Dissertations / Theses on the topic 'Cosmic ray muon'
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1
Quintero, Eric Antonio. "The cosmic ray muon energy spectum via Čerenkov radiation." Thesis, Massachusetts Institute of Technology, 2010. http://hdl.handle.net/1721.1/61261.
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Thesis (S.B.)--Massachusetts Institute of Technology, Dept. of Physics, 2010.Cataloged from PDF version of thesis.
Includes bibliographical references (p. [55]).
In this thesis, I designed and constructed a basic Cerenkov detector to measure the energy spectrum of cosmic ray muons for use in the graduate experimental physics courses, 8.811/2. The apparatus consists of a light-tight central volume with a phototube to detect the Cerenkov radiation of muons whose speed is higher than the speed of light in the medium with which the volume is filled. The measurement is triggerd by coincidence in scintillating detectors above and below the volume. I constructed a signal chain for measurement, collected data for muon energies with the goal of constructing the muon energy spectrum from different Cerenkov spectra. In the range 20-100 GeV, the spectrum is found to obey a power law with exponent -a = -2.90 t .04, which compares well to the value of -2.844 found in the literature. In addition, calculations and considerations were made to aid in the use of this apparatus in a pedagogical manner.
by Eric Antonio Quintero.
S.B.
2
Bullock, A. D. "The determination of the muon content of EAS from CygnusX-3." Thesis, University of Nottingham, 1988. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.384303.
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Kwok, Talent, and 郭天能. "Cosmic-ray muon in the Aberdeen Tunnel laboratory in Hong Kong." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2011. http://hub.hku.hk/bib/B45961372.
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Yifan, Zheng. "Research on a material discrimination method by cosmic ray muon tomography." Thesis, KTH, Fysik, 2018. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-231331.
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Camp, David L. "Using a two-scintillator paddle telescope for cosmic ray flux measurements." Digital Archive @ GSU, 2012. http://digitalarchive.gsu.edu/phy_astr_theses/17.
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A two-scintillator paddle muon telescope with variable angular acceptance at the earth's surface was used to study correlations between flux distribution and barometric pressure. The detector was placed in 2 different locations around Georgia State University with varying paddle separations of 0, 7, and 14 inches. Correlation and anti-correlation analyses were conducted by using the muon count from the detector along with the barometric pressure, surface temperature, stratospheric temperature and solar activity. It was observed that there was a short and long-term variation relationship between cosmic ray counts and barometric pressure and also cosmic ray counts and temperature. No significant relationship was found between cosmic ray flux and solar activity. A new two-scintillator paddle telescope with larger detecting area was constructed in order to observe a stronger correlation between cosmic ray flux and pressure.
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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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Ngai, Ho-yin, and 倪浩然. "Measurement of cosmic-ray muon induced neutrons in the Aberdeen Tunnelunderground laboratory in Hong Kong." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2012. http://hub.hku.hk/bib/B47249250.
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The Daya Bay reactor neutrino experiment aims to determine sin2 2θ13
with a sensitivity of 0.01 or better at 90% confidence level. One of the major
backgrounds to neutrino measurements is the muon-induced neutrons. An ex-
periment had been set up inside the Aberdeen Tunnel laboratory, Hong Kong,
to study spallation neutrons induced by cosmic-ray muons in an underground
environment similar to the Daya Bay experiment.
The Aberdeen Tunnel laboratory is 22 m above sea level at 22:23?N and
114:6?E. The amount of overburden is approximately 235 m of rocks, which
is equivalent to 611 m.w.e. Rock compositions in the Aberdeen Tunnel area
is similar to that in Daya Bay. MUSIC simulation results showed that in the
laboratory the mean energy of muons 〈Eμ〉= 122 GeV and the integrated muon
intensity I = 9:64 X10??6 cm??2 s??1.
A Bonner Spheres Neutron Spectrometer (BSS) was developed to measure
the ambient neutron energy spectrum. The BSS consists of a thermal neutron
detector and a set of eight polyethylene spherical shells. The overall detection efficiency of the BSS was (96:7 +3:3
??13:1)% with a detector background rate of
(1:96_0:03)_10??3 s??1. The total neutron fluence rate measured at the Surface
Assembly Building (SAB) of the Daya Bay experiment was (5:20 +0:81
??0:44) _ 10??3
cm??2 s??1, which agreed with the neutron fluence rate measured in the air/ground
interface in Taiwan. The unfolded SAB neutron energy spectrum showed a clear
thermal-neutron peak around 20 meV and a cascade peak around 100 MeV. Detectable number of neutrons could be seen at 1 GeV. The neutron fluence rate
measured at the Aberdeen Tunnel (ABT) laboratory was significantly higher
then some other underground laboratories. The unfolded ABT neutron energy
spectrum showed a pronounced evaporation peak around 1 MeV, and a sup-
pression in the cascade peak.
Detections of muon-induced neutrons inside the Aberdeen Tunnel laboratory
is achieved by a Muon Tracker and a Neutron Detector. The Muon Tracker
consists of three main layers of crossed plastic scintillator hodoscopes capable
of determining the incoming direction of muons. The average efficiency for most
of the hodoscopes was above 95%. The Neutron Detector consists of about 760
L of gadolinium-doped liquid scintillator and sixteen photomultiplier tubes. The
liquid scintillator target is shield by about 1900 L of mineral oil from external
radiations. The overall average detection efficiency of muon-induced neutrons
was about 16%.
The measurement of muon-induced neutrons in the Aberdeen Tunnel lab-
oratory started from June 2011, with a total live time of about 30 days. The
average rate of the accepted muon events was 0.013 Hz. The muon-induced
neutron yield was determined to be Nn = (8:5 _ 0:4(syst.) _ 1:8(stat.)) _
10??5 neutron/(μg cm??2). This value agreed with the parametrization of
FLUKA-1999 simulation results if the muon energy dependence of muon-induced
neutron yields was considered.published_or_final_version
Physics
Doctoral
Doctor of Philosophy
8
Cui, Kexi, and 崔科晰. "Analysis of cosmic-ray-muon induced spallation neutrons in Aberdeen Tunnel experiment in Hong Kong." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2014. http://hdl.handle.net/10722/197506.
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The muon-induced radioactive isotopes, especially neutrons, are dangerous background component for rare-event detection in underground experiments, like neutrino-less double-beta decay and dark matter search. Understanding these cosmogenic backgrounds is crucial for these experiments. An underground experiment aiming at measuring the cosmic-ray muons' flux and their neutron production yield in liquid scintillator through spallation process is being carried out in the Aberdeen Tunnel laboratory located in Hong Kong with a total vertical overburden of 235 m of rocks (611 m.w.e.).
The Aberdeen Tunnel detection system is constituted of a Muon Tracker (MT) for muon tagging and a Neutron Detector (ND) for neutron detection. The MT consists of 60 plastic scintillator hodoscopes to determine the incoming muon direction and the ND is a two-zone detector containing 760 L of gadolinium-doped liquid scintillator as target volume and 1900 L of mineral oil as shields. The experiment has been taking data stably since 2012. To obtain reliable results, the detector performance and the stability of the experiment have been studied in this work. Muon-induced fast neutrons can be captured in Gd-LS with characteristic energies released and the capture time follows a characteristic exponential distribution. By using the capture time and energy information, we can select the neutron candidates and thus calculate the neutron production yield. The energy of a neutron capture event is reconstructed from the calibrated photo-multiplier tube signals, while the directions of cosmic-ray muons can be reconstructed from the MT.
The mean energy of the incoming muons that pass the selection criteria was estimated by a simulation code MUSIC that transported atmospheric muon spectrum through the mountains to the laboratory, and is found to be 92 GeV. The neutron production yield is calculated to be Yn = (3:28 ±0:12(sta:) ±0:24(sys:)) X 〖10〗^(-4) (n/μ〖gcm〗^(-2)) for both the showering muon and single muon events. This result is about two times higher than the expectation value from previous simulations and experiments. The neutron production yield of the single muons is calculated to be Yn = (1:04 ± 0:08(sta:) ± 0:07(sys:)) X 〖10〗^(-4) (n/μ〖gcm〗^(-2)). This reveals a enhancement of the neutron production from the muons accompanied by showers.published_or_final_version
Physics
Master
Master of Philosophy
9
Edwards, Peter J. "A study of the muon content of EAS initiated by the UHE gamma-ray emission from Cygnus X-3." Thesis, University of Nottingham, 1990. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.238238.
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Nutbeam-Tuffs, Sian Louise. "A prototype scintillating fibre tracker for the cosmic-ray muon tomography of legacy nuclear waste containers." Thesis, University of Glasgow, 2014. http://theses.gla.ac.uk/5870/.
