Search for Neutrinos from the Sun Using the Reaction 71Ga(v e ,e –)71 Ge

Abazov, A. I.; Anosov, O. L.; Faizov, E. L.; Gavrin, V. N.; Kalikhov, A. V.; Knodel, T. V.; Knyshenko, I.I.; Корноухов, В. Н.; Mezentseva, S. A.; Mirmov, I. N.; Ostrinsky, A. V.; Pshukov, A. M.; Revzin, N. E.; Shikhin, A. A.; Timofeyev, P. V.; Veretenkin, E. P.; Vermul, V. M.; Zalscpin, G. T.; Bowles, T. J.; Cleveland, B. T.; Elliott, S. R.; O’Brien, H. A.; Wark, D. L.; Wilkerson, Jessica; Davis, R.; Lande, K.; Cherry, M. L.; Kouzes, R. T.

doi:10.1201/9780429502811-49

Cited by 13 publications

(51 citation statements)

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“…In 1989, the Kamiokande-II experiment confirmed the deficit of 8 B solar electron neutrinos relative to the standard solar model [13]. In 1991 and 1992, the deficit was further confirmed by two experiments, SAGE [14] and GALLEX [10], which both measured the rate of the less energetic pp solar neutrinos. These experiments showed that the flux deficit Either the standard solar model was incorrect or electron neutrinos produced in the sun do not all survive the journey to the Earth.…”

Section: Neutrino Physicsmentioning

confidence: 91%

Measurement of Muon Neutrino Disappearance with the NOvA Experiment

Vinton

2018

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The NOvA experiment consists of two functionally identical tracking calorimeter detectors which measure the neutrino energy and flavour composition of the NuMI beam at baselines of 1 km and 810 km. Measurements of neutrino oscillation parameters are extracted by comparing the neutrino energy spectrum in the far detector with predictions of the oscillated neutrino energy spectra that are made using information extracted from the near detector. Observation of muon neutrino disappearance allows NOvA to make measurements of the mass squared splitting ∆m 2 32 and the mixing angle θ 23. The measurement of θ 23 will provide insight into the make-up of the third mass eigenstate and probe the muon-tau symmetry hypothesis that requires θ 23 = π/4. This thesis introduces three methods to improve the sensitivity of NOvA's muon neutrino disappearance analysis. First, neutrino events are separated according to an estimate of their energy resolution to distinguish well resolved events from events that are not so well resolved. Second, an optimised neutrino energy binning is implemented that uses finer binning in the region of maximum muon neutrino disappearance. Third, a hybrid selection is introduced that selects muon neutrino events with greater efficiency and purity. The combination of these improvements produces an increase in the sensitivity of the analysis equivalent to collecting 40-100% more data across the range of possible values of ∆m 2 32 and sin 2 θ 23. iv This thesis presents new results using a 14 ktonne detector equivalent exposure of 6.05 × 10 20 protons on target. A fit to the far detector data, assuming normal hierarchy, produces ∆m 2 32 = 2.45 +0.087 −0.079 × 10 −3 eV 2 and sin 2 θ 23 in the range 0.429-0.593 with two statistically degenerate best fit points at 0.481 and 0.547. This measurement is consistent with maximal mixing where θ 23 = π/4. The data used for this thesis is 1/6 of the total data that NOvA expects to collect. v Acknowledgements I would like to thank my viva examiners, Dr Iacopo Vivarelli and Dr Evgueni Goudzovski, for both the time they took to read my thesis and the invaluable feedback they provided. I feel immense gratitude to my supervisor, Professor Jeff Hartnell, for giving me the opportunity to pursue my fascination in neutrino physics. Over the years our discussions have given me new insights and increased my appreciation for the need of precision. This piece of work would not have been possible without the amazing members of the NOvA collaboration. The members of this collaboration built both the detectors and the fantastic software frameworks used for everything from data collection through to data analysis. The NOvA post-doctoral researchers at Sussex had to bear the brunt of my many questions and frustrations. I would like to thank Bruno Zamorano, Michael Baird, Jonathon Davies and Matthew Tamsett who all provided unique advice and taught me a lot. I've enjoyed my time in both of the offices I've shared during my time as a student at Sussex. That is thanks to my fellow students...

