cent ans, de nombreuses questions restent aujourd’hui sans réponse : que sont les rayons cosmiques, comment sont-ils créés et d’où viennent-ils ? Depuis 2002, l’instrument CODALEMA, basé sur le site de l’Observatoire de radio-astronomie de Nançay, étudie les rayons cosmiques d’ultra haute énergie (RCUHE, au delà de 1017 eV) qui arrivent dans l’atmosphère terrestre. Leur faible flux rend impossible une détection directe à ces énergies. Ces rayons cosmiques vont cependant interagir avec les atomes de l’atmosphère, engendrant une cascade de particules secondaires chargées communément appelée gerbe de particules, détectable depuis le sol, et dont on va extraire des informations sur le rayon cosmique primaire. L’objectif est de remonter aux caractéristiques du primaire ayant engendré la gerbe de particules, donc de déterminer sa direction d’arrivée, sa nature et son énergie. Lors du développement de la gerbe, les particules chargées en mouvement engendrent notamment l’émission d’une impulsion de champ électrique très brève, que CODALEMA détecte au sol avec des antennes radio dédiées, sur une large bande de fréquences (entre 1 et 200 MHz). L’avantage majeur de la radio-détection est sa sensibilité au profil complet de la gerbe et son cycle utile proche des 100 %, qui pourrait permettre d’augmenter le nombre d’évènements détectés à très haute énergie, et donc de mieux contraindre les propriétés des RCUHE. Au fil des ans, des efforts importants ont été consacrés à la compréhension de l’émission radio-électrique des grandes gerbes de particules dans la gamme [20-80] MHz mais, malgré certaines études menées jusqu’aux années 90, la bande [1-10] MHz est restée inutilisée pendant près de 30 ans. L’une des contributions de cette thèse porte sur l’expérience EXTASIS, adossée à CODALEMA, qui vise à ré-investiguer cette bande et à étudier la contribution dite de ”mort subite”, impulsion de champ électrique créé par les particules de la gerbe lors de leur arrivée et de leur disparition au sol. Nous présentons la configuration instrumentale d’EXTASIS, composée de 7 antennes basses fréquences exploitées dans [1.7-3.7] MHz, couvrant environ 1 km2. Nous rapportons l’observation, sur 2 ans, de 25 évènements détectés en coïncidence par CODALEMA et EXTASIS et estimons un seuil de détection de 23±4 μV/m à partir de comparaisons avec des simulations. Nous rapportons également une forte corrélation entre l’observation du signal basse fréquence et le champ électrique atmosphérique. L’autre contribution majeure de cette thèse porte sur l’étude du champ électrique émis par les gerbes et l’amélioration des performances du détecteur dans la bande [20-200] MHz. Nous proposons dans un premier temps une méthode de calibration des antennes de CODALEMA en utilisant l’émission radio de la Galaxie. Nous investiguons aussi plusieurs algorithmes de réjection de bruit afin d’améliorer la sélectivité des évènements enregistrés. Nous présentons ensuite une méthode de reconstruction des paramètres du rayon cosmique primaire, mettant en oeuvre des comparaisons combinant des informations de polarisation et fréquentielles entre les données enregistrées et des simulations, nous menant enfin à une proposition de composition en masse des rayons cosmiques détectésDespite the discovery of cosmic rays there are more than one hundred years ago, many questions remain unanswered today: what are cosmic rays, how are they created and where do they come from ? Since 2002, the CODALEMA instrument, located within the Nançay Radio Observatory, studies the ultra-high energy cosmic rays (UHECR, above 1017 eV) arriving in the Earth atmosphere. Their low flux makes it impossible to detect them directly at these energies. These cosmic rays, however, will interact with the atoms of the atmosphere, generating a cascade of secondary charged particles, commonly known as extensive air shower (EAS), detectable at ground level, and from which we will extract information on the primary cosmic ray. The objective is to go back to the characteristics of the primary that generated the EAS, thus to determine its direction of arrival, its nature and its energy. During the development of the shower, these charged particles in movement generate a fast electric field transient, detected at ground by CODALEMA with dedicated radio antennas over a wide frequency band (between 1 and 200 MHz). The major advantage of radio-detection is its sensibility to the whole profile of the shower and its duty cycle close to 100 %, which could increase the number of events detected at very high energy, and thus to better constrain the properties of the RCUHE. Over the years, significant efforts have been devoted to the understanding of the radio emission of extensive air shower (EAS) in the range [20-80] MHz but, despite some studies led until the nineties, the[1-10] MHz band has remained unused for nearly 30 years. One of the contributions of this thesis concerns the EXTASIS experiment, supported by the CODALEMA instrument, which aims to reinvestigate the [1-10] MHz band and to study the so-called ”sudden death” contribution, which is the expected impulsive electric field created by the particles at their arrival and their disappearance on the ground. We present the instrumental set up of EXTASIS, composed of 7 low frequency antennas exploited in [1.7-3.7] MHz, covering approximately 1 km2. We report the observation, over 2 years, of 25 low-frequency events detected in coincidence by CODALEMA and EXTASIS and estimate a detection limit of 23±4 μV/m from comparisons with simulations. We also report a strong correlation between the observation of the low frequency signal and the atmospheric electric field. The other major contribution of this thesis concerns the study of the electric field emitted by the EAS and the improvement of the detector’s performances in the [20-200] MHz band. First, we propose a calibration method for CODALEMA antennas using the radio emission of the Galaxy. We are also investigating several noise rejection algorithms to improve the selectivity of recorded events. We then present a method for reconstructing the parameters of the primary cosmic ray, implementing systematic comparisons combing polarization and frequency information between the recorded data and simulations, leading finally to a proposal for a mass composition of cosmic rays detected
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周志堅 and Chi-kin Chow. "Parameter estimation in small extensive air showers." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1993. http://hub.hku.hk/bib/B31211379.