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Tomographic imaging techniques using the Coulomb scattering of cosmic-ray muons are increasingly being exploited for the non-destructive assay of shielded containers in a wide range of applications. One such application is the characterisation of legacy nuclear waste materials stored within industrial containers. The design, assembly and performance of a prototype muon tomography system developed for this purpose are detailed in this thesis. This muon tracker consists of two tracking modules above and below the volume to be assayed. Each module comprises two orthogonal planes of 2mm fibres. The modular configuration allows the reconstruction of the initial and scattered muon trajectories which enable the container content, with respect to atomic number Z, to be determined. Fibre signals are read out by Hamamatsu H8500 MAPMTs with two fibres coupled to each pixel via dedicated pairing schemes developed to avoid space point ambiguities and retain the high spatial resolution of the fibres. The design, component tests and assembly of the detector system are detailed and presented alongside results from commissioning and performance studies with data collected after construction. These results reveal high stability during extended collection periods with detection efficiencies in the region of 80% per layer. Minor misalignments of millimetre order have been identified and corrected in software. A GEANT4 simulation was created and used for testing image reconstruction algorithms and for comparison to experimental scenario. A likelihood-based image reconstruction algorithm was developed and is described with reconstructed image results from simulated and experimental data for various scenarios are presented. These results verify the simulation and show discrimination between the low, medium and high-Z materials imaged and highlight the high spatial resolution provided by the detector system.
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Damauskaitė, Jovita. "Research And Application Of Hard Cosmic Ray Flux For Forecasting Meteorological Conditions." Doctoral thesis, Lithuanian Academic Libraries Network (LABT), 2010. http://vddb.laba.lt/obj/LT-eLABa-0001:E.02~2010~D_20101222_130615-72153.
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The thesis investigates cosmic rays and their scattering in the atmosphere and the change in their intensity caused by the frequency of meteorological phenomenon. The main objective of the research is the change in cosmic rays as well as atmospheric pressure and estimation of their connection. A thorough analysis and interpretation allow to supplement meteorological information for weather forecasts.Disertacijoje nagrinėjama kosminė spinduliuotė ir jos sklaida atmosferoje bei jos intensyvumo kaita, kurią lemią meteorologinių reiškinių dažnumas. Pagrindinis tyrimo objektas yra kietosios kosminės spinduliuotės ir atmosferos slėgio pokyčiai bei jų sąryšio įvertinimas. Kosminės spinduliuotės duomenų detali analizė ir interpretacija leidžia papildyti meteorologinę informaciją orų prognozei.
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Lázaro, Roche Ignacio. "Design, réalisation et test in situ d’une caméra muon pour des applications en sciences de la terre et en génie civil." Thesis, Université Côte d'Azur (ComUE), 2018. http://www.theses.fr/2018AZUR4074/document.
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Cette thèse est dédiée à la création d'un nouvel outil pour la mesure directionnelle du flux muonique basé sur une chambre de projection temporelle fine avec un plan de lecture Micromegas, afin d’obtenir un détecteur compact avec une résolution angulaire compatible avec les applications d’imagerie ou de monitoring en génie civil et géophysique. La principale motivation est de développer un détecteur capable de combler le vide technologique pour les applications ayant des contraintes d’encombrement et de transportabilité. Cette thèse fournit une revue des différentes technologies de détection de muons existantes et de leurs divers domaines d’application. Deux techniques de mesure de muons sont présentées : la muographie par transmission ou par diffusion. La muographie par transmission, mieux adaptée aux grandes cibles, est basée sur l'atténuation du flux naturel de muons cosmiques due à l'opacité des matériaux traversés. Cette technique passive et non-destructive fournit des informations originales qui pourront être intégrées dans une démarche d’imagerie. Le manuscrit présente la méthodologie utilisée pour la caractérisation du flux incident de muons à la fois en surface et dans des conditions souterraines. Une description détaillée des processus physiques déclenchés par le passage d'un muon à travers le détecteur est fournie. Les résultats des simulations des processus de formation du signal sont présentés et commentés pour justifier les choix du design des composants clés afin de répondre aux exigences de performance quant à résolutions temporelle, spatiale et angulaire. L'influence des paramètres opérationnels ou externes tels que le gain, la température ou la présence de contaminants est également traitée. La thèse étudie en détail les principales phases de conception et d'assemblage du détecteur MUST2, incluant (i) le design du plan de lecture Micromegas, (ii) le choix du gaz, (iii) le design d'un élément homogénéisateur de champ électrique (iv) le choix de l'instrumentation électronique et du signal de déclenchement associé au passage du muon, et (v) la création d'un système auxiliaire de gestion du gaz. La polyvalence du détecteur MUST2 a été prouvée avec l'utilisation réussie de différentes options de déclenchement et d’acquisition. Les données sont obtenues au travers d’un logiciel développé pour le système d’acquisition modulaire du CERN SRS, puis analysées avec un algorithme de reconstruction de la trajectoire, qui récupère le temps de passage, la position 2D, les angles zénith et azimut des muons qui traversent le détecteur. Les caractéristiques, les performances et les limites de la chaîne d'acquisition de données sont présentées et évaluées. Une série de directives visant à améliorer l’efficacité de la chaîne d'acquisition est proposée. Une série de tests de caractérisation a été effectuée dans différents environnements : faisceau contrôlé de muons, ciel ouvert, au fond d'une vallée et dans des conditions souterraines. Ces tests ont contribué à une meilleure compréhension des performances du détecteur et ont permis de régler ses paramètres opérationnels. Malgré les faibles statistiques des tests, les flux mesurés montrent une bonne corrélation avec les environnements ciblés. Une campagne de mesures en conditions réelles a été menée sur le barrage de Saint-Saturnin-les-Apt (Vaucluse). Les résultats expérimentaux obtenus, sont conformes aux valeurs anticipées par le modèle numérique, la transportabilité sur le terrain et la capacité à effectuer des mesures hors laboratoire à long terme ont été démontrées. En revanche, l’impact de la température externe sur l’acquisition des données devra être compensée pour obtenir une acquisition stable permettant de surveiller l’évolution temporelle du flux de muons. En conclusion, les bons résultats obtenus lors de ces tests permettent de valider la caméra MUST2 à des fins de muographie en transmissionThis thesis is dedicated towards the creation of a new direction-sensitive tool for muon flux measurement based on a thin time projection chamber with a Micromegas readout, to achieve a compact detector with an angular resolution compatible with civil engineering and geophysics imagery and monitoring applications. The main motivation is to develop a detector capable to fill the technological gap for applications with compactness and transportability constraints. The dissertation provides a review of the different existing muon detection technologies and their diverse fields of application. Two muon imaging techniques are introduced: transmission and scattering muography. Transmission muography, more suitable for big targets, is based on the attenuation of the natural-occurring cosmic-muon flux due to the opacity of the material they traverse. This non-destructive, passive technique provides original information that can be used for imaging purposes. The work covers the methodology used towards the characterization of the incidental muon flux both on the surface and in underground conditions. A detailed description of the physical processes triggered by the passage of a muon through the detector is provided. Results of the simulations of the signal formation processes are presented and discussed to justify the design choices of the key components so as to meet performance requirements in term of temporal, spatial and angular resolution. The influence of operational or external parameters such as the gain, temperature or presence of contaminants is covered as well. The thesis describes in detail the principal phases of design and assembly of the MUST2 detector, including: (i) the design of the Micromegas readout layout, (ii) the choice of gas, (iii) the conception of an electric field homogenizer, (iv) the choice of the electronics instrumentation and its trigger signal, and (v) the creation of an auxiliary system to manage the gas. The versatility of MUST2 has been proved with the successful use of different trigger options and electronics. The data is acquired by means of software developed for the CERN’s Scalable Readout System electronics and subsequently analyzed with a muon trajectory reconstruction algorithm, which retrieves the: time of passage, 2D position, zenith and azimuth angles of the muons traversing the detector. The characteristics, performance and limitations of the data acquisition chain are presented and evaluated, a series of guidelines towards the improvement of its efficiency of are provided. A series of characterization tests has been carried out in different environments: controlled muon beam, open sky, at the bottom of a valley and in underground conditions. These tests have enabled a better understanding of the performance of the detector and allowed to tune up its operational parameters. Despite the weak statistics of the test runs, the measured muon flux has shown a good correlation with the surrounding target volumes. A campaign of measurements in real field conditions has been carried out at the Saint-Saturnin-les-Apt (Vaucluse, France) dam. The experimental results obtained are in consonance with the values anticipated by the digital model, the field transportability and the capability to perform long-term out-of-lab measurements have been demonstrated. On the downside, the impact of the external temperature on the data acquisition should be balanced out to get a steady acquisition and monitor the temporal evolution of the muon flux. In conclusion, the successful proof-of-concept trial allows to validate the MUST2 camera for transmission muography purposes
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Tisserant, Sylvain. "Etude des groupes de muons souterrains observes dans l'experience du frejus (4800 metres d'equivalent-eau) : un moyen d'etude de la composition des rayons cosmiques primaires au-dela de 1000 tev." Paris 7, 1987. http://www.theses.fr/1987PA077167.
