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

No description available.

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.

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.

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;

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.

Dortmund, Univ., Diss., 2002. / Computerdatei im Fernzugriff.

Dortmund, Univ., Diss., 2002. / Computerdatei im Fernzugriff.

University, Diss., 2004--Heidelberg.

Submitted by JÚLIO HEBER SILVA (julioheber@yahoo.com.br) on 2017-06-23T17:07:23Z No. of bitstreams: 2 Dissertação - Abner Leonel Gadelha Gomes - 2013.pdf: 12566466 bytes, checksum: de6788671342c72dc83a388cf0a1f093 (MD5) license_rdf: 0 bytes, checksum: d41d8cd98f00b204e9800998ecf8427e (MD5) / Approved for entry into archive by Cláudia Bueno (claudiamoura18@gmail.com) on 2017-07-07T20:24:16Z (GMT) No. of bitstreams: 2 Dissertação - Abner Leonel Gadelha Gomes - 2013.pdf: 12566466 bytes, checksum: de6788671342c72dc83a388cf0a1f093 (MD5) license_rdf: 0 bytes, checksum: d41d8cd98f00b204e9800998ecf8427e (MD5) / Made available in DSpace on 2017-07-07T20:24:16Z (GMT). No. of bitstreams: 2 Dissertação - Abner Leonel Gadelha Gomes - 2013.pdf: 12566466 bytes, checksum: de6788671342c72dc83a388cf0a1f093 (MD5) license_rdf: 0 bytes, checksum: d41d8cd98f00b204e9800998ecf8427e (MD5) 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 10􀀀3 GeV=s, which corresponds to a decay lifetime 3=m3 > 2:4 10􀀀12 s=eV , improving a previous MINOS measurement who is 3=m3 > 2:1 10􀀀12 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 10􀀀3 GeV=s, que corresponde a um tempo de vida de 3=m3 > 2;4 10􀀀12 s=eV no limite inferior, melhorando a medida anterior do MINOS que era de 3=m3 > 2;1 10􀀀12 s=eV .