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Chow, Chi-kin. "Parameter estimation in small extensive air showers /." [Hong Kong : University of Hong Kong], 1993. http://sunzi.lib.hku.hk/hkuto/record.jsp?B1363771X.
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Acton, Paul Darrell. "The Hadron component of cosmic-ray extensive air showers." Thesis, University of Leeds, 1989. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.328984.
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Filosa, Christopher. "Tomographie muonique : du développement de détecteurs à la résolution du problème inverse." Thesis, Université Paris-Saclay (ComUE), 2019. http://www.theses.fr/2019SACLS506.
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Cette thèse porte sur le développement des détecteurs gazeux Micromegas pour la tomographie muonique. Cette technique permet d’utiliser les muons cosmiques issus des interactions entre des rayons cosmiques et l’atmosphère, afin d’imager des objets de grandes dimensions et de grande opacité tels que des bâtiments, des dalles de béton, des volcans ou encore des pyramides comme la pyramide de Khéops en Égypte. En étudiant l’atténuation du flux de muons à travers un objet, nous pouvons obtenir des informations sur sa structure interne. Pour imager de telles structures et détecter les muons qui les traversent, des télescopes muoniques utilisant des détecteurs Micromegas sont utilisés. Les travaux effectués pendant cette thèse ont eu pour but d'améliorer les performances en résolution spatiale et en gaz de ces détecteurs.Un des objectifs de cette thèse a été d’imager une dalle de béton de 2 m de longueur, 1 m de largeur et 50 cm d’épaisseur. Dans un premier temps, nous avons réalisé une étude sur la détection de défauts dans cette dalle. Grâce à un algorithme développé pendant cette thèse, un trou de 15 cm de côté peut être détecté avec un niveau de confiance de 98% à partir de 4h de prise de données. Par la suite, nous avons réalisé une étude de faisabilité en deux dimensions, dans le plan de la longueur de la dalle, afin de pouvoir reconstruire la carte de densité de la dalle de béton. Pour ce faire, nous avons dû résoudre ce qu'on appelle le problème inverse : l’estimation des paramètres d’un objet en fonction des données collectées. Ici la densité de la dalle de béton joue le rôle de paramètres à estimer et le flux de muons ayant traversés la dalle et collectés par nos détecteurs celui de données. Après analyses des différentes systématiques du problème, nous pouvons reconstruire la densité d’une dalle de béton, avec une résolution en épaisseur de 125 mm et une résolution en longueur de 437.5 mm, avec une erreur relative maximale de 12%This thesis presents the development of Micromegas gaseous detectors for muon tomography. This technique use cosmic muons, resulting from interactions between cosmic rays and the atmosphere to image objects of large dimensions and opacity such as buildings, concrete slabs, volcanoes or pyramids such as the Khufu's pyramid in Egypt. By studying the attenuation of the muon flux through objects, we can access their internal structure. To image such structures and detect muons passing through them, muon telescopes using Micromegas detectors are used. Many efforts have been developed during this thesis to improve the spatial resolution and gas performance of the latter.One of the main goal of this thesis is to image a concrete slab, which dimensions were 2000 mm x 1000 mm x 500 mm. Firstly, a study on the detection of defects in this slab was carried out. Thanks to an algorithm developed during this thesis, a 15cm wide default can be detected with a 98% confidence level from 4h of data collection. Subsequently, a two-dimensional feasibility study, in the plan of the slab length, was carried out in order to reconstruct the density map of the concrete slab. To do this, we need to solve what is commonly referred to as the inverse problem: estimating the parameters of an object based on the data collected. Here the density of the concrete slab will play the role of parameters to be estimated and the flux of muons that have passed through the slab and collected by our detectors will play the role of data. After analysing the different systematic problem analyses, we can reconstruct the density of a concrete slab, with a thickness resolution of 125mm and a length resolution of 437.5mm, with a maximum relative error of 12%
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吳本韓 and Pun-hon Ng. "Measurement of PeV cosmic rays extensive air showers at mountain altitude." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1993. http://hub.hku.hk/bib/B31233156.