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Analyse d'environ 6250 groupes de muons enregistres par le detecteur du frejus situe a une profondeur equivalente a 4800 m d'eau. La comparaison de la distribution de la multiplicite observee avec une loi de puissance a permis de constater une deviation au-dela de m=11. Etude de la distribution laterale des muons. En supposant une dependance exponentielle par rapport a la distance a l'axe de la gerbe, on analyse l'evolution de la distance caracteristique par rapport a la multiplicite vraie n a la profondeur du laboratoire. L'interpretation des resultats en termes de composition chimique du rayonnement cosmique primaire dans la region du pev est en faveur d'une composition relativement legere: loga=0,8
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Coenders, Stefan Verfasser], Elisa [Akademischer Betreuer] [Gutachter] Resconi, Jochen [Gutachter] [Greiner, and Miguel [Gutachter] Mostafa. "High-energy cosmic ray accelerators: searches with IceCube neutrinos : Probing seven years of IceCube muon data for time-integrated emission of point-like neutrino sources / Stefan Coenders ; Gutachter: Jochen Greiner, Elisa Resconi, Miguel Mostafa ; Betreuer: Elisa Resconi." München : Universitätsbibliothek der TU München, 2016. http://d-nb.info/1120013941/34.
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Hembrow, K. P. "Observations of the muon component of PeV EAS." Thesis, University of Nottingham, 1990. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.277628.
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Kirby-Gallagher, Lucy Mary. "A study of underground muons in the Soudan II Detector." Thesis, University of Oxford, 1990. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.276567.
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Lee, Ka-pik. "Studies of gadolinium-loaded liquid scintillator used in the Aberdeen tunnel experiment in Hong Kong." Click to view the E-thesis via HKUTO, 2008. http://sunzi.lib.hku.hk/hkuto/record/B41508658.
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Kwok, Talent. "A study of background radiation and cosmic muon detection at the Aberdeen Tunnel laboratory in Hong Kong." Click to view the E-thesis via HKUTO, 2007. http://sunzi.lib.hku.hk/hkuto/record/B38819971.
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Kwok, Talent, and 郭天能. "A study of background radiation and cosmic muon detection at the Aberdeen Tunnel laboratory in Hong Kong." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2007. http://hub.hku.hk/bib/B38819971.
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Thomson, Mark Andrew. "An experimental study of the possible association of deep underground muons with astronomical point sources." Thesis, University of Oxford, 1991. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.303607.
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Tummey, Steven Peter. "A search for diffuse and point source emission of UHE gamma rays using muon content selected EAS." Thesis, University of Nottingham, 1993. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.336196.
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Barley, Steven Keith. "Investigation of the muon component of EAS initiated by primary radiation from Hercules X-1." Thesis, University of Nottingham, 1990. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.238221.
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Lee, Ka-pik, and 李嘉碧. "Studies of gadolinium-loaded liquid scintillator used in the Aberdeen tunnel experiment in Hong Kong." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2008. http://hub.hku.hk/bib/B41508658.
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Tcaciuc, Rodica. "Lateral distribution of cosmic ray muons underground results from the CosmoALEPH experiment /." [S.l.] : [s.n.], 2006. http://deposit.ddb.de/cgi-bin/dokserv?idn=982729480.
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Giller, Graham L. "The construction and analysis of a whole-sky map using underground muons." Thesis, University of Oxford, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.386589.
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Räihä, T. (Tomi). "Analysis tools for the EMMA experiment." Doctoral thesis, University of Oulu, 2012. http://urn.fi/urn:isbn:9789514299469.
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Abstract
Cosmic rays are energetic particles traversing space that bombard Earth's atmosphere frequently and produce vast particle showers while interacting with air nuclei. The origin and composition of high-energy cosmic rays in the knee region (1015 - 1016 eV) of the cosmic-ray energy spectrum remain unclear despite of novel detection and analysis methods used in various surface and underground experiments. The understanding of the knee has improved from its first detection but still there is notable deviation in results between experiments depending on the used detection methods.
The aim of the underground cosmic-ray experiment EMMA (Experiment with Multi-Muon Array) is to shed more light on the origin of the knee. EMMA is based on the idea to measure the lateral shape of high-energy muon component produced in cosmic-ray initiated particle showers on an event-by-event basis, that is, separately for each shower, offering a unique way to study the composition of cosmic rays in the knee region.
The present work comprises the design, development and implementation of a comprehensive set of analysis tools for the EMMA experiment. It includes the development of the simulation program to generate realistic event data, the track reconstruction program ETANA to reconstruct hits and tracks in detector stations, the visualisation program EmmaEve to scan events, the graphical monitoring program EmmaDiagnosticsGUI to control the functionality of detectors on-line, the efficiency monitoring program to control chamber efficiencies in three-layer stations and the design of the EMMA database to store reconstruction results. Especially the design and tests of ETANA form the backbone of the present work as its optimised performance is crucial for the analysis of EMMA data.
Furthermore, in the present work the influence of rock overburden above EMMA on the properties of high-energy muons is investigated by detailed simulations. The reconstruction of hits in drift chambers is studied with measured data including the estimation of the quality of reconstructed hits, the functionality of hit formation procedure and the influence of afterpulses on hit reconstruction. The validity of simulated data that are generated by the EMMA event generation program is evaluated by comparing simulated and measured data with each other. Finally, synergy benefits between the EMMA and ALICE experiments are discussed, which are both underground experiments but different in nature.
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Hashim, Nadir Omar. "Measurement of the momentum spectrum of cosmic ray muons at a depth of 320 mwe." [S.l.] : [s.n.], 2007. http://deposit.ddb.de/cgi-bin/dokserv?idn=985020326.
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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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Sousa, Guilherme Tomishiyo Teixeira de. "Thinning effects in the simulation of muon production profiles." Universidade de São Paulo, 2017. http://www.teses.usp.br/teses/disponiveis/76/76131/tde-22032017-160056/.
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Extensive air showers’ (EAS) observables sensible to primary cosmic ray mass are a valuable asset in constraining competing astrophysical and particle physics scenarios proposed both to explaining cosmic rays features, such as their all-particle spectra, as well as their origin. These observables, however, need to be interpreted by comparison to EAS simulations, which are a source of great uncertainty. Shower simulations need to rely on a technique called thinning, an algorithm created to reduce computing time and storage requirement. In this work, we evaluate the effects of thinning over the muon production profile of an EAS simulation. For heavier particles it appears that thinned showers generate profiles with a deeper maximum, while results were not conclusive for protons and photon primaries. We investigate the thinning technique by constructing a toy model for shower simulations in which we have full control of the thinning implementation. To that end, we parameterized the energy distribution and particle production multiplicity from proton-air interactions and proton-pion interactions. However, we find that thinning effects over our model were too severe, rendering it impossible to draw further conclusions about its effects on full air showers simulations.Observáveis sensíveis à composição de raios cósmicos primários em chuveiros atmosféricos extensos são um recurso valioso na constrição de cenários competidores em astrofísica e física de partículas, propostos tanto para explicar características dos raios cósmicos, como o espectro de energia de todas as partículas, quanto sua origem. Estes observáveis, no entanto, precisam ser interpretados por comparação a simulações de chuveiros atmosféricos, que constituem fonte de grandes incertezas. Simulações de chuveiros são dependentes de uma técnica chamada thinning, um algoritmo criado para reduzir o tempo de computação e exigências de armazenamento. Neste trabalho, nós avaliamos os efeitos do thinning sobre o perfil de produção de múons em uma simulação de chuveiro atmosférico. Para partículas mais pesadas, aparentemente, chuveiros sujeitos ao thinning geram perfis com máximos mais profundos, e para prótons e fótons nossas análises foram inconclusivas. Nós investigamos a técnica do thinning construindo um simulador de chuveiros simplificado, em que o total controle sobre a implementação do thinning é garantido. Para este fim, parametrizamos a distribuição de energia e a multiplicidade de partículas em interações de próton com o ar e de píons com o ar. Entretanto, descobrimos que o efeito do thinning sobre o nosso modelo era muito severo, tornando impossível concluir seus efeitos sobre simulações completas.
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Hashim, Nadir O. [Verfasser]. "Measurement of the Momentum Spectrum of Cosmic Ray Muons at a Depth of 320 mwe / Nadir O Hashim." Aachen : Shaker, 2007. http://d-nb.info/116651272X/34.
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Smith, Mark A. "A detector to measure 9Li production rate in liquid scintillator at the earth’s surface by cosmic ray muons." Diss., Kansas State University, 2009. http://hdl.handle.net/2097/1542.
