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Dissertations / Theses on the topic 'Solar Neutrino Observatory'

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Published: 4 June 2021

Last updated: 1 February 2022

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1

Miknaitis, Kathryn Kelly Schaffer. "A search for matter enhanced neutrino oscillations through measurements of day and night solar neutrino fluxes at the Sudbury Neutrino Observatory /." Thesis, Connect to this title online; UW restricted, 2005. http://hdl.handle.net/1773/9636.

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2

Laberge, Gaetan (Gaetan Joseph Henri) Carleton University Dissertation Physics. "212Pb assay for the determination of the neutral current background at the Sudbury Neutrino Observatory." Ottawa, 1995.

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3

Smith, Miles Walter Eldon. "An investigation of matter enhanced neutrino oscillation with the Sudbury Neutrino Observatory /." Thesis, Connect to this title online; UW restricted, 2002. http://hdl.handle.net/1773/9701.

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4

Thornewell, Peter Michael. "Â³He neutral current detectors for the Sudbury Neutrino Observatory." Thesis, University of Oxford, 1997. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.343004.

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5

Loach, James Chilton. "Measurement of the Flux of 8B Solar Neutrinos at the Sudbury Neutrino Observatory." Thesis, University of Oxford, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.490107.

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The Sudbury Neutrino Observatory (SNO) was a heavy water Cerenkov detector that had the unique ability to measure both the total il active flux of solar neutrino, using a neutral current (NC) interaction, and the flux of electron neutrinos, using a charged current (CC) interaction. The experiment has demonstrated that neutrinos 3 change flavour and that the total neutrino flux is consistent with the prediction of solar models.

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6

Heron, Heidi. "Techniques to measure the NC background in the SNO experiment." Thesis, University of Oxford, 1998. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.244578.

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7

DeKok, Alan (Alan T. ). Carleton University Dissertation Physics. "A Process degasser for the SNO Ultra-pure light water facility." Ottawa, 1996.

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8

Paterson, David John Carleton University Dissertation Physics. "Studies of a novel method for solar neutrino neutral current detection in the Sudbury neutrino observatory." Ottawa, 1989.

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9

Yeung, Alan B. (Alan Brian) Carleton University Dissertation Physics. "A Monte Carlo study of the Sudbury Neutrino Observatory small test detector experiment." Ottawa, 1990.

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10

Stonehill, Laura C. "Deployment and background characterization of the Sudbury Neutrino Observatory neutral current detectors /." Thesis, Connect to this title online; UW restricted, 2005. http://hdl.handle.net/1773/9665.

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11

Lay, Michael David. "Creation and detection of Cerenkov light in the Sudbury Neutrino Observatory." Thesis, University of Oxford, 1994. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.239323.

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12

Wilson, Jeanne R. "A measurement of the â¸B solar neutrino energy spectrum at the Sudbury Neutrino Observatory." Thesis, University of Oxford, 2004. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.409729.

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13

Orebi, Gann Gabriel D. "An improved measurement of the B Solar Neutrino energy spectrum at the sudbury neutrino observatory." Thesis, University of Oxford, 2008. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.510201.

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14

Chen, Xin. "Monte Carlo simulations and analyses of backgrounds in the Sudbury Neutrino Observatory." Thesis, University of Oxford, 1997. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.244717.

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15

Orrell, John Laurence. "A search for an electron antineutrino signal in the Sudbury Neutrino Observatory /." Thesis, Connect to this title online; UW restricted, 2004. http://hdl.handle.net/1773/9794.

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16

O'Keeffe, Helen Mary. "Low energy background in the NCD phase of the Sudbury Neutrino Observatory." Thesis, University of Oxford, 2008. http://ora.ox.ac.uk/objects/uuid:b53c04b1-5dba-4cfb-98ec-c0d8b87fb58b.

