DOCSLIB.ORG

Daya at Antineutrinos Reactor Eebr1 2006 1, December Proposal Aabay Daya Θ 13 Using Daya Bay Collaboration

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Daya at Antineutrinos Reactor Eebr1 2006 1, December Proposal Aabay Daya Θ 13 Using Daya Bay Collaboration Daya Bay Proposal December 1, 2006 A Precision Measurement of the Neutrino Mixing Angle θ13 Using Reactor Antineutrinos At Daya Bay arXiv:hep-ex/0701029v1 15 Jan 2007 Daya Bay Collaboration Beijing Normal University Xinheng Guo, Naiyan Wang, Rong Wang Brookhaven National Laboratory Mary Bishai, Milind Diwan, Jim Frank, Richard L. Hahn, Kelvin Li, Laurence Littenberg, David Jaffe, Steve Kettell, Nathaniel Tagg, Brett Viren, Yuping Williamson, Minfang Yeh California Institute of Technology Christopher Jillings, Jianglai Liu, Christopher Mauger, Robert McKeown Charles Unviersity Zdenek Dolezal, Rupert Leitner, Viktor Pec, Vit Vorobel Chengdu University of Technology Liangquan Ge, Haijing Jiang, Wanchang Lai, Yanchang Lin China Institute of Atomic Energy Long Hou, Xichao Ruan, Zhaohui Wang, Biao Xin, Zuying Zhou Chinese University of Hong Kong, Ming-Chung Chu, Joseph Hor, Kin Keung Kwan, Antony Luk Illinois Institute of Technology Christopher White Institute of High Energy Physics Jun Cao, Hesheng Chen, Mingjun Chen, Jinyu Fu, Mengyun Guan, Jin Li, Xiaonan Li, Jinchang Liu, Haoqi Lu, Yusheng Lu, Xinhua Ma, Yuqian Ma, Xiangchen Meng, Huayi Sheng, Yaxuan Sun, Ruiguang Wang, Yifang Wang, Zheng Wang, Zhimin Wang, Liangjian Wen, Zhizhong Xing, Changgen Yang, Zhiguo Yao, Liang Zhan, Jiawen Zhang, Zhiyong Zhang, Yubing Zhao, Weili Zhong, Kejun Zhu, Honglin Zhuang Iowa State University Kerry Whisnant, Bing-Lin Young Joint Institute for Nuclear Research Yuri A. Gornushkin, Dmitri Naumov, Igor Nemchenok, Alexander Olshevski Kurchatov Institute Vladimir N. Vyrodov Lawrence Berkeley National Laboratory and University of California at Berkeley Bill Edwards, Kelly Jordan, Dawei Liu, Kam-Biu Luk, Craig Tull Nanjing University Shenjian Chen, Tingyang Chen, Guobin Gong, Ming Qi Nankai University Shengpeng Jiang, Xuqian Li, Ye Xu National Chiao-Tung University Feng-Shiuh Lee, Guey-Lin Lin, Yung-Shun Yeh National Taiwan University Yee B. Hsiung National United University Chung-Hsiang Wang Princeton University Changguo Lu, Kirk T. McDonald Rensselaer Polytechnic Institute John Cummings, Johnny Goett, Jim Napolitano, Paul Stoler Shenzhen Univeristy Yu Chen, Hanben Niu, Lihong Niu Sun Yat-Sen (Zhongshan) University Zhibing Li Tsinghua University Shaomin Chen, Hui Gong, Guanghua Gong, Li Liang, Beibei Shao, Qiong Su, Tao Xue, Ming Zhong University of California at Los Angeles Vahe Ghazikhanian, Huan Z. Huang, Charles A. Whitten, Stephan Trentalange University of Hong Kong, K.S. Cheng, Talent T.N. Kwok, Maggie K.P. Lee, John K.C. Leung, Jason C.S. Pun, Raymond H.M. Tsang, Heymans H.C. Wong University of Houston Michael Ispiryan, Kwong Lau, Logan Lebanowski, Bill Mayes, Lawrence Pinsky, Guanghua Xu University of Illinois at Urbana-Champaign S. Ryland Ely, Wah-Kai Ngai, Jen-Chieh Peng University of Science and Technology of China Qi An, Yi Jiang, Hao Liang, Shubin Liu, Wengan Ma, Xiaolian Wang, Jian Wu, Ziping Zhang, Yongzhao Zhou University of Wisconsin A. Baha Balantekin, Karsten M. Heeger, Thomas S. Wise Virginia Polytechnic Institute and State University Jonathan Link, Leo Piilonen Preprint numbers: BNL-77369-2006-IR LBNL-62137 TUHEP-EX-06-003 I Executive Summary This document describes the design of the Daya Bay reactor neutrino experiment. Recent discoveries in neutrino physics have shown that the Standard Model of particle physics is incomplete. The observation of neutrino oscillations has unequivocally demonstrated that the masses of neutrinos are nonzero. The small- ness of the neutrino masses (<2 eV) and the two surprisingly large mixing angles measured have thus far provided important clues and constraints to extensions of the Standard Model. The third mixing angle, θ13, is small and has not yet been determined; the current experimental bound 2 2 −3 2 is sin 2θ13 < 0.17 at 90% confidence level (from Chooz) for ∆m31 = 2.5 10 eV . It is important to measure this angle to provide further insight on how to extend the Standard Model.