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Doctor of PhilosophyDepartment of Physics
Glenn A. Horton-Smith
The next generation of nuclear fission reactor based neutrino experiments seeking to measure the Theta-13 mixing angle rely upon measurements made by detectors placed close to the reactor, and therefore less shielded from cosmic ray muons by the earth. 9Li production in liquid scintillator by these cosmic ray muons becomes a serious problem for these experiments that must be dealt with since the 9Li production rate is still a significant fraction of the neutrino interaction rate. This 9Li background reduces the experiment’s sensitivity to measure the Theta-13 mixing angle. This thesis discusses a small detector designed to measure the 9Li production rate in liquid scintillator at the earth’s surface by cosmic ray muons. The detector was designed, built, and finally, calibrated. The ability to find the signals necessary to actually measure the 9Li production rate is shown, establishing that this detector will be able to measure the production rate. A 90% significance level upper limit for the 9Li-like production rate, based on only 3.5 days worth of data, is reported as 213 9Li-like events per day per ton.
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Smith, Mark A. "A detector to measure ⁹Li production rate in liquid scintillator at the earth's surface by cosmic ray muons." Manhattan, Kan. : Kansas State University, 2009. http://hdl.handle.net/2097/1542.
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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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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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Costa, Kelen Cristiane Noleto da. "Simulação da razão de carga de múons atmosféricos na escala TeV." Universidade Federal de Goiás, 2011. http://repositorio.bc.ufg.br/tede/handle/tde/2902.
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Conselho Nacional de Pesquisa e Desenvolvimento Científico e Tecnológico - CNPq
Coordenação de Aperfeiçoamento de Pessoal de Nível Superior - CAPES
Several analysis can be performed using atmospheric muons produced in chain reactions caused by a cosmic ray particle. We can study the muon flux for different parameterizations of the atmosphere, the moon and sun shadowing effect, the muon charge ratio, etc. In this work, we are interested in the atmospheric muon charge ratio (rμ = Nμ+/Nμ−). This ratio has been observed by several experiments, for different energy ranges. The MINOS experiment has determined the muon charge ratio (rμ) in the GeV energy scale using the Near Detector and in the TeV energy scale using the Far Detector. This experiment has observed an increase of the muon charge ratio from 1.27 to 1.37 when the energy of the primary particle changed from ∼ 100 GeV to ∼ 1 TeV. This fact can be explained by the properties of the pions ( ) and the kaons (K). For higher energies, around 10 TeV, the decay of charming hadrons becomes important as a source of atmospheric leptons. Investigating the parameterization given by the Gaisser equation in order to study the intensity of positive and negative muons separately, it is possible to obtain the equation of the pion-kaon ( K) model. Using this model it was made an adjust with the of MINOS Near and Far Detector data, finding the f and fK parameters. These parameters are the fractions that contribute to the production of positive muons coming from de e K, respectively. The experimental values obtained were: f = 0.55 and fK = 0.70. In this work we simulated extensive air showers using the CORSIKA code. Different models that describe the hadronic interactions for high energy particles were used. Our goal was to verify if the models could reproduce the increase of muon charge ratio. This increase is associated with physics involving pion and kaon decays. We found the following parameters: f = 0.547 ± 0.003 and fK = 0.64 ± 0.02 for the QGSJET 01C model, f = 0.604 ± 0.003 and fK = 0.73 ± 0.02 for the SIBYLL model, f = 0.572 ± 0.003 and fK = 0.70 ± 0.02 for the VENUS model, f = 0.545 ± 0.004 and fK = 0.62 ± 0.03 for the QGSJETII model and f = 0.570 ± 0.003 and fK = 0.65 ± 0.02 for the DPMJET model. The increase of the muon charge ratio found in the MINOS data was 7.8%. In our simulation we found an increase of 3.2%, 8.3%, 5.7%, %4.0 and 2.5% for each one of the models, respectively. With these results, it was possible to observe that simulation models also show a significant increase of ratio, when we moved from scale GeV scale for TeV. And of course, this increase is characterized by properties of pions and kaons noting that physics is considered by the codes of models.
Várias análises podem ser feitas a partir de múons atmosféricos produzidos na reação em cadeia provocada por uma partícula de raio cósmico, como o estudo do fluxo de múons para diferentes parametrizações da atmosfera, da sombra da lua e do sol, da razão da carga entre múons atmosféricos. Neste trabalho estamos interessados na razão da carga entre múons atmosféricos (rμ = Nμ+/Nμ−). Essa razão foi determinada por diversos experimentos, para diferentes intervalos de energias. Especificamente, o experimento MINOS determinou a razão (rμ) na escala GeV com o Near Detector e na escala TeV com o Far Detector. Esse experimento observou um aumento da razão de 1,27 para 1,37 com o aumento da energia de ∼100 GeV para ∼ 1 TeV. O aumento dessa razão pode ser entendido a partir das propriedades dos píons ( ) e káons (K). Para energias maiores, cerca de 10 TeV, o decaimento de hádrons charmosos torna-se importante como fonte de léptons atmosféricos. Investigando a parametrização dada pela equação de Gaisser para estudar separadamente a intensidade dos múons positivos e negativos, é possível chegar na equação do modelo píon-káon ( K). Utilizando este modelo, foi feito um ajuste com os dados do MINOS Near e Far Detector, encontrando os parâmetros f e fK. Esses parâmetros são as frações que contribuem para a produção de múons positivos vindos de e K, respectivamente. Os valores experimentais encontrados foram: f = 0,55 e fK = 0,70. Neste trabalho simulamos chuveiros atmosféricos com o código CORSIKA. Diferentes modelos de interações hadrônicas de altas energias foram utilizados. O objetivo foi verificar se os modelos conseguiriam reproduzir o aumento da razão da carga de múons entre GeV e TeV. Esse aumento está associado à física envolvida no decaimento dos píons e káons. Encontramos os seguintes parâmetros: f = 0,550 ± 0,006 e fK = 0,61±0,03 para o modelo QGSJET 01C, f = 0,611±0,004 e fK = 0,67±0,02 para o modelo SIBYLL, f = 0,571 ± 0,005 e fK = 0,70 ± 0,03 para o modelo VENUS, f = 0,547±0,006 e fK = 0,61±0,04 para o modelo QGSJETII e para o modelo DPMJET, f = 0,574±0,004 e fK = 0,63±0,02. O aumento da razão para os dados do experimento MINOS foi de 7,8%; para a nossa simulação o aumento foi de 3,2%; 8,3%; 5,7%; 2,4% e 2,9%; respectivamente. Com esses resultados, foi possível observar que os modelos de simulação também evidenciam um aumento significativo da razão, quando passamos da escala GeV para escala TeV. Esse aumento é caracterizado pelas propriedades dos píons e káons, constatando que essa física é considerada pelos códigos dos modelos.
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Sarkamo, J. (Juho). "Design, construction and commissioning of the EMMA experiment." Doctoral thesis, University of Oulu, 2014. http://urn.fi/urn:isbn:9789526205694.
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Abstract
The work describes the design, construction and commissioning of the underground cosmic-ray experiment Experiment with MultiMuon Array (EMMA). The experiment is built into the Pyhäsalmi mine, in the town of Pyhäjärvi, Finland. The aim of EMMA is to determine the elemental composition of cosmic rays at an energy region around 4 PeV, the energy region called the ’knee’ region. This is achieved by measuring the lateral density distribution of high-energy muons originating from Extensive Air Showers (EAS).
The design calculations for the EMMA experiment, which are based on the use of the parametrization of the lateral density distribution of muons, the method of shower reconstruction, and the energy and composition indicators, are presented. A strategy for reconstructing the composition of the cosmic rays is presented and it demonstrates the potential of applying unfolding techniques to the EMMA data. The effect of an array extension on the performance of EMMA is studied.
The hardware used in the EMMA experiment is presented starting with an overview of the array and its detector stations. The EMMA array employs three different particle detectors, for which the main technical properties are given, and their use in the EMMA array is presented. A description of the infrastructure of the experiment is given and the rock overburden at the EMMA site at the depth of 80 metres is documented.
The work contains the latest analysis of EAS data recorded by the tracking detectors of the experiment, which demonstrates that the experiment is taking data as planned and that the data are according to EAS physics expectations. Methods for event selection and tracking efficiency correction are presented, after which the analysis results of measured track multiplicity spectra are given. The shape of the recorded multiplicity spectrum indicates that the simplest model of a knee-like spectrum with a pure proton composition can not explain the data and that further analysis of the spectrum is required.
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Nunes, Mônica Soares 1987. "Medidas de intensidade de múons cósmicos com cintiladores plásticos." [s.n.], 2015. http://repositorio.unicamp.br/jspui/handle/REPOSIP/276950.
