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The energy calibration for the solar neutrino analysis of all three phases of the Sudbury Neutrino ObservatoryMacLellan, Ryan 26 September 2009 (has links)
This work presents the calibration of the energy response of the Sudbury Neutrino
Observatory (SNO). The development of the energy response processor RSP and its
use in setting the energy scale of SNO and reconstructing the energy
of neutrino-like events is presented for each of the three phases of SNO: the pure
heavy water phase, the salt phase, and the neutral current detector (NCD) phase. A 16N calibration
source, producing mainly 6.13 MeV γ-rays, is the primary energy calibration source.
It is used to set the energy scale of the detector and to test for errors in the energy
calibration and reconstruction process. The errors associated with energy reconstruction in the pure heavy water and salt phase data, that is to be used in a low energy threshold
solar 8B neutrino analysis, are derived for the RSP energy response processor and
shown to be in agreement with other analyses. The largest of the errors, that associated with using the 16N source to set the energy scale of the detector, is improved
through a detailed and thorough analysis.
The calibration of the energy scale of the photomultiplier tube array in the third
phase, with an array of 3He proportional counters (NCDs) distributed within the heavy water, is presented. The event energy reconstruction errors in the NCD phase are reassessed
with more precise measurements and shown to be in agreement with the conservative
estimates used in the analysis SNO presented in 2008. The implications of the improvements in the
error are assessed and the solar 8B neutrino fluxes—charged current (CC), elastic
scattering (ES), and neutral current (NC)—are determined to be:
φCC = 1.68+0.09−0.07,
φES = 1.79+0.25-0.22, and
φNC = 5.52+0.48-0.45,
in units of 10^6/cm^2/s. The errors quoted are the combined statistical and systematic
uncertainties. These results are in good agreement with the results published by SNO in 2008 with a modest improvement in the CC measurement. / Thesis (Ph.D, Physics, Engineering Physics and Astronomy) -- Queen's University, 2009-09-23 01:40:45.237
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An Underwater Six-Camera Array for Monitoring and Position Measurements in SNO+Petriw, Zachary D. Unknown Date
No description available.
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A Cascade Analysis for the IceCube Neutrino TelescopeHickford, Stephanie Virginia January 2012 (has links)
IceCube is the largest operating neutrino observatory. An array of photomultiplier tubes deployed throughout a cubic kilometre of the Antarctic ice at the South Pole detect the Cherenkov radiation from neutrino-nucleon interactions. IceCube is capable of detecting neutrinos over a large energy range. The physics manifesto includes dark
matter searches, cosmic ray observation, all sky point source searches, and particle physics parameter constraints. Astrophysical neutrinos are expected to originate from hadronic interactions in some of the most energetic regions in the Universe. The detection of high energy astrophysical neutrinos will provide direct information about the astrophysical sources that produced them.
This thesis concentrates on the cascade channel for neutrino detection. Two separate studies are performed; a high energy cascade analysis and a parameterisation of the production of muons within hadronic cascades.
The experimental data for the cascade analysis was taken by IceCube from April 2008 to May 2009 when the first 40 IceCube strings were deployed and operational. The analysis was designed to isolate the astrophysical neutrino signal from the atmospheric and muon background. Fourteen cascade-like events were observed, on a background of 2.2 ⁺⁰·⁶ ₋₀·₈
atmospheric neutrino events and 7.7 ± 1.0 atmospheric muon events. This gives a 90% confidence level upper limit of ΦlimE²≤ 7.46 × 10⁻⁸ GeVsr⁻¹s⁻¹cm⁻²
, assuming an E⁻² spectrum and a neutrino flavour ratio of 1 : 1 : 1, for the energy range 25.12 TeV to 5011.87 TeV.
Decay of hadronic particles in cascades produces muons. If the muons are energetic enough they can significantly alter the topology of the cascade and hence the reconstruction of the event in an analysis. The production of high energy muons within hadronic cascades was simulated and parameterised using Pythia and GEANT simulation programs.