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Ng, Pun-hon. "Measurement of PeV cosmic rays extensive air showers at mountain altitude /." [Hong Kong : University of Hong Kong], 1993. http://sunzi.lib.hku.hk/hkuto/record.jsp?B13781431.
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Norén, Magnus. "Measuring the vertical muon intensity with the ALTO prototype at Linnaeus University." Thesis, Linnéuniversitetet, Institutionen för fysik och elektroteknik (IFE), 2021. http://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-107133.
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ALTO is a project, currently in the research and development phase, with the goal of constructing a Very High Energy (VHE) gamma-ray observatory in the southern hemisphere. It will detect the particle content reaching the ground from the interactions of either VHE gamma rays or cosmic rays in the atmosphere known as extensive air showers. In this thesis, we use an ALTO prototype built at Linneaus University to estimate the vertical muon intensity in Växjö. The atmospheric muons we detect at ground level come from hadronic showers caused by a cosmic ray entering the atmosphere. Such showers are considered background noise in the context of VHE gamma-ray astronomy, and the presence of muons is an important indicator of the nature of the shower, and thus of the primary particle. The measurement is done by isolating events that produce signals in two small scintillation detectors that are part of the ALTO prototype, and are placed almost directly above each other. This gives us a data set that we assume represents muons travelling along a narrow set of trajectories, and by measuring the rate of such events, we estimate the muon intensity. We estimate the corresponding momentum threshold using two different methods; Monte Carlo simulation and calculation of the mean energy loss. The vertical muon intensity found through this method is about 21% higher than commonly accepted values. We discuss some possible explanations for this discrepancy, and conclude that the most likely explanation is that the isolated data set contains a significant number of “false positives”, i.e., events that do not represent a single muon following the desired trajectory.
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Asch, Thomas. "Self-Triggering of Radio Signals from Cosmic Ray Air Showers." [S.l. : s.n.], 2008. http://digbib.ubka.uni-karlsruhe.de/volltexte/1000010076.
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Asch, Thomas. "Self-triggering of radio signals from cosmic ray air showers." Karlsruhe Forschungszentrum Karlsruhe, 2009. http://d-nb.info/994365705/34.
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Tridapalli, Diogo Bernardes. "Estudo do efeito da composição das partículas primárias na distribuição lateral de chuveiros atmosféricos do Observatório Pierre Auger." Universidade de São Paulo, 2012. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-17042012-145717/.
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No estudo dos raios cósmicos de ultra alta energia utilizando detectores de superfície a energia da partícula primária é estimada pela distribuição lateral (LDF - Lateral Distribution Function), que descreve a amplitude do sinal das estações em função da distância ao centro do chuveiro. Entretanto, com exceção da estimativa do centro do chuveiro, não se utiliza a LDF para obter mais nenhuma informação sobre o chuveiro, talvez porque ela não possua uma parametrização que a descreva completamente, especialmente para os chuveiros com energias mais altas. As primeiras interações dos raios cósmicos com a atmosfera são determinantes para o desenvolvimento dos chuveiros atmosféricos extensos. Tais interações dependem, entre outras coisas, da composição química dos raios cósmicos. Diferenças nessas interações podem causar alterações nas flutuações da distribuição lateral. Através de simulações dos chuveiros com diferentes partículas primárias pode ser possível estimar a composição dos raios cósmicos de ultra alta energia, comparando as flutuações das distribuições laterais de eventos reais com as de eventos simulados. Uma das grandezas relevantes para a flutuação da LDF é a incerteza do sinal das estações. O framework de análise do Observatório Pierre Auger aplica uma correção parametrizada empiricamente à incerteza do sinal das estações. Neste trabalho foi apresentada uma justificativa estatística para esta correção, que está relacionada à distribuição do sinal não ser uma Poisson, mas uma composição de processos com diferentes distribuições. Para a realização deste trabalho foi gerada uma biblioteca de chuveiros produzidos por dois simuladores de chuveiros atmosféricos, AIRES e CORSIKA, sendo que o AIRES utilizou o SIBYLL como modelo de interação hadrônica enquanto o CORSIKA utilizou o EPOS. Foram produzidos chuveiros iniciados por prótons e núcleos de ferro com os dois simuladores, e suas distribuições angulares foram consideradas isotrópicas. A distribuição de energia desses eventos segue uma lei de potência e varia entre 1 e 200 EeV. Utilizando a função de Nishimura, Kamata e Greisen (NKG) como parametrização para a LDF se observa resíduos sistematicamente positivos nas estações mais distantes do centro do chuveiro, que também têm o sinal mais próximo do trigger. Uma das hipóteses levantadas em outros trabalhos para esse comportamento é que ele estaria relacionado à influência das estações silenciosas, mas este trabalho mostra que o uso dessas estações tem pouca influência na flutuação da LDF. Na verdade esse efeito é causado porque as parametrizações da LDF no Offline não consideram que os sinais das estações possuem um corte devido o trigger, isto é, que a função de densidade de probabilidade que descreve o sinal real não é a mesma que descreve o sinal que é observado. Neste trabalho é proposta uma correção para as parametrizações da LDF que é implementada no Offline. Como resultado desta correção é observada uma redução significativa dos resíduos que eram sistematicamente positivos e que, após a correção, passam a ser compatíveis