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Orientador: Ernesto KempDissertação (mestrado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin
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Resumo: O estudo da radiação cósmica é de extrema importância para a astrofísica. Partículas oriundas de diferentes locais, tanto do sistema solar, quanto fora dele, chegam constantemente à Terra, carregando muitas informações a respeito da sua origem. Quando essas partículas encontram a atmosfera terrestre da-se início a uma cascata de partículas secundárias resultantes da interação do raio cósmico primário com a atmosfera. Dessa chuva de partículas secundárias, os múons são as partículas carregadas mais abundantes que chegam à superfície da Terra. Múons são altamente penetrantes, o que pode representar um problema muito grande em ex- perimentos, mesmo que subterrâneos, de outras partículas. Devido ao seu grande número, eles se tornam extremamente necessários em reconstruções de chuveiros atmosféricos para obtenção de informações a respeito da partícula primária. Tendo conhecimento de suas características, como por exemplo fluxo, ruídos em experimentos podem ser tratados e outros estudos podem ser otimizados. A intensidade de múons na superfície terrestre é bem conhecida como sendo anisotrópica e com uma dependência do ângulo zenital da forma ? (?) = ?0?osn(?). Por simplicidade nos cálculos, este expoente n é freqüentemente utilizado com valor igual a 2, mas estudos mostram que este parâmetro possui dependência com a posição geográfica e com a faixa de energia dos múons em questão. Esta dissertação propõe um método simples para a precisa determinação do expoente n e da intensidade vertical de múons simultaneamente, que pode ser realizado de maneira rá- pida em qualquer laboratório de raios cósmicos, utilizando detectores de partículas, que juntos formam o chamado Telescópio de Múons. Como resultado da aplicação do método no Laboratório de Léptons em Campinas - SP, foi obtido um valor de n de aproximadamente 2.30 e um valor para a intensidade vertical de múons em torno de 146.40? z/m2sr. Dados muito satisfatórios e de acordo com outros experimentos semelhantes já realizados anteriormente no Laboratório. O método também foi aplicado no Fermilab, localizado nos Estados Unidos. Nesta outra loca- lização geográfica, os resultados diferiram bastante dos obtidos em Campinas, com n aproxima- damente 3.66 e intensidade vertical de múons em torno de 158.33 ? zm-2sr-1. O mesmo experimento com o telescópio será realizado em outras posições geográficas afim de se verificar o comportamento do expoente n e da intensidade vertical de múons em diferentes locais
Abstract: The study of cosmic radiation is of utmost importance to astrophysics. Particles from different locations, from inside the solar system, and outside it, constantly arrive on Earth, carrying a lot of information about its origin. When these particles arrives to Earth¿s atmosphere they initiate a cascade of secondary particles resulting from the interaction of the primary cosmic ray with the atmosphere. From this rain of secondary particles, muons are the most abundant charged particles that reach the Earth¿s surface.Muons are highly penetrating, which can be a very big problem in some experiments, even if underground, of other particles. Because of their large number, they become extremely necessary in reconstructions of air showers to obtain information about the primary particle. Having knowledge of its characteristics, such as flux and distribution, noise in some experiments can be treated and other studies can be optimized.Muon intensity in the Earth¿s surface is well known to be anisotropic and has dependence on the zenith angle of ? (?) = ?0 cosn(?). For simplicity in the calculations, this n exponent is often used with a value of 2, but studies show that this parameter has dependence on the geographical position and on the energy range of muons in question. This dissertation proposes a simple method for accurate determination of the exponent n and muon vertical intensity simultaneously, that can be determined quickly in any laboratory cosmic rays using a particle detector, which was called Muon Telescope. As a result of the application of the method on the Leptons Laboratory, in Campinas - SP - Brazil, the value for n that was obtained is about 2.30 and a value for the vertical intensity of muons around 146.40? z/m2sr. This data is very satisfactory and according to similar experiments previously conducted at the Laboratory.This method was applied on Fermilab, located at the United States. On this new geographical location, the results were different from that obtained at Campinas, with n about 3.66 and the vertical intensity around 158.33 ? zm-2sr-1.The same experiment with the telescope will be held in other geographical locations in order to check the n exponent behavior and the muon intensity at different locations
Mestrado
Física
Mestra em Física
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Li, Cavoli Pierre. "Études théoriques et expérimentales des effets singuliers induits par les muons atmosphériques sur les technologies numériques d’échelle nanométrique." Thesis, Aix-Marseille, 2016. http://www.theses.fr/2016AIXM4098/document.
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Cette étude s’inscrit dans le domaine de la microélectronique. Elle consiste à étudier l’impact de la morphologie 3D du dépôt d’énergie sur la modélisation des événements singuliers (SEE) induits par les muons atmosphériques. La démarche a consisté dans un premier temps à modéliser le dépôt d’énergie induits par des protons dans des volumes nanométriques. Pour cela, le code Monte-Carlo GEANT4 a permis de simuler et de stocker dans une base de données, les caractéristiques des traces des dépôts d’énergie des protons. Une fois la démarche validée pour les protons, des simulations du dépôt d’énergie induit par des muons ont été réalisées. Une caméra CCD a été utilisée afin de réaliser des mesures de l’environnement radiatif atmosphérique et de contraindre la modélisation des dépôts d’énergie induits par les muons. Cette étude met en évidence et quantifie l’apport de considérer la distribution radiale du dépôt d’énergie induit par des protons pour des volumes nanométriques, dans les calculs de prédiction des SEE. En revanche, l’étude montre que la considération de la distribution radiale du dépôt d’énergie induit par des muons dans des volumes nanométriques a un impact négligeable sur la modélisation des SEE. Il serait intéressant de réaliser des mesures du dépôt d’énergie induit par des muons dans des technologies nanométriques sous accélérateur. Cela permettrait d’apporter des données expérimentales encore inexistantes, nécessaires au développement de nouveaux modèles physiques plus précis sur la modélisationdu dépôt d’énergie induit par des muonsThis study concerns the domain of the microelectronics. It consists in the studyof the impact of the 3D morphology of the energy deposit on the Single EventEffect (SEE) modeling, induced by atmospheric muons. Over a first phase, theapproach has consisted in the modeling of the energy deposit induced by protonsin nanometric volumes. For that purpose the use of the Monte Carlo code GEANT4has allowed to simulate and stock in a database the tracks characteristics of theenergy deposit induced by protons. Once the approach validated for the protons,simulations of the energy deposit induced by muons have been realized. A CCDcamera has been used in order to measure the radiative atmospheric environmentand to constrain the modeling of the energy deposit induced by muons. This studyhighlights and quantify the contribution of the radial distribution of the energydeposit incuced by protons in nanometric volumes for the SEE prediction. On theother hand, the study shows that the contribution of the radial distribution of theenergy deposit induced by muons in nanometric volumes has a negligeable impacton the SEE modeling. It will be interesting to realize measurements of the energydeposit induced by muons in nanometric technologies under accelerator. This willallow to bring experimental data still nonexistant necessary to the developpmentof new physical models more accurate on the modelization of the energy depositinduced by muons
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Reichhart, Lea. "ZEPLIN-III direct dark matter search : final results and measurements in support of next generation instruments." Thesis, University of Edinburgh, 2013. http://hdl.handle.net/1842/7914.
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Astrophysical observations give convincing evidence for a vast non-baryonic component, the so-called dark matter, accounting for over 20% of the overall content of our Universe. Direct dark matter search experiments explore the possibility of interactions of these dark matter particles with ordinary baryonic matter via elastic scattering resulting in single nuclear recoils. The ZEPLIN-III detector operated on the basis of a dualphase (liquid/gas) xenon target, recording events in two separate response channels { scintillation and ionisation. These allow discrimination between electron recoils (from background radiation) and the signal expected from Weakly Interacting Massive Particle (WIMP) elastic scatters. Following a productive first exposure, the detector was upgraded with a new array of ultra-low background photomultiplier tubes, reducing the electron recoil background by over an order of magnitude. A second major upgrade to the detector was the incorporation of a tonne-scale active veto detector system, surrounding the WIMP target. Calibration and science data taken in coincidence with ZEPLIN-III showed rejection of up to 30% of the dominant electron recoil background and over 60% of neutron induced nuclear recoils. Data taking for the second science run finished in May 2011 with a total accrued raw fiducial exposure of 1,344 kg days. With this extensive data set, from over 300 days of run time, a limit on the spin-independent WIMP-nucleon cross-section of 4.8 10-8 pb near 50 GeV/c2 WIMP mass with 90% confidence was set. This result combined with the first science run of ZEPLIN-III excludes the scalar cross-section above 3.9 10-8 pb. Studying the background data taken by the veto detector allowed a calculation of the neutron yield induced by high energy cosmic-ray muons in lead of (5.8 0.2) 10-3 neutrons/muon/(g/cm2) for a mean muon energy of 260 GeV. Measurements of this kind are of great importance for large scale direct dark matter search experiments and future rare event searches in general. Finally, this work includes a comprehensive measurement of the energy dependent quenching factor for low energy nuclear recoils in a plastic scintillator, such as from the ZEPLIN-III veto detector, increasing accuracy for future simulation packages featuring large scale plastic scintillator detector systems.