× A precision measurement 2 of sin 2θ13 using nuclear reactors has been recommended by the 2004 APS Multi-divisional Study on the Future of Neutrino Physics as well as a recent Neutrino Scientific Assessment Group (NuSAG) report. We propose to perform a precision measurement of this mixing angle by searching for the disappearance of electron antineutrinos from the nuclear reactor complex in Daya Bay, China. A reactor-based determi- 2 nation of sin 2θ13 will be vital in resolving the neutrino-mass hierarchy and future measurements of CP violation in the lepton sector because this technique cleanly separates θ13 from CP violation and effects of 2 neutrino propagation in the earth. A reactor-based determination of sin 2θ13 will provide important, com- plementary information to that from long-baseline, accelerator-based experiments. The goal of the Daya 2 Bay experiment is to reach a sensitivity of 0.01 or better in sin 2θ13 at 90% confidence level. The Daya Bay Experiment The Day Bay nuclear power complex is one of the most prolific sources of antineutrinos in the world. Currently with two pairs of reactor cores (Daya Bay and Ling Ao), separated by about 1.1 km, the complex generates 11.6 GW of thermal power; this will increase to 17.4 GW by early 2011 when a third pair of reactor cores (Ling Ao II) is put into operation and Daya Bay will be among the five most powerful reactor complexes in the world. The site is located adjacent to mountainous terrain, ideal for siting underground detector laboratories that are well shielded from cosmogenic backgrounds. This site offers an exceptional 2 opportunity for a reactor neutrino experiment optimized to perform a precision determination of sin 2θ13 through a measurement of the relative rates and energy spectrum of reactor antineutrinos at different base- lines. In addition, this project offers a unique and unprecedented opportunity for scientific collaboration involving China, the U.S., and other countries. The basic experimental layout of Daya Bay consists of three underground experimental halls, one far and two near, linked by horizontal tunnels. Figure 0.1 shows the detector module deployment at these sites. Eight identical cylindrical detectors, each consisting of three nested cylindrical zones contained within a stainless steel tank, will be deployed to detect antineutrinos via the inverse beta-decay reaction. To maxi- mize the experimental sensitivity four detectors are deployed in the far hall at the first oscillation maximum. The rate and energy distribution of the antineutrinos from the reactors are monitored with two detectors in each near hall at relatively short baselines from their respective reactor cores, reducing the systematic 2 uncertainty in sin 2θ13 due to uncertainties in the reactor power levels to about 0.1%. This configuration significantly improves the statistical precision over previous experiments (0.2% in three years of running) and enables cross-calibration to verify that the detectors are identical. Each detector will have 20 metric tons of 0.1% Gd-doped liquid scintillator in the inner-most, antineutrino target zone. A second zone, separated from the target and outer buffer zones by transparent acrylic vessels, will be filled with undoped liquid scin- tillator for capturing gamma rays that escape from the target thereby improving the antineutrino detection efficiency. A total of 224 photomultiplier tubes are arranged along the circumference of the stainless steel tank in the outer-most zone, which contains mineral oil to attenuate gamma rays from trace radioactivity in the photomultiplier tube glass and nearby materials including the outer tank. The detector dimensions are II Fig. 0.1. Default configuration of the Daya Bay experiment, optimized for best sensi- 2 tivity in sin 2θ13. Four detector modules are deployed at the far site and two each at each of the near sites. summarized in Table 0.1. Dimensions Inner Acrylic Outer Acrylic Stainless Steel Diameter (mm) 3200 4100 5000 Height (mm) 3200 4100 5000 Wall thickness (mm) 10 15 10 Vessel Weight (ton) 0.6 1.4 20 Liquid Weight (ton) 20 20 40 ∼ ∼ ∼ Table 0.1. Summary of antineutrino detector properties. The liquid weights are for the mass of liquid contained only within that zone. With reflective surfaces at the top and bottom of the detector the energy resolution of the detector is about 12% at 1 MeV. The mountainous terrain provides