com zero. Neste trabalho foram realizadas três análises independentes para comparar os eventos reais com os simulados, das quais duas não dependem diretamente do ajuste da LDF e também não são sensíveis à energia. Elas permitem uma comparação entre os sinais supondo uma relação simples entre eles. No primeiro caso supõe-se que a diferença no sinal é devido à componente muônica do chuveiro e no segundo supõe-se que os dois conjuntos de eventos comparados são bem descritos por funções NKG mas com parâmetros S1000 diferentes. A terceira análise utiliza os resíduos dos ajustes da LDF e permite observar a composição em função da energia da partícula primária. Essa última análise foi realizada utilizando a função NKG com e sem correção do efeito do trigger. As diferentes análises utilizadas para estimar a composição dos raios cósmicos apresentaram resultados consistentes entre si, apesar das limitações encontradas em algumas delas. Todos esses indicadores de composição da partícula primária obtidos pelo detector de superfície são consistentes com os resultados obtidos pelas análises de Xmax do detector de fluorescência, reforçando a tese de que a composição dos raios cósmicos é predominantemente de próton entre 1 e 10 EeV e entre próton e ferro para energias acima de aproximadamente 10 EeV.The energy of ultra high energy cosmic rays can be estimated from the lateral distribution function (LDF) of the shower as measured by surface detectors. The LDF describes the particle density as a function of the distance from the shower center. However, with the exception of the position of the shower center, no other information is extracted from it, may because it does not have a parametrization or an analytic function that describes it completely. The first interactions of cosmic rays with the atmosphere are decisive for the development of the extensive air showers. Such interactions, among other things, depend on the chemical composition of comic rays. Differences in these interactions can cause changes in the fluctuation shape of lateral distribution. Through simulations of showers with different primary particles it may be possible to estimate the composition of ultra high energy cosmic rays comparing the fluctuation shape of the lateral distributions of real events with those from simulated ones. One of the quantities relevant to the fluctuation of the LDF signal is the uncertainty of the stations. The analysis framework of the Pierre Auger Observatory applies a correction to the signal uncertainty of the signal. The parameterization of this correction is obtained empirically. In this work a statistical justification for this correction is proposed and is related to distribution of the signal which is not Poisson, but a composition of processes with different distributions. For this work a library of showers using two simulators of air showers, AIRES and CORSIKA, was produced. The showers simulated with the AIRES used SIBYLL as a hadronic interaction model while COSIKA used EPOS. Showers initiated by protons and iron nuclei with the two simulators were produced, and their angular distribution was considered isotropic. The energy distribution of these events follows a power law and ranges from 1 to 200 EeV. Using the Nishimura, Kamata and Greisen (NKG) function as a parameterization for the LDF, one obtains residues that are systematically positive at stations further from the center of the shower. These stations have a signalclose to the trigger level. One of the hypothesis raised in other works for this behavior is that it is related to the influence of the silent stations, but this work shows that their use has little impact on the fluctuation shape of the LDF. In fact, this effect is caused because the parametrizations of LDF in the Offline ignore that the signals of the stations have a cut due to the trigger, ie, the probability density function that describes the real signal is not the same that describes the observed signal. This work proposes a correction to the parameterizations of the LDF and implements it in the Offline. As a result of this correction, the residues, which were always positive, are significantly reduced and compatible with zero. In this study three independent analysis were performed to compare real and simulated events, two of them not dependent directly of the LDF fit and also not sensitive to the primary particle energy. They allow a comparison between the signals assuming a simple relationship between them. The first case assumes that the difference in signal is due to the muonic component of the shower and the second assumes that the two compared sets of events are well described by NKG functions but with different S1000. The third analysis uses the residues of the LDF fits and is able to observe the composition of as a function of primary particle energy. This last analysis was performed using the NKG function with and without correction of the trigger effect. The different analysis used to estimate the composition of cosmic rays showed results consistent, despite the limitations found in some of them. The primary particle composition obtained from the surface detectors in this work is consistent with the results derived from the elongation rate measured by the fluorescence detectors, supporting the hypotesis that the composition of cosmic rays is predominantly proton becoming heavier for energies above 10 EeV.
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Nehls, Steffen. "Calibrated measurements of the radio emission of cosmic ray air showers." Karlsruhe : Forschungszentrum Karlsruhe, 2008. http://d-nb.info/992107431/34.
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Corani, Claire Leslie. "Small cosmic ray air showers observed by the extended Buckland Park array /." Title page, contents and abstract only, 1986. http://web4.library.adelaide.edu.au/theses/09SM/09smc788.pdf.
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Asch, Thomas [Verfasser]. "Self-triggering of radio signals from cosmic ray air showers / Thomas Asch." Karlsruhe : Forschungszentrum Karlsruhe, 2009. http://d-nb.info/994365705/34.