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Theodoro, Vanessa Menezes 1985. "Contribuição para os métodos de identificação das componentes eletromagnética e muônica de chuveiros atmosféricos extensos no Observatório Pierre Auger." [s.n.], 2011. http://repositorio.unicamp.br/jspui/handle/REPOSIP/278282.
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Orientadores: José Augusto Chinellato, Márcio Aparecido MüllerDissertação (mestrado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin
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Resumo: O Observatório Pierre Auger foi construído para detectar raios cósmicos de altas energias. Um dos principais objetivos das pesquisas realizadas pelo Observatório Auger, é o estudo da composição de massa dos raios cósmicos primários. O conteúdo muônico dos chuveiros atmosféricos extensos, produzidos a partir das interações dessas partículas primárias no alto da atmosfera, é um dos parâmetros mais sensíveis para o estudo da composição de massa. Ao nível do solo, as partículas detectadas com os 1600 tanques Cherenkov, que constituem o detector de superfície do Observatório, são essencialmente uma mistura de fótons, elétrons e pósitrons, que formam a componente eletromagnética; e os múons da componente muônica dos chuveiros extensos. A contribuição relativa dessas componentes depende do estágio de desenvolvimento do chuveiro e da distância radial ao eixo do mesmo. Nas regiões mais afastadas do eixo do chuveiro, num determinado estagio de seu desenvolvimento, um chuveiro iniciado por um núcleo de ferro, pode sob as mesmas condições que um chuveiro com primário de próton, induzir até 40% mais múons. Um dos métodos possíveis para estimar a contribuição muônica é o uso da estrutura temporal do sinal Cherenkov no detector de superfície. Esses sinais digitalizados em FADCs, mostram que múons induzem picos de sinais acima de um contínuo eletromagnético formado de pequenos picos. De forma que essa estrutura de sinal característica das componentes dependem da distância radial ao eixo do chuveiro. Esse trabalho tem como objetivo contribuir para a identificação e discriminação das componentes muônicas e eletromagnética dos chuveiros, a partir de um desenvolvimento matemático sobre o método de análise ¿Muon Jump¿. O método de jumps é baseado nas estruturais temporais dos sinais das componentes registrados pelos tanques Cherenkov do Observatório Auger e digitalizados em unidades FADCs. Usando essa característica estrutura temporal dos sinais, poderemos estimar o sinal de cada componente, definindo filtros de separação nas distribuições temporais dos sinais das frentes dos chuveiros e nas distribuições das derivadas desses sinais. Partindo dos diferentes sinais depositados por múons e partículas eletromagnéticas nos tanques Cherenkov, fizemos um estudo de contaminação desse sinal muônico pela componente eletromagnética, de forma individual e em frentes de chuveiros atmosféricos. Com isso, definimos o conceito de um filtro a ser aplicado nas distribuições de sinais, que nos permitisse separar de forma eficiente os sinais produzidos pelas partículas
Abstract: The Pierre Auger Observatory was built to detect high-energy cosmic rays. Studies of the mass composition of the highest energy cosmic rays is a major focus of research developed by the Pierre Auger Observatory. The muon content of the extensive air showers produced from the interactions of these primary particles with the atmosphere, is one of the most sensitive parameters to the mass composition. At the ground level, the detected particles by the Surface Detector of the Auger Observatory consists of 1660 water-Cherenkov detectors, are essentially a mixture of photons, electrons and positrons, the electromagnetic component, and muons, the muonic component. The relative contribution of these components depends on the stage developmental stage and on the radial distance of the showers. Far enough from the shower axis at a given development stage, a shower initiated by a iron primary may induce up to 40% more muons than a proton primary under the same conditions. The time structure of the Cherenkov signal profile in the surface detectors of particles reaching ground is used to estimate the muonic contribution. The Cherenkov signals are digitized as FADCs traces, and show that muons induce peaks signal above a continuous electromagnetic formed of small peaks. So this characteristic structure of the muonic and eletromagnetic peaks depend on the radial distance from the shower axis. The goals of my work is to contribute to the identification and discrimination of the eletromagnetic and muonic components, from a mathematical model to apply filters in the signal distributions of the particles. This method is based on the Jump method. Using the detailed time structure of signs, we can estimate the sign of each component, defining a set of separation filters to make an efficient selection of the muonic signal. The different signals deposited by muons and electromagnetic particles in Cherenkov tanks, allowed us to study the electromagnetic contamination in individual muonic signals and in the showers fronts
Mestrado
Física
Mestra em Física
41
Moreno, Thiago Victor 1988. "Comparação entre produção de múons nos chuveiros atmosféricos extensos observados no Observatório Pierre Auger e nos detetores do experimento CMS do CERN, a partir de colisões próton-próton." [s.n.], 2014. http://repositorio.unicamp.br/jspui/handle/REPOSIP/277005.
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Orientador: José Augusto ChinellatoDissertação (mestrado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin
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Resumo: Neste trabalho o programa CORSIKA foi utilizado para gerar eventos de colisão próton-próton e chuveiros atmosféricos extensos com partícula primária sendo próton ou ferro. Como modelo de interações hadrônicas usou-se o EPOS LHC, QGSJET 01c, QGSJET II-4 e SIBYLL 2,1. As colisões p-p foram simuladas com energia igual a 7 TeV no referencial centro de momenta e foi estudada a distribuição de multiplicidade de hádrons carregados e a densidade em pseudorapidez. Comparando estes observáveis com dados do CMS escolheu-se os modelos que melhor reproduzissem os dados para posteriormente, simular chuveiros atmosféricos extensos. Estes chuveiros foram gerados com partícula primária de energia igual a 1019eV no referencial do laboratório. Observou-se a densidade de múons na altitude do Detetor de Superfície do Observatório de raios cósmicos Pierre Auger. O objetivo é estudar a possibilidade de usar esta densidade para sondar modelos de interações hadrônicas e identificar a partícula primária dos eventos detetados pelo Observatório Pierre Auger
Abstract: In this work CORSIKA program was used to generate events from proton-proton collision and extensive air showers with primary particle being proton or iron. The hadronic interaction models used was EPOS LHC, QGSJET 01c, QGSJET II-4 and SIBYLL 2,1. The p-p collisions were simulated with energy equal to 7 TeV in the center of momenta reference system and the charged hadron multiplicity and the pseudorapidity density was studied. Comparing this with data collected by the CMS detector at the LHC it was chosen the best models to generate air showers. The extensive air showers were generated with primary particle energy equal to 1019 eV in the laboratory frame. It was observed the muon density in the altitude of the Surface Detector of the Pierre Auger Observatory. The objective is to study the possibility of using this density to probe the model and the primary particle of the events detected by the Pierre Auger Observatory
Mestrado
Física
Mestre em Física
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Medeiros, Michelle Mesquita de. "Estudo e simulação do déficit de raios cósmicos devido à lua no experimento MINOS." Universidade Federal de Goiás, 2011. http://repositorio.bc.ufg.br/tede/handle/tde/2907.