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Simulation of Cascades for the IceCube Neutrino TelescopeHickford, Stephanie Virginia January 2007 (has links)
Neutrino telescopes open a new observational window on the universe. Neutrino interactions in these detectors can give rise to a combination of electromagnetic cascades, hadronic cascades and long range muons. Cerenkov radiation from these products is detected by the neutrino telescope. In this thesis the observational signatures associated with various neutrino-nucleon interaction products are investigated. Cerenkov radiation is emitted at a distinctive angle, about 40o in ice. The maximum number of optical photons that can be produced per unit charged tracklength is calculated to be 562 photons cm−1. The simulation programs Pythia and GEANT are used to study neutrino interactions using ice as the medium. The production of tau from the tau neutrino interaction is considered and it is found that the Cerenkov angle from tau is not distinctive at low energies, due to its lifetime tau decays before travelling an observable distance. The energy required for a tau neutrino to produce a sharp tau Cerenkov signal is on the order of 1 PeV. In a high energy electron neutrino interaction the resulting hadronic cascade contains high energy pions and kaons. These particles decay, often producing muons that are also high energy and therefore long range. Due to the muons travelling faster than the local speed of light in ice, their signal may be received by the detector earlier than the signal resulting from the event that created the muon. This can complicate the reconstruction of electron neutrino events.
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Search for neutron oscillation and study of neutrino reaction rates using multiprong events in Soudan 2 /Chung, Jin-Hyuk. January 2001 (has links)
Thesis (Ph.D.)--Tufts University, 2001. / Adviser: W. Anthony Mann. Submitted to the Dept. of Physics. Includes bibliographical references (leaves 125-130). Access restricted to members of the Tufts University community. Also available via the World Wide Web;
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A search for [nu mu to nu e] oscillations in the NOMAD experimentGodley, Andrew R. January 2000 (has links)
Thesis (Ph. D.)--University of Sydney, 2001. / Squiggly right arrow used in title. Title from title screen (viewed Apr. 23, 2008). Submitted in fulfilment of the requirements for the degree of Doctor of Philosophy to the School of Physics, Faculty of Science. Degree awarded 2001; thesis submitted 2000. Includes bibliography. Also available in print form.
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Neutrino interactions and nuclear effects in oscillation experiments and the nonperturbative dispersive sector in strong (quasi-) Abelian fieldsYu, Ji-Young. January 2002 (has links)
Dortmund, Univ., Diss., 2002. / Computerdatei im Fernzugriff.
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Neutrino interactions and nuclear effects in oscillation experiments and the nonperturbative dispersive sector in strong (quasi-) Abelian fieldsYu, Ji-Young. January 2002 (has links)
Dortmund, Univ., Diss., 2002. / Computerdatei im Fernzugriff.
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Development of metal loaded liquid scintillators for future detectors to investigate neutrino propertiesBuck, Christian. Unknown Date (has links) (PDF)
University, Diss., 2004--Heidelberg.
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Limites nos parâmetros do modelo de oscilação com decaimento de neutrinos usando os dados do experimento MINOS / Limits on the parameters of the neutrino decay oscillation model using data from the MINOS experimentGomes, Abner Leonel Gadelha 13 March 2014 (has links)
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Previous issue date: 2014-03-13 / Coordenação de Aperfeiçoamento de Pessoal de Nível Superior - CAPES / We use the and produced from MINOS beam line that recently reported a
disappearence analysis using their full data and combining the beam line and atmospheric
neutrinos and antineutrinos events. We used their beam data analysis to constrain the
neutrino lifetime under the oscillation plus decay framework. Our analysis reports 3 <
1:4 103 GeV=s, which corresponds to a decay lifetime 3=m3 > 2:4 1012 s=eV ,
improving a previous MINOS measurement who is 3=m3 > 2:1 1012 s=eV . / Usamos dados de e produzidos da linha de feixe do experimento MINOS publicados
recentemente em uma análise de desaparecimento de neutrinos muônicos utilizando
dados completos de neutrinos e antineutrinos da linha de feixe e atmosféricos. Estabelecemos
limites sobre a razão tempo de vida por massa do neutrino para o modelo de
oscilação com decaimento. Obtivemos da análise um limite superior de 3 < 1;4 103
GeV=s, que corresponde a um tempo de vida de 3=m3 > 2;4 1012 s=eV no limite
inferior, melhorando a medida anterior do MINOS que era de 3=m3 > 2;1 1012 s=eV .
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