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Perrett, J. C. "Measurements of scintillation and water-Cerenkov detector densities in extensive air showers produced by 10sup(16) - 5x10sup(19) eV cosmic rays." Thesis, University of Leeds, 1985. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.355950.
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Nehls, Steffen [Verfasser]. "Calibrated measurements of the radio emission of cosmic ray air showers / Steffen Nehls." Karlsruhe : FZKA, 2008. http://d-nb.info/998341746/34.
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Horneffer, Andreas. "Measuring radio emission from cosmic ray air showers with a digital radio telescope." [S.l.] : [s.n.], 2006. http://deposit.ddb.de/cgi-bin/dokserv?idn=980171938.
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Saich, M. R. "The muon content of cosmic ray air showers 10sup(16) - 10sup(17) eV." Thesis, University of Nottingham, 1985. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.356037.
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Ludwig, Marianne [Verfasser], and J. [Akademischer Betreuer] Blümer. "Modelling of radio emission from cosmic ray air showers / Marianne Ludwig. Betreuer: J. Blümer." Karlsruhe : KIT-Bibliothek, 2011. http://d-nb.info/1014279380/34.
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Asch, Thomas [Verfasser], and H. [Akademischer Betreuer] Gemmeke. "Self-Triggering of Radio Signals from Cosmic Ray Air Showers / Thomas Asch. Betreuer: H. Gemmeke." Karlsruhe : KIT-Bibliothek, 2008. http://d-nb.info/1113109246/34.
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Soldin, Dennis [Verfasser]. "Laterally Separated Muons from Cosmic Ray Air Showers Measured with the ICECUBE Neutrino Observatory / Dennis Soldin." Wuppertal : Universitätsbibliothek Wuppertal, 2018. http://d-nb.info/1169068839/34.
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CASTRO, MARY LUCIA DIAZ. "INTRINSIC FLUCTUATIONS OF EXTENSIVE AIR SHOWERS AND THE CHEMICAL COMPOSITION OF ULTRA HIGH ENERGY COSMIC RAYS." PONTIFÍCIA UNIVERSIDADE CATÓLICA DO RIO DE JANEIRO, 2012. http://www.maxwell.vrac.puc-rio.br/Busca_etds.php?strSecao=resultado&nrSeq=19921@1.
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PONTIFÍCIA UNIVERSIDADE CATÓLICA DO RIO DE JANEIROO Observatório Pierre Auger é um detector de raios cósmicos ultra-energéticos (E maior ou igual 1018 eV) com características híbridas, que combinam detectores de superfície e de fluorescência. A determinação da composição química primária destes raios cósmicos é um dos seus principais objetivos. Há indícios de que os primários dos raios cósmicos com E maior que 1018.5 eV tem massa maior, conclusão baseada nos resultados recentes sobre a evolução dos chuveiros atmosféricos extensos (cascatas de partículas formadas quando da colisão do raio cósmico primário no topo da atmosfera com moléculas de N2 ou O2). Encontrar parâmetros, que caracterizam o chuveiro, no processo de sua reconstrução e que forneçam informações associadas a este resultado, são essenciais para validar esta conclusão. Nesta tese estuda-se a evolução como função da energia, de parâmetros que caracterizam os chuveiros, que sejam sensíveis à sua composição primária. Mais especificamente aqueles determinados pelo detector de superfície, pois há uma estatística de chuveiros detectados significativamente maior. Damos especial atenção às flutuações intrínsecas – chuveiro-a-chuveiro – do parâmetro de inclinação (beta) da Função de Distribuição Lateral, que descreve a variação da densidade de partículas ao longo da direção perpendicular ao eixo do chuveiro, como função da distância a esse eixo. Os resultados indicam que a flutuação intrínseca em beta, para eventos inclinados (45-60 graus) com E maior que 1018.5 eV, possui uma tendência de diminuição com a energia até valores em torno de 1019.8 eV. Este resultado é consistente com o encontrado anteriormente em análises de composição química sobre a evolução com a energia da profundidade de máximo (Xmax) dos chuveiros atmosféricos extensosmedida pelos detectores do Auger em modo híbrido, em que em energias acima de 1018.5 eV, observase que os chuveiros tendem a atingir seu máximo numa região mais bem definida da atmosfera, levando, por conseguinte, a flutuações menores no sinal no solo.
The Pierre Auger Observatory is an ultra high energy cosmic ray detector (E more than or equal as 1018 eV) which has hybrid characteristics combining surface and fluorescence detectors. Determining the cosmic rays chemical composition is one of its most important challenges. There are evidences that cosmic ray primaries with energy above 1018.5 eV are heavy and this conclusion is based on recent results on the evolution of extensive air showers (cascades of particles formed by the collision of primary cosmic rays in the top of the atmosphere with nitrogen and oxygen molecules). Therefore, it is mandatory to find additional parameters supporting that conclusion. In this thesis, the evolution with energy of parameters characterizing the shower and with sensitivity to chemical composition are studied. More specifically, parameters determined by the surface detector are analyzed due to the high statistics in this operation mode. Special attention is given to the instrinsic - shower to shower - fluctuations of the slope parameter (beta) of the Lateral Distribution Function which describes the particles density variation in the plane perpendicular to the shower axis as a function of distance to that axis. The results show that the intrinsic fluctuation of Beta, for inclined showers (45-60 degrees) with energy above 1018.5 eV, where the detector resolution is small compared to the total fluctuation, has a trend to decrease with energy up to 1019.6 eV. This result is consistent with recent results on the energy evolution of the depth of shower maxima (Xmax) of extensive air showers, where above 1018.5 eV, the distributions of Xmax show less fluctuations, leading, in turn, to less fluctuations on the ground level.