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Dissertacao Michelle M de Medeiros.pdf: 2738633 bytes, checksum: e1e98c1ee5ac88193602d29a282e5c6b (MD5)Made available in DSpace on 2014-08-15T15:17:28Z (GMT). No. of bitstreams: 2 license_rdf: 23148 bytes, checksum: 9da0b6dfac957114c6a7714714b86306 (MD5) Dissertacao Michelle M de Medeiros.pdf: 2738633 bytes, checksum: e1e98c1ee5ac88193602d29a282e5c6b (MD5) Previous issue date: 2011-09-01
Coordenação de Aperfeiçoamento de Pessoal de Nível Superior - CAPES
Conselho Nacional de Pesquisa e Desenvolvimento Científico e Tecnológico - CNPq
Celestial objects
Objetos celestes como a Lua e o Sol bloqueiam os raios cósmicos que vem de suas direções para a Terra, produzindo um défcit chamado de sombra. A medida deste défcit possibilita a determinação da resolução angular e do alinhamento de detectores de raios cósmicos, o estudo dos campos magnéticos terrestre, solar e interplanetário e a determinação da razão antipróton/próton na escala de energia TeV. Vários experimentos já observaram a sombra de raios cósmicos da Lua e/ou do Sol com o objetivo de calibrar seus detectores. Descrevemos neste trabalho o experimento MINOS e seus resultados da sombra da Lua e do Sol. Simulamos a sombra da Lua levando em conta seu movimento no céu e, para tanto, de nimos e testamos métodos de simulação e diferentes composições para os raios cósmicos. Também avaliamos várias proporções para antiprótons no fluxo de raios cósmicos a m de comparar com os resultados do experimento MINOS e conjecturar uma possível razão p=p para os dados observados. Ambos os métodos que de nimos, método do dé cit e da fonte de raios cósmicos, permitiram uma análise qualitativa da sombra. No entanto, só foi possível realizar uma análise quantitativa na simulação tendo a Lua como um défcit. Dessa forma, adotamos este método para as simulações subsequentes. Notamos algumas diferenças para as sombras obtidas usando próton e núcleo de hélio como partículas primárias de raios cósmicos. Todavia, a sombra encontrada combinando prótons (90%) e núcleos de hélio (10%) foi semelhante à sombra obtida apenas para prótons. Na simulação incluindo o movimento da Lua, avaliamos os efeitos do campo geomagnético na partícula primária, desde a Lua até a atmosfera terrestre, e nos múons (partícula secundária) desde sua produção até o nível do mar. Como esperado, obtivemos uma sombra da Lua mais similar com os resultados do experimento MINOS ao incluir a de exão tanto das partículas primárias dos raios cósmicos quanto das partículas do chuveiro do que considerando apenas o desvio destas últimas. Nossa simulação foi capaz de reproduzir a sombra provocada pela Lua com a localização do maior dé cit comparável àquela encontrada pelo experimento MINOS. Entretanto, ainda acrescentamos núcleos de hélio e antiprótons na simulação incluindo o movimento da Lua com o objetivo de melhorar o resultado. Obtivemos um défcit localizado o mais próximo possível do obtido pelo experimento MINOS usando a proporção p=p = 0;45. Tal resultado deve ser melhor estudado e a simulação aprimorada para que se determine esta razão entre antiprótons e prótons com a precisão adequada.
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Martraire, Diane. "Étude du pouvoir de discrimination des primaires initiant les grandes gerbes atmosphériques avec des réseaux de détecteurs au sol : analyse des rayons cosmiques de ultra haute énergie détectés à l’observatoire Pierre Auger, Estimation des performances pour la detection de gamma de très haute énergie du future observatoire LHAASO." Thesis, Paris 11, 2014. http://www.theses.fr/2014PA112276/document.
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Depuis plus d’un siècle, les rayons cosmiques d’ultra-haute énergie (RCUHE), ayant une énergie supérieure à 1018 eV, continuent d’entretenir le mystère : Quelle est leur composition ? D’où viennent-ils ? Comment atteignent-ils de telles énergies ? Ces particules chargées, suffisamment énergétiques pour atteindre la Terre, forment des gerbes de particules secondaires via leurs interactions avec l’atmosphère dont le développement est caractéristique de la nature de la particule primaire. L’observatoire Pierre Auger, avec sa structure hybride et son gigantesque réseau de détecteurs peuvent apporter des réponses. L’étude de la composition des RCUHEs a été étudiée avec le réseau de surface de l’observatoire Pierre Auger. Cette dernière est cruciale à la fois pour comprendre les interactions hadroniques, qui constituent le développement des gerbes, et pour identifier leurs sources. Cela peut également aider à comprendre l’origine de la coupure spectrale aux plus hautes énergies : s’agit-il de la coupure GZK ou à l’extinction des sources. Toutes ces raisons motivent la première partie de la thèse, à savoir la mise en place d’une méthode permettant d’extraire la composante muonique des gerbes atmosphériques et d’en déduire la composition. Les résultats de cette méthode montrent une dépendance de la composition avec la distance à l’axe de la gerbe, qui pourrait aider à améliorer les modèles hadroniques. Dans les conditions actuelles du réseau de surface, l’identification de la composante muonique présente des limites.La seconde partie est consacrée au nouvel observatoire en Chine, LHAASO. Ce projet s’intéresse à l’étude des gammas supérieurs à 30 TeV, qui signeraient l’accélération de proton dans la galaxie, donnant ainsi des informations indirectes sur les rayons cosmiques. D’autre part, l’observatoire vise à étudier les rayons cosmiques entre 10 TeV et 1 EeV, région où le spectre en énergie présente une rupture. Cette région nécessite de pouvoir discriminer les gammas des rayons cosmiques. A ce titre, l’un des détecteurs de LHAASO, le KM2A, a été simulé et son pouvoir de discrimination gamma/hadron évaluéDuring the past century, ultra-high-energy cosmic rays (UHECR), those with an energy larger than 1018 eV, remain as a mystery: What are cosmic rays? Where do they come from? How do they attain their huge energy? When these charged particles strike the earth's atmosphere, they dissipate their energy by generating a shower of secondary particles whose development is significantly different depending on the nature of the primaries. The Pierre Auger observatory, with its hybrid structure and huge size network of ground detectors, can shed some light into these questions.The study of the composition of UHECR was performed with the Pierre Auger apparatus. This is crucial both to understand the hadronic interactions, which govern the evolution of showers, and to identify their sources. It can help to understand the origin of the energy spectrum cut-off: is it the GZK cut-off or the exhaustion of sources? These reasons motivate the first part of this thesis: the development of a method to extract the muonic component of air showers and deduce the implications on the composition of UHECR at the Pierre Auger observatory. The results of this method show a dependence of the composition with the distance to the axis of the shower, which could help to improve the hadronic models. The determination of the muon component is limited by the surface detector setup.The second part is devoted to the new observatory in China, LHAASO. This project focuses on the study of gamma rays with an energy higher than 30 TeV, which probe the acceleration of protons in the galaxy, providing indirect information on cosmic rays. Moreover, the observatory studies cosmic rays between 10 TeV and 1 EeV, one of the regions where the energy spectrum presents a break. This region requires the ability to discriminate gamma rays and cosmic rays. For this reason, one of the detectors of LHAASO, the KM2A, was simulated and its power of discrimination gamma/hadron evaluated
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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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Chang, CHIH-CHIA, and 張智嘉. "Using Cosmic Ray Muon Detector to measure the muon lifetime." Thesis, 2009. http://ndltd.ncl.edu.tw/handle/13654337684435055675.
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碩士輔仁大學
物理學系
97
We use the quarknet muon detector to measure the muon lifetime and flux. The detector is made by Fermilab, USA. In the muon lifetime study, we find the results in our lab are similar as the PDG world average, ~2.2 micro seconds. One day, we take the detector to Yu-San mountain and repeat the muon lifetime data taking. We find that the muon lifetime is too small. We wonder that some other high energy charged pion particles may affect our results. In the flux study, we find that the flux would become smaller while the angle between the scintillator plane and the horizontal increases. The behavior can be described by the cosine square function. Besides, the flux in the higher story is larger than that in the lower story. The quarknet project in Taiwan becomes better and better this year. We hope to distribute the knowledge of cosmic ray related issues to high school students and teachers. Hopefully, this thesis would help people to learn this.
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"Cosmic muon-induced neutron background study in underground laboratories." 2008. http://library.cuhk.edu.hk/record=b5896850.
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Luk, Wing Hong Antony = 地底實驗室的渺子致中子本底研究 / 陸永康.Thesis (M.Phil.)--Chinese University of Hong Kong, 2008.
Includes bibliographical references (leaves 74-77).
Abstracts in English and Chinese.
Luk, Wing Hong Antony = Di di shi yan shi de miao zi zhi zhong zi ben di yan jiu / Lu Yongkang.
Chapter 1 --- Introduction --- p.1
Chapter 1.1 --- Muons at Earth´ةs Surface --- p.1
Chapter 1.2 --- Underground Muons --- p.2
Chapter 1.2.1 --- Muon Intensity --- p.2
Chapter 1.2.2 --- Muon Energy --- p.6
Chapter 1.3 --- Muon-induced Neutrons --- p.7
Chapter 1.3.1 --- Production of Neutrons from Muons --- p.7
Chapter 1.3.2 --- The Influence of Muon-induced Neutrons on Underground Experiments --- p.9
Chapter 1.4 --- Aberdeen Tunnel Laboratory --- p.11
Chapter 1.4.1 --- Geological Properties --- p.12
Chapter 1.4.2 --- Detectors Description --- p.14
Chapter 1.4.3 --- Detection Principles --- p.18
Chapter 2 --- Simulation of Cosmic Muons for Aberdeen Tunnel Laboratory --- p.22
Chapter 2.1 --- Muon Spectrum at Sea level --- p.22
Chapter 2.2 --- Simulation of Muon Propagation through Rock --- p.23
Chapter 2.3 --- Estimation of Expected Event Rate for the Muon Tracker --- p.28
Chapter 3 --- Neutron Detector Simulation --- p.30
Chapter 3.1 --- Simulation Parameters --- p.32
Chapter 3.2 --- Energy Response --- p.35
Chapter 3.3 --- Energy Resolution --- p.35
Chapter 3.4 --- Neutron Drift Distance and Capture Efficiency --- p.40
Chapter 3.5 --- Neutron Detection Efficiency --- p.42
Chapter 3.6 --- Photons Arrival Time --- p.45
Chapter 3.6.1 --- Cobalt-60 Source --- p.45
Chapter 3.6.2 --- LED --- p.47
Chapter 4 --- Simulation of Muon-induced Neutron Background --- p.49
Chapter 4.1 --- Review on Muon-induced Neutron Simulations --- p.50
Chapter 4.1.1 --- Methodology --- p.50
Chapter 4.1.2 --- Results in the Literature --- p.52
Chapter 4.1.3 --- Simulation of Muon-induced Neutrons in GdLS --- p.56
Chapter 4.2 --- Full Monte Carlo Simulation of Expected Neutron Rate --- p.64
Chapter 4.2.1 --- Simulation Details --- p.65
Chapter 4.2.2 --- Results --- p.65
Chapter 4.3 --- Estimation of the Expected Neutron Rate using Parameterization from Monte Carlo Simulations --- p.68
Chapter 4.3.1 --- Simulation Details --- p.68
Chapter 4.3.2 --- Results --- p.69
Chapter 4.4 --- Summary --- p.71
Chapter 5 --- Future Work --- p.72
Chapter 5.1 --- Neutrons from Rock Radioactivity --- p.72
Chapter 5.2 --- Muon-induced Neutrons from Rock --- p.73
Chapter 5.3 --- Variation of Muon flux --- p.73
Bibliography --- p.74
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"comprehensive study of cosmic muon and muonic reaction in Aberdeen tunnel experiment." 2011. http://library.cuhk.edu.hk/record=b5894797.
