An array of low-background 3He proportional counters for the Sudbury Neutrino Observatory

Amsbaugh, J. F.; Anaya, Juan Manuel; Banar, J.; Bowles, T. J.; Browne, M. C.; Bullard, T. V.; Burritt, T. H.; Cox-Mobrand, G. A.; Dai, Xiongxin; Deng, Hui; Marco, M. Di; Doe, P. J.; Dragowsky, M. R.; Duba, C. A.; Duncan, F. A.; Earle, E.D.; Elliott, S. R.; Esch, Ernst I; Fergani, H.; Formaggio, J. A.; Fowler, Μ. M.; Franklin, J.E.; Geissbühler, P.; Germani, J. V.; Goldschmidt, A.; Guillian, E.; Hallin, A. L.; Harper, G.; Harvey, P. J.; Hazama, R.; Heeger, K. M.; Heise, J.; Hime, A.; Howe, M. A.; Huang, M.; Kormos, L. L.; Kraus, C.; Krauss, C. B.; Law, J.; Lawson, I.; Lesko, K. T.; Loach, J. C.; Majerus, Steve; Manor, J.; McGee, Steven; Miknaitis, Kathryn; Miller, Guthrie; Morissette, B.; Myers, A.W.; Oblath, N. S.; O’Keeffe, H. M.; Ollerhead, R. W.; Peeters, S. J. M.; Poon, A. W. P.; Prior, G.; Reitzner, S. D.; Rielage, K.; Robertson, R. G. H.; Skensved, P.; Smith, Alan Р.; Smith, M. W. E.; Steiger, Thomas; Stonehill, L. C.; Thornewell, P. M.; Tolich, N.; VanDevender, B. A.; Wechel, T. D. Van; Wall, B. L.; Tseung, H. Wan Chan; Wendland, J.; West, N.; Wilhelmy, J.B.; Wilkerson, J. F.; Wouters, J.M.

doi:10.1016/j.nima.2007.05.321

Cited by 59 publications

(63 citation statements)

References 22 publications

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“…This enhanced the neutron detection efficiency and the ability to statistically separate the NC and CC signals, and resulted in significant improvement in the accuracy of the measured ν e and ν x fluxes without any assumption about the energy dependence of the neutrino flavor transformation [6,7]. In the present measurement, the NC signal neutrons were predominantly detected by an array of 3 He proportional counters (Neutral Current Detection, or NCD, array [8]) consisting of 36 "strings" of counters that were deployed in the D 2 O. Four additional strings filled with 4 He were insensitive to the neutron signals and were used to study backgrounds.…”

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confidence: 98%

“…The Sudbury Neutrino Observatory (SNO) used an array of 3 He proportional counters to measure the rate of neutral-current interactions in heavy water and precisely determined the total active (ν x ) 8 B solar neutrino flux. This technique is independent of previous methods employed by SNO The Sudbury Neutrino Observatory [1] detects 8 B solar neutrinos through three reactions: charged-current interactions (CC) on deuterons, in which only electron neutrinos participate; neutrino-electron elastic scattering (ES), which are dominated by contributions from electron neutrinos; and neutral-current (NC) disintegration of the deuteron by neutri-nos, which has equal sensitivity to all active neutrino flavors.…”

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confidence: 99%

“…In its first phase of operation, SNO measured the NC rate by observing neutron captures on deuterons and found that a Standard-Electro-Weak-Model description with an undistorted 8 B neutrino spectrum and CC, NC, and ES rates due solely to ν e interactions was rejected at 5.3σ [2,3,4,5]. The second phase of SNO measured the rates and spectra after the addition of ∼2000 kg of NaCl to the 10 6 kg of heavy water (D 2 O).…”

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confidence: 99%

“…The number of raw NCD triggers was 1,417,811 and the data set was reduced to 91,636 NCD events after data reduction described in [8]. Six strings filled with 3 He were excluded from the analysis due to various defects.…”

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confidence: 99%

“…Because of particles hitting the counter walls [8], the detected ionization energy was between 191 and 764 keV. The signals from each string were amplified logarithmically to provide sufficient dynamic range before they were digitized [8].…”