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Itow, Y. "Verification of hadron interaction models of cosmic rays at 10**17 eV by the LHCf experiment." American Institite of Physics, 2008. http://hdl.handle.net/2237/12228.
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Fuchs, Benjamin Lothar [Verfasser], and J. [Akademischer Betreuer] Blümer. "The lateral distribution of radio signals from cosmic ray air showers / Benjamin Lothar Fuchs. Betreuer: J. Blümer." Karlsruhe : KIT-Bibliothek, 2012. http://d-nb.info/1031709002/34.
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Newton, David William. "Measuring the lateral distribution of extensive air showers to characterise properties of cosmic rays above 1 EeV." Thesis, University of Leeds, 2005. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.423005.
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Kemp, Julian [Verfasser], Thomas Akademischer Betreuer] Hebbeker, and Thomas [Akademischer Betreuer] [Bretz. "Development of a silicon photomultiplier based scintillator detector for cosmic air showers / Julian Kemp ; Thomas Hebbeker, Thomas Bretz." Aachen : Universitätsbibliothek der RWTH Aachen, 2020. http://d-nb.info/1227447434/34.
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Fliescher, Stefan [Verfasser]. "Antenna devices and measurement of radio emission from cosmic ray induced air showers at the Pierre Auger Observatory / Stefan Fliescher." Aachen : Hochschulbibliothek der Rheinisch-Westfälischen Technischen Hochschule Aachen, 2012. http://d-nb.info/1023977079/34.
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Holt, Ewa Marlen [Verfasser], J. [Akademischer Betreuer] Blümer, and A. [Akademischer Betreuer] Etchegoyen. "Combined Detection of Muons and Radio Emission of Cosmic-Ray Air Showers / Ewa Marlen Holt ; Betreuer: J. Blümer , A. Etchegoyen." Karlsruhe : KIT-Bibliothek, 2018. http://d-nb.info/116100873X/34.
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Gate, Florian Sylvain. "Estimation of the composition of cosmic rays using the radio signal." Thesis, Nantes, Ecole des Mines, 2016. http://www.theses.fr/2016EMNA0295/document.
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Plus d'un siècle après leur découverte, les rayons cosmiques continuent d'intriguer les physiciens. Le flux de ces particules d'origine extraterrestre décroît fortement en fonction de leur énergie. Au-delà de 1 PeV(10¹⁵ eV), le flux devient trop faible pour permettre la détection directe sur des échelles de temps raisonnables. Cependant, les cascades de particules secondaires créées après l'interaction des rayons cosmiques avec les constituants de l'atmosphère sont détectables depuis le sol, c'est la détection indirecte. A partir de 100 PeV, le nombre d'observations est trop faible pour estimer de manière précise la masse des rayons cosmiques et ainsi contraindre les modèles de mécanismes d'accélération, de propagation et de type de sources. La détermination de la composition est effectuée à l'Observatoire Pierre Auger par les télescopes de fluorescence via la mesure de la variable Xmax avec un cycle utile de 14%. Xmax est la profondeur d'atmosphère traversée à laquelle le nombre de particules secondaires atteint sa valeur maximale. Cette observable est fortement corrélée à la masse du rayon cosmique qui a initié la gerbe. Un grand nombre d'observations est requis pour effectuer une détermination précise de la masse car les fluctuations statistiques de Xmax sont importantes. La radio détection apparaît alors comme une excellente alternative à la détection par fluorescence, puisque la technique mesurant ce signal a un cycle utile proche de 100%. Cette thèse propose une méthode d'estimation de la masse des rayons cosmiques d'ultra haute énergie basée seulement sur l'étude des signaux radio et leur simulation, afin de reconstruire de manière systématique l’énergie, le cœur et la profondeur Xmax des gerbes détectées par l’expérience AERA sur le site de l'Observatoire Pierre Auger en Argentine. L'influence de la modélisation de l'atmosphère dans le code de simulation SELFAS sur les valeurs reconstruites est étudiée. Notamment la géométrie des couches atmosphériques, la manière de traiter l'indice de réfraction et la densité de l'air ainsi que leurs variations journalières et saisonnièresMore than a century after their discovery, cosmic-raysare still puzzling physicists. The flux of these particlescoming from extraterrestrial sources strongly decreasesas a function of their energy. Above 1 PeV (10¹⁵ eV), theparticle flux becomes too low to allow a direct detectionon a reasonable time scale. However, the cascades ofsecondary particles produced after the interaction ofcosmic-rays with the constituents of the atmosphere aredetectable at the ground level; it is the indirect detection.Above 100 PeV, the number of observations is too lowto accurately estimate the mass of the cosmic rays andthen to constrain the prediction models of accelerationmechanisms, propagation and type of sources. Thedetermination of their composition is achieved at thePierre Auger Observatory using fluorescencetelescopes from the measurement of the Xmaxobservable with a duty cycle of 14%. Xmax, defined asthe atmosphere depth at which the number