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The Sudbury Neutrino Observatory (SNO) was a 1 kilotonne heavy water Č{C}erenkov detector. Evidence for flavour changing neutrino oscillations was found by comparing the rate of Charged Current interactions with that of Neutral Current (NC) interactions. This thesis is concerned with the accurate determination of the NC flux in the Neutral Current Detector (NCD) phase of SNO. The measurement and understanding of radioactive backgrounds arising from decays of naturally occurring $^{232}$Th and $^{238}$U chain nuclei is crucial. This is because their daughter nuclei can produce neutrons via photodisintegration of deuterium. These would be indistinguishable from those produced by NC neutrino interactions. As the probability of neutron production was dependent upon the nature and location of activity, each contribution had to be determined separately. Of particular concern were $^{232}$Th and $^{238}$U in the D$_2$O and Neutral Current Detectors (NCDs). A maximum likelihood method was developed that exploited differences in the event isotropy and radial profile of each event class. These results were in agreement with water assay results and pre-deployment radioassays of the NCDs. An independent measurement of the $^{232}$Th content in the D$_2$O and H$_2$O was made by regularly assaying the water using filters loaded with hydrous titanium oxide. The concentration of $^{232}$Th in the water was determined by coincidence counting of the final assay sample. A new counter system was designed and built and the calibration and use of this system are presented. Two areas of increased activity were discovered on two of the NCDs deployed in the detector which would have prevented an accurate measurement of the NC flux. A method was devised to determine the composition and activity of one of these hotspots. The results were in good agreement with two independent methods and the uncertainty on the NC flux was reduced from $>7$% to $<1$%. The total number of neutrons produced per day by photodisintegration for $^{232}$Th and $^{238}$U in the D$_2$O and NCDs was measured to be $0.66^{+0.08}_{-0.07}$. This was significantly less than the expected 12.6 NC neutrino interactions per day. In the third phase, two independent data streams existed: PMT and NCD. A Monte Carlo study was undertaken to determine whether an accurate measure of the NC flux could be obtained using only PMT data. Results showed that no improvement could be made upon results from previous phases and the best measurement of the NC flux in the final phase would be made using PMT and NCD data.

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17

Heeger, Karsten Miklas. "Model-independent measurement of the neutral-current interaction rate of solar ⁸B neutrinos with deuterium in the Sudbury Neutrino Observatory /." Thesis, Connect to this title online; UW restricted, 2002. http://hdl.handle.net/1773/9774.

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18

Cox-Mobrand, Gary A. "Data integrity and electronic calibrations for the neutral current detector phase measurement of the 8B solar neutrino flux at the Sudbury Neutrino Observatory /." Thesis, Connect to this title online; UW restricted, 2008. http://hdl.handle.net/1773/9647.

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19

Wiebe, Klaus [Verfasser]. "All-flavor based searches for solar dark matter with the IceCube Neutrino Observatory / Klaus Wiebe." Mainz : Universitätsbibliothek Mainz, 2017. http://d-nb.info/1124030700/34.

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20

Dalnoki-Veress, Ferenc J. R. Carleton University Dissertation Physics. "Investigation of the triggered source technique for the calibration of SNO." Ottawa, 1996.

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21

Dragowsky, Michael Raymond. "Sudbury Neutrino Observatory energy calibration using gamma-ray sources." Thesis, 1999. http://hdl.handle.net/1957/33088.

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22

Howard, Christopher William. "A search for hep neutrinos with the Sudbury Neutrino Observatory." Phd thesis, 2010. http://hdl.handle.net/10048/1284.

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This thesis focuses on the search for neutrinos from the solar hep reaction using the combined three phases of the Sudbury Neutrino Observatory (SNO) data. The data were taken over the years 19992006, totalling 1,083 days of live neutrino time. The previous published SNO hep neutrino search was completed in 2001 and only included the first phase of data taking. That hep search used an event counting approach in one energy bin with no energy spectral information included. This thesis will use a spectral analysis approach. The hep neutrino search will be a Bayesian analysis using Markov Chain Monte Carlo (MCMC), and a Metropolis-Hastings algorithm to sample the likelihood space. The method allows us to determine the best fit values for the parameters. This signal extraction will measure the 8B flux, the atmospheric neutrino background rate in the SNO detector, and the hep flux. This thesis describes the tests used to verify the MCMC algorithm and signal extraction. It defines the systematic uncertainties and how they were accounted for in the fit. It also shows the correlations between all of the parameters and the effect of each systematic uncertainty on the result. The three phase hep signal extraction was completed using only 1/3 of the full data set. With these lowered statistics, this analysis was able to place an upper limit on the hep flux of 4.2 10^4 cm2 s1 with a 90% confidence limit. It was able to measure a hep flux of (2.40(+1.19)(-1.60))10^4 cm2 s1. These numbers can be compared with the previous SNO upper limit of 2.310^4 cm2 s1 with a 90% confidence limit, and the standard solar model prediction of (7.970 1.236) 10^3 cm2 s1.