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Section: Neutrino Physicsmentioning

confidence: 91%

Measurement of Muon Neutrino Disappearance with the NOvA Experiment

Vinton

2018

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“…I begin by motivating these measurements through a description of neutrinos and the phenomenon of oscillations in Chapter 2 and introducing the challenges regarding neutrino interactions and detection in Chapter 3. In Chapter 4, I describe the NOvA experiment, detailing some of my contributions to commissioning, maintenance, and detector operations and monitoring in Secs. 4.2.2, 4. 2.3, and 4.2.…”

Section: Dissertation Overviewmentioning

confidence: 98%

“…Neutrino physicists have performed oscillation measurements using neutrinos from a variety of natural sources. Solar electron neutrinos, which brought the solar neutrino problem to light, have also been studied by experiments like Kamiokande [3], SAGE [4], Gallex [5], and SNO [6]. Atmospheric muon and electron neutrinos, which are produced by cosmic rays in the Earth's atmosphere, fueled the first observations of neutrino oscillations by the Super-Kamiokande [7] experiment in 1998 and 1 While it is actually not the case that every single channel needs to be observed in order to understand as much as we can about neutrino oscillations, a large subset of them does need to be probed by experiments to complete the picture of probabilities for each single flavor to oscillate into another.…”

Section: -Albert Einsteinmentioning

confidence: 99%

Measurement of Long Baseline Neutrino Oscillations and Improvements from Deep Learning

Psihas¹

2018

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Especially, I want to acknowledge Evan Niner for his support, his respect and also his patience, and to Michael Baird for his wisdom and example. Whatever stage of our careers Evan and Michael will continue to be my older brother examples to follow.Naturally, a special thanks should go to my closest CVN companions, Dominick Rocco who academia misses terribly, Alex Radovic my best arguing buddy, and Adam Aurisano who is just super nice.More recently, to Micah Groh, who has taken on so much in such a short time, thank you for allowing me to get you started and for all the fun that followed. And to Diana P. Mendez, Teresa Lackey, Ryan Murphy and Shiqi Yu for taking the many batons I had been running with on NOvA. Science is a passion from which half the fun is talking about. Thank you for listening.I was lucky to learn important lessons from many of my peers, for those lessons I thank Erika Catano-Mur, an unexpected companion at crunch time and an accomplice to always sneak in "just one more improvement", as well as my friends Kuldeep Kaur Maan, Biswaranjan Behera, and Liudmila Kolux paeva who are my examples of hard work and commitment and who make me always want to do better.I would also like to acknowledge people outside of NOvA who gave me advice, friendship, and opportunities for growth, such as Joseph Zennamo with whom I am delighted to talk about any physics, any day. To Sergei Gleyzer for introducing me to new perspectives to problems and the whole field, and especially my good friend Francesco Capozzi with whom I endured the longest, best hikes ever, and who in turn endured with me the proof-reading of my theory chapter.Lastly, a special acknowledgement to the people who have marked my PhD and my last few years, and potentially the few who have continued to read this far:To my friend, colleague and co-watchdog leader Louise Suter, whom I love not only for her friendship but for her example of brilliance and integrity.To Gavin Davies for being for me, like for NOvA, the string tying all loose ends together. Sometimes things seem to stand tall on their own, but there is always a support that keeps them from falling.To Justin Vasel, who is my family away from family, my brother and partner in adventure. Thank you for all the proof-reads, all the encouragement, and for always believing in me. I would not be where I am now if I didn't have you in my life.Thank you to Fermi National Accelerator Laboratory, a home away from home where I learned the true meaning and value of great American science.

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“…Two radio-chemical experiments using gallium as neutrino target, SAGE (Soviet-American Gallium Experiment) [2] and GALLEX (Gallium Experiment) [89] used the properties of gallium and become sensitive to the lower energy pp neutrinos by the reaction ν e + 71 Ga → 71 Ge + ν e and, again by looking at Fig. 1.3, to most of the solar neutrino flux spectrum.…”

Section: The Solar Neutrino Anomalymentioning

confidence: 99%

Measurement of the Kaon Production Normalization in the NuMI Target Using Uncontained Charged-Current Muon Neutrino Interactions in the NOvA Far Detector

Sepulveda-Quiroz

2018

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Search for Neutrinos from the Sun Using the Reaction 71Ga(v e ,e –)71 Ge

Cited by 13 publications

References 0 publications

Measurement of Muon Neutrino Disappearance with the NOvA Experiment

Measurement of Muon Neutrino Disappearance with the NOvA Experiment

Measurement of Long Baseline Neutrino Oscillations and Improvements from Deep Learning

Measurement of the Kaon Production Normalization in the NuMI Target Using Uncontained Charged-Current Muon Neutrino Interactions in the NOvA Far Detector

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