ofsecondary particles reaches its maximal value, is highlycorrelated to the mass of the cosmic ray that hascreated the air shower. A large number of observationsis required for a precise estimation of the mass as theXmax statistical fluctuations are important. The radiodetection is a perfect alternative to the fluorescencemethod as the duty cycle of a typical radio detector isclose to 100%. This thesis proposes a method toestimate the mass of ultra-high energy cosmic raysusing only the radio signals and their simulation. Thegoal is to systematically reconstruct the Xmax depth ofeach air shower detected by the AERA experimentwithin the site of the Pierre Auger Observatory inArgentina. The influence of the description of theatmosphere on the reconstructed shower parameters, inthe SELFAS code, has been studied. It includes thegeometry of the atmospheric layers, the way to calculatethe air refractive index and density, as well as their dailyand seasonal fluctuations
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Díaz, Damián Abraham Neftali. "A new model and tests of the JEM-EUSO Balloon pathfinders Fresnel optics." Thesis, Luleå tekniska universitet, Rymdteknik, 2016. http://urn.kb.se/resolve?urn=urn:nbn:se:ltu:diva-81149.
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EUSO-Balloon and EUSO-SPB are balloon borne pathfinder projects designed to val- idate the techniques of the JEM-EUSO space observatory. They are nadir pointing UV telescopes that use experimental experimental Fresnel optics to detect the ultravi- olet emission of Extensive Air Showers (EAS) induced by Ultra High Energy Cosmic Rays (UHECR) in the atmosphere. EUSO-Balloon was launched by the balloon di- vision of CNES (the french space agency) from Timmins, Ontario, Canada in 2014. Despite the success of the mission the performance of the optics was lower than what it was originally modeled and led to many doubts regarding the understanding of the optics and fresnel lenses themselves. This thesis explores three parameters proposed to explain the reduction in eciency of the system which were not simulated in the original characterization: the rounded valleys in the Fresnel lens grooves created by the tool peak radii, scratches on the surface of the lenses and the surface roughness of the fresnel lenses. These parameters were simulated and results show that they show a reduction in performance which approximates more the characterization measure- ments but still do not match exactly, leaving room for further analysis. EUSO-SPB1 is the successor of EUSO-Balloon with a launch planned in 2017 from Wanaka, New Zealand. The results of the first phase of the optics characterization campaign is pre- sented in this work. The results indicate that the optics performance is similar to that of EUSO-Balloon and require further understanding.Thesis defended in Toulouse, France as part of the SPACEMASTER programme.
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Junior, Washington Rodrigues de Carvalho. "Detecção de chuveiros atmosféricos iniciados por hádrons massivos." Universidade de São Paulo, 2008. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-13102008-102648/.
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Nesta tese investigamos uma possível componente de partículas previstas por modelos além do modelo padrão da física de partículas, como por exemplo o massive gluino LSP, nos raios cósmicos de altíssimas energias (UHECR). Nosso objetivo é determinar os sinais experimentais em telescópios de fluorescência devidos a hádrons exóticos massivos e neutros, genericamente denominados de UHECRons. Para simular chuveiros iniciados por essa classe de partículas, alteramos o pacote Aires de simulação de chuveiros atmosféricos e o modelo hadrônico Sibyll. Estes chuveiros foram utilizados como entrada em simulações de telescópios de fluorescência por nós desenvolvidas, obtendo-se assim as distribuições dos observáveis desses chuveiros exóticos. A partir da comparação entre as características de chuveiros iniciados uhecrons e prótons, desenvolvemos métodos para a separação de sinais entre esses dois tipos de partículas. Esses métodos podem ser utilizados em uma análise inicial, com o intuito de procurar por sinais de partículas exóticas nos dados reais de observatórios de UHECR.In this thesis we investigate a possible component of particles predicted by models beyond the standard model of particle physics, like the massive gluino LSP, in the ultra high energy cosmic rays (UHECR). Our objective is to determine the experimental signals on fluorescence telescopes due to exotic massive and neutral hadrons, generically called UHECRons. To simulate showers initiated by this class of particle, we altered the shower simulation package Aires and the hadronic model Sibyll. These showers were used as input in our simulations of fluorescence telescopes, thus obtaining the distribuitons of the observables for these exotic showers. By comparing the characteristics of showers initiated by uhecrons and protons, we developed methods to distinguish the signals between these two particles. These methods can be used in an initial analysis in order to look for signals of exotic particles in the real data of UHECR observatories.