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Ngan, Sze Yuen = 渺子及其於香港仔隧道實驗室內的綜合研究 / 顏思遠.Thesis (M.Phil.)--Chinese University of Hong Kong, 2011.
Includes bibliographical references (leaves 84-85).
Abstracts in English and Chinese.
Ngan, Sze Yuen = Miao zi ji qi yu Xianggangzi sui dao shi yan shi nei de zong he yan jiu / Yan Siyuan.
Chapter 1 --- Introduction --- p.1
Chapter 1.1 --- Cosmic Rays --- p.1
Chapter 1.2 --- Muons --- p.3
Chapter 1.3 --- Neutrino Oscillation --- p.5
Chapter 1.4 --- The Daya Bay Reactor Neutrino Experiment --- p.8
Chapter 1.4.1 --- Overview --- p.8
Chapter 1.4.2 --- Detection Mechanism --- p.9
Chapter 1.5 --- The Aberdeen Tunnel Experiment --- p.11
Chapter 1.5.1 --- Overview --- p.11
Chapter 1.5.2 --- Muon Tracker --- p.13
Chapter 1.5.3 --- Neutron Detector --- p.16
Chapter 2 --- Underground Muons --- p.18
Chapter 2.1 --- Muon Simulation in the Daya Bay Experiment --- p.18
Chapter 2.1.1 --- Gaisser's Formula --- p.20
Chapter 2.1.2 --- Digitization of the Geographical Profile --- p.23
Chapter 2.1.3 --- Underground Muon Flux --- p.24
Chapter 2.2 --- Muon Simulation in the Aberdeen Tunnel Experiment --- p.25
Chapter 3 --- Muon Behaviors in the Aberdeen Tunnel Laboratory --- p.28
Chapter 3.1 --- Preparation --- p.29
Chapter 3.1.1 --- Definition of the Coordinate System --- p.29
Chapter 3.1.2 --- Generation of Muon Events --- p.30
Chapter 3.1.3 --- Muon Trajectory --- p.35
Chapter 3.1.4 --- Muon Energy Dissipation --- p.36
Chapter 3.2 --- Muon Detection by the ND --- p.38
Chapter 3.2.1 --- Energy Deposition in Gd-LS --- p.38
Chapter 3.2.2 --- Experimental Measurements and Comparison --- p.40
Chapter 3.2.3 --- Energy Deposition in MO --- p.42
Chapter 3.2.4 --- ND Muon Rate --- p.43
Chapter 3.2.5 --- Stopping Muons and Muon Decay --- p.44
Chapter 3.3 --- Muon Detection by the Muon Tracker --- p.46
Chapter 3.3.1 --- Selection of Top-Bottom Muons --- p.47
Chapter 3.3.2 --- Selection of Muons which cut the Gd-LS Volume Diagonally --- p.49
Chapter 4 --- Optimization of the Photomultiplier Tubes --- p.52
Chapter 4.1 --- Photomultiplier Tube --- p.52
Chapter 4.2 --- The Earth Field Effect --- p.55
Chapter 4.2.1 --- FINEMET Magnetic Shield on PMT --- p.56
Chapter 4.2.2 --- Magnetic Fields Measurement near the PMT Mount --- p.63
Chapter 4.3 --- p-sec Region Ringing in PMT Signal --- p.65
Chapter 4.3.1 --- The PMT Body and Simulated PMT Signal --- p.67
Chapter 4.3.2 --- The Dummy Base --- p.69
Chapter 4.3.3 --- High Voltage and the PMT Base Design --- p.71
Chapter 5 --- Summary --- p.81
Chapter 5.1 --- Underground Muon simulation --- p.81
Chapter 5.2 --- Optimization of the PMTs in the Daya Bay Experiment --- p.82
Bibliography --- p.84
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"Study of cosmic-ray muons and muons induced neutrons." 2013. http://library.cuhk.edu.hk/record=b5884495.
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Tam, Yiu Ho = 宇宙射線渺子及其引致中子的研究 / 譚耀豪.Thesis (Ph.D.)--Chinese University of Hong Kong, 2013.
Includes bibliographical references (leaves 148-153).
Electronic reproduction. Hong Kong : Chinese University of Hong Kong, [2012] System requirements: Adobe Acrobat Reader. Available via World Wide Web.
Abstracts also in Chinese.
Tam, Yiu Ho = Yu zhou she xian miao zi ji qi yin zhi zhong zi de yan jiu / Tan Yaohao.
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O'Connor, Daniel Joseph. "Cosmic ray muons in the deep ocean." Thesis, 1990. http://hdl.handle.net/10125/10074.
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"Study of cosmic muons at the Aberdeen underground lab." 2010. http://library.cuhk.edu.hk/record=b5894456.
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Wong, Koon Kei Jackie = 香港仔地底實驗室中的宇宙渺子研究 / 黃冠棋.Thesis (M.Phil.)--Chinese University of Hong Kong, 2010.
Includes bibliographical references (leaves 74-76).
Abstracts in English and Chinese.
Wong, Koon Kei Jackie = Xianggangzi di di shi yan shi zhong de yu zhou miao zi yan jiu / Huang Guanqi.
Chapter 1 --- Introduction --- p.1
Chapter 1.1 --- Motivation --- p.1
Chapter 1.1.1 --- Neutrino Oscillation --- p.1
Chapter 1.1.2 --- The Daya Bay Reactor Neutrino Experiment --- p.5
Chapter 1.2 --- Cosmic muons --- p.8
Chapter 1.2.1 --- Propagation of cosmic muons --- p.10
Chapter 1.3 --- Aberdeen Tunnel Experiment --- p.11
Chapter 1.3.1 --- Detection principles of Muon Tracker --- p.13
Chapter 1.3.2 --- Detection principles of Neutron Detector --- p.16
Chapter 1.3.3 --- The data acquisition (DAQ) and online monitoring system --- p.17
Chapter 2 --- Study of Angular distribution of the Expected Muon Flux --- p.20
Chapter 2.1 --- Determination of muon angular distribution detected by the muon tracker --- p.21
Chapter 2.2 --- Spherical Harmonics Expansion of muon angular distribution --- p.29
Chapter 3 --- Hardware Development of the Muon Tracker --- p.35
Chapter 3.1 --- Front-end electronics board --- p.35
Chapter 3.1.1 --- The circuit of front-end daughter board --- p.37
Chapter 3.1.2 --- Test of the front-end daughter board --- p.39
Chapter 3.2 --- Muon tracker PMT gain calibration --- p.45
Chapter 4 --- Photomultiplier tubes (PMT) characterization --- p.48
Chapter 4.1 --- Magnetic field test --- p.49
Chapter 4.2 --- Nonlinearity test --- p.54
Chapter 4.2.1 --- Two-LED system --- p.54
Chapter 4.2.2 --- LED and reference PMT system --- p.56
Chapter 4.3 --- Optimization of waveform --- p.59
Chapter 4.4 --- Comparison with Hamamatsu's recommended PMT bases --- p.65
Chapter 5 --- Summary --- p.71
Chapter 5.1 --- Calculations about muon angular distribution --- p.71
Chapter 5.2 --- Front-end electronics tests and PMT measurements --- p.71
Chapter 5.3 --- Outlook for the Aberdeen Tunnel Experiment --- p.72
Bibliography --- p.74