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23

Kos, Mark Szymon. "Low energy solar neutrino analysis of the salt phase of the Sudbury neutrino observatory." Thesis, 2007. http://hdl.handle.net/1974/959.

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The neutrino fluxes from the neutral current (NC), charged current (CC), and elastic scattering (ES) neutrino interactions in the salt phase of SNO have been extracted. The signals were extracted above an energy threshold of 4MeV, which is the lowest energy threshold at which the neutrino signals have been extracted from SNO to date. To achieve this low energy threshold the internal and external radioactive background signals have also been measured. The $^{8}$B neutrino fluxes for the 4MeV threshold were found to be \begin{eqnarray*} \Phi_{CC} & = & 1.60 ~^{+0.04}_{-0.04}~(\mbox{stat}) ~^{+0.06}_{-0.06}~(\mbox{syst}) \times 10^6 \mbox{cm}^{-2} \mbox{sec}^{-1},\\ \Phi_{NC} & = & 4.84 ~^{+0.16}_{-0.16}~(\mbox{stat}) ~^{+0.29}_{-0.32}~(\mbox{syst}) \times 10^6 \mbox{cm}^{-2} \mbox{sec}^{-1},\\ \Phi_{ES} & = & 2.75 ~^{+0.23}_{-0.23}~(\mbox{stat}) ~^{+0.25}_{-0.26}~(\mbox{syst}) \times 10^6 \mbox{cm}^{-2} \mbox{sec}^{-1}. \end{eqnarray*} \noindent These results are in agreement with the values published in ~\cite{SNO3} and the NC flux is in agreement with the standard solar model calculation from ~\cite{bp2004}. The published fluxes were \begin{eqnarray*} \Phi_{CC} &= & 1.68 ~^{+0.06}_{-0.06}~(\mbox{stat}) ~^{+0.08}_{-0.09}~(\mbox{syst}) \times 10^6 \mbox{cm}^{-2} \mbox{sec}^{-1} , \\ \Phi_{NC} &= & 4.94 ~^{+0.21}_{-0.21}~(\mbox{stat}) ~^{+0.38}_{-0.34}~(\mbox{syst}) \times 10^6 \mbox{cm}^{-2} \mbox{sec}^{-1}, \\ \Phi_{ES} &= & 2.35 ~^{+0.22}_{-0.22}~(\mbox{stat}) ~^{+0.15}_{-0.15}~(\mbox{syst}) \times 10^6 \mbox{cm}^{-2} \mbox{sec}^{-1}. \end{eqnarray*} \noindent The uncertainties on the extracted NC and CC fluxes are significantly smaller than on the published values. A comparison of the total uncertainty from flux measurements presented here and those published are given below. \begin{table}[htp] \begin{center} \begin{tabular}{|c|c|c|} \hline & uncertainties presented here (\%) & uncertainties from ~\cite{SNO3} (\%) \\ \hline $\Phi_{CC}$ & $~^{+4.6}_{-4.4}$ & $~^{+5.9}_{-6.4}$ \\ \hline $\Phi_{NC}$ & $~^{+6.8}_{-7.4}$ & $~^{+8.9}_{-8.2}$ \\ \hline $\Phi_{ES}$ & $~^{+12.3}_{-12.6}$ & $~^{+11.3}_{-11.3}$ \\ \hline \end{tabular} \label{funcert1} \end{center} \end{table} The shape of the CC energy spectrum has also been extracted with the 4MeV energy threshold. The uncertainties on the extracted fluxes are smaller than what was previously published. The CC spectrum gives a measure of the neutrino energy shape distortion due to neutrino oscillations. The uncertainties on the lowest energy bins in the extracted CC spectrum are much larger than the predicted distortion. We are therefore not sensitive to the upturn in the neutrino survival probability at lower energies predicted by neutrino oscillations in the large mixing angle (LMA) region.
Thesis (Ph.D, Physics, Engineering Physics and Astronomy) -- Queen's University, 2007-12-19 13:58:16.601