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confidence: 99%

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Independent Measurement of the Total ActiveB8Solar Neutrino Flux Using an Array ofHe3Proportional Counters at th

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The Sudbury Neutrino Observatory (SNO) used an array of 3 He proportional counters to measure the rate of neutral-current interactions in heavy water and precisely determined the total active (ν x ) 8 B solar neutrino flux. This technique is independent of previous methods employed by SNO The Sudbury Neutrino Observatory [1] detects 8 B solar neutrinos through three reactions: charged-current interactions (CC) on deuterons, in which only electron neutrinos participate; neutrino-electron elastic scattering (ES), which are dominated by contributions from electron neutrinos; and neutral-current (NC) disintegration of the deuteron by neutri-

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confidence: 98%

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confidence: 99%

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confidence: 99%

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confidence: 99%

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confidence: 99%

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Independent Measurement of the Total ActiveB8Solar Neutrino Flux Using an Array ofHe3Proportional Counters at th

Aharmim¹,

Ahmed²,

Amsbaugh³

et al. 2008

Phys. Rev. Lett.

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287

180

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The Sudbury Neutrino Observatory: Observation of flavor change for solar neutrinos

McDonald

2016

Annalen der Physik

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The Sudbury Neutrino Observatory (SNO) experiment was constructed by an international scientific collaboration primarily to provide a clear determination of whether solar neutrinos change their flavor in transit from the core of the sun to the earth. The detector used 1000 tonnes of heavy water (>99.92% D2O) in an ultra-clean location 2 km underground in INCO's Creighton mine near Sudbury, Canada to observe two separate reactions of neutrinos on deuterium. The first reaction was sensitive only to electron flavor neutrinos and the second reaction was equally sensitive to all neutrino flavors. The measurements by SNO showed clearly that the hypothesis of no neutrino flavor change was ruled out by more than 5.3 standard deviations. The observation of flavor change for neutrinos implies that they have a non-zero mass. The measured total flux of active neutrinos from 8 B decay in the sun was found to be in excellent agreement with the predictions of solar model calculations. This paper describes the history and scientific measurements of the SNO experiment.*** Solar neutrinosThe nuclear fusion processes that power the sun take place at such high temperatures that the nuclei of atoms are able to fuse together, a process that results in the creation of very large numbers of fundamental particles called neutrinos. As you heard from my friend and scientific colleague Professor Kajita, neutrinos only interact through the weak interaction and gravity and therefore can penetrate out from the core of the sun and through the earth with little or no interaction. It is these neutrinos from the sun that are the subject of our measurements with the Sudbury Neutrino Observatory (SNO), 2 km underground in a mine near Sudbury, Canada. With the use of heavy water as a central element in the design of SNO it was possible to determine clearly that electron neutrinos change to one of the other active flavors before reaching our detector, a property that requires that they have a mass greater than zero. Both of these fundamental neutrino properties are beyond the predictions of the Standard Model for Elementary Particles. Extensions of the Standard Model to include these neutrino properties can give us a more complete understanding of our Universe at a very basic level.The study of the sun and the processes that power it has been the subject of strong interest for many years and it is clear that in our work we "see farther because we stand on the shoulders of giants" as was said by Isaac Newton. Nobel Laureates Hans Bethe (1967) and Willy Fowler (1983) were pioneers in the study of the physics of nuclear reactions in the sun: Bethe for his work on energy production in stars via nuclear reactions and Fowler for working out the details of the pp reactions and others that are responsible for the creation of the majority of the elements in stars and supernovae. The general conclusion of their work was that the "pp cycle" shown in Figure 1 was the principal source of energy generation in the sun.I was fortunate to be a graduate student in F...

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Introduction and Theoretical Background

Dunger¹

2019

Springer Theses

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An array of low-background 3He proportional counters for the Sudbury Neutrino Observatory

Cited by 59 publications

References 22 publications

Independent Measurement of the Total ActiveB8Solar Neutrino Flux Using an Array ofHe3Proportional Counters at th

Independent Measurement of the Total ActiveB8Solar Neutrino Flux Using an Array ofHe3Proportional Counters at th

The Sudbury Neutrino Observatory: Observation of flavor change for solar neutrinos

Introduction and Theoretical Background

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