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Klepser, Stefan. "Reconstruction of extensive air showers and measurement of the cosmic ray energy spectrum in the range of 1 - 80 PeV at the South Pole." Doctoral thesis, Humboldt-Universität zu Berlin, Mathematisch-Naturwissenschaftliche Fakultät I, 2008. http://dx.doi.org/10.18452/15790.
Full textAbstract:
IceTop ist ein Detektorfeld fuer kosmische Strahlung, das momentan am Suedpol errichtet wird. Es ist Teil des IceCube-Observatoriums und wird nach Fertigstellung eine Flaeche von 1km^2 ueberspannen. Es zielt auf den Nachweis von Teilchenkaskaden ab, die von kosmischer Strahlung mit Energien im PeV-Bereich induziert werden. Die Dissertation beinhaltet die erste Analyse hochenergetischer kosmischer Strahlung mit IceTop. Zunaechst wird hierfuer die Lichtausbeute der Detektortanks untersucht. Dies ermoeglicht die Erstellung einer Erwartungswertverteilung der Schauersignale, und eines entsprechenden Likelihood-Rekonstruktionsalgorithmus. Die damit erreichten Aufloesungen werden untersucht und Effizienzen berechnet. Anschliessend wird das Ansprechverhaltenn von IceTop im Bezug auf die Energie genauer evaluiert. Aus den Ergebnissen werden Faltungsmatrizen fuer unterschiedliche Primaerteilchensorten extrahiert. Darauf basierend werden zwei Entfaltungsalgorithmen vorgestellt, und vier Faltungsmatrizen fuer verschiedene Kompositionsannahmen berechnet. Im August 2007 genommene Daten werden in drei Zenithwinkel-Abschnitte eingeteilt und separat mit den Kompositionsmodellen entfaltet. Die resultierenden Spektren decken einen Energiebereich von 1-80PeV ab. Mit der Forderung isotropen Flusses lassen sich Wahrscheinlichkeiten definieren, die sensitiv sind auf die Konsistenz der Kompositionsannahmen. Diese neue Methode ermoeglicht eine Untersuchung der Komposition ohne Zuhilfenahme weiterer Detektorkomponenten. Die Analyse zeigt eine klare Praeferenz der Modelle gemischter Komposition. Schliesslich wird das Spektrum mit der hoechsten relativen Wahrscheinlichkeit untersucht. Die gemessenen Parameter stimmen innerhalb der systematischen Fehler gut mit denen anderer Experimente ueberein. Die ermittelte Position des sogenannten Knies des Spektrums ist 3,1+-0,3(stat.)+-0,3(sys.)PeV, die Exponenten davor und danach sind -2,71+-0,07(stat.) und -3,110+-0,014(stat.)+-0,08(sys.).IceTop is a square-kilometer scale detector array for highly energetic cosmic radiation. It is a part of the IceCube Observatory that is presently being built at the geographic South Pole. It aims for the detection of huge particle cascades induced by PeV cosmic rays in the atmosphere. This thesis presents the first analysis of highly energetic cosmic ray data taken with IceTop. First, the light response of the IceTop tanks is parametrised as a function of energy and particle type. An expectation function for the distribution of shower signals in the detector plane is developed. Based on that, a likelihood reconstruction algorithm is developed and its resolution and performance is studied. The resulting energy response of the array is investigated to set up response matrices for different primary nuclei and inclinations. Two unfolding algorithms are implemented, and response matrices are modeled for four different composition assumptions. With each assumption, energy spectra are unfolded for three different bins in inclination, using a data sample taken in August 2007. The range of the spectrum is 1-80PeV. Finally, a new analysis method is developed that uses the fact that cosmic rays in the PeV range are expected to be isotropic. It is shown that this requirement can be used for a likelihood estimation that is sensitive to composition without using additional information from other detector components. The analysis shows a clear preference of the mixed composition models over pure proton or iron assumption. The spectrum with the highest likelihood shows good agreement with results from other experiments within the systematic uncertainties. The found position of the so-called knee feature is 3.1+-0.3(stat.)+-0.3(sys.)PeV, the power indices before and after that are -2.71+-0.07(stat.) and -3.110+-0.014(stat.)+-0.08 (sys.).
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Neuser, Jens [Verfasser]. "Cosmic Rays and the Atmospheric Electric Field - Reconstruction and Data Analysis of Radio Emission from Air Showers at the Auger Engineering Radio Array / Jens Neuser." Wuppertal : Universitätsbibliothek Wuppertal, 2016. http://d-nb.info/1093600012/34.
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Müller, Sarah Nicola [Verfasser], and J. [Akademischer Betreuer] Blümer. "Measurement of the Cosmic Ray Composition with Air Showers Detected by the AMIGA Extension at the Pierre Auger Observatory / Sarah Nicola Müller ; Betreuer: J. Blümer." Karlsruhe : KIT-Bibliothek, 2019. http://d-nb.info/1176022679/34.
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