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24

Seibert, Stanley Reid. "A low energy measurement of the ⁸B solar neutrino spectrum at the Sudbury Neutrino Observatory." 2008. http://hdl.handle.net/2152/17755.

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The Sudbury Neutrino Observatory has previously shown that ⁸B solar neutrinos undergo flavor transformation between the Sun and the Earth. This work presents a joint analysis of one-third of the pure D₂O and salt phase data sets with an electron energy threshold of 3.5 MeV. A measurement of the neutral current interaction rate, sensitive to all neutrino flavors, gives a total ⁸B flux of 4.79 ± 0.22 (stat) ± 0.13(syst) × 10⁶ cm⁻²s⁻¹. This is in agreement with the prediction of the Standard Solar Model. For the first time we obtain the v[sunscript e] survival probability separately for downward-going (day) and upward-going (night) solar neutrinos. No significant distortion is observed day or night for ⁸B neutrinos with energies greater than 6 MeV. The lack of distortion, but overall suppression of electron neutrinos relative to the total flux, is consistent with matter-induced neutrino transformation in the Sun and the large mixing angle solution.
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25

MacLellan, Ryan. "The energy calibration for the solar neutrino analysis of all three phases of the Sudbury Neutrino Observatory." Thesis, 2009. http://hdl.handle.net/1974/5207.

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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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26

Martin, RYAN. "An Analysis of the 3-He Proportional Counter Data from the Sudbury Neutrino Observatory Using Pulse Shape Discrimination." Thesis, 2009. http://hdl.handle.net/1974/5177.

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This thesis presents an independent analysis of the data from 3-He-filled proportional counters from the third phase of the Sudbury Neutrino Observatory (SNO) data. These counters were deployed in SNO's heavy water to independently detect neutrons produced by the neutral current interaction of 8-B solar neutrinos with deuterium. Previously published results from this phase were based on a spectral analysis of the energy deposited in the proportional counters. The work in this thesis introduces a new observable based on the time-profile of the ionization in the counters. The inclusion of this observable in a maximum-likelihood fit increases the potential to distinguish neutrons from backgrounds which are primarily due to alpha-decays. The combination of this new observable with the energy deposited in the counters results in a more accurate determination of the number of neutrons. The analysis presented in this thesis was limited to one third of the data from the proportional counters, uniformly distributed in time. This limitation was imposed to reconcile different time-lines between the submission of this thesis, a thorough review of this work by the SNO Collaboration and results from an independent analysis that is still underway. Analysis of this reduced data set determined that 398 +/- 29 (stat.) +/- 9 (sys.) neutrons were detected in this reduced data-set. The number compares well to the previous analysis of the data, based only on a spectral analysis of the deposited energy, which determined that 410 +/- 44 (stat.) +/- 9 (sys.) were detected in the same time period. The analysis presented here has led to a substantial increase in the statistical accuracy. Assuming that the statistical accuracy will increase when the full data set is analyzed, the results from this thesis would bring the uncertainty in the 8-B solar neutrino flux to down 6.8% from 8.5% in the previously published results. The work from the thesis is intended to be included in a future analysis of the SNO data and will result in a more accurate measurement of the total flux of solar neutrinos from 8-B as well as reduce the uncertainty in the $\theta_{12}$ neutrino oscillation mixing angle.
Thesis (Ph.D, Physics, Engineering Physics and Astronomy) -- Queen's University, 2009-09-16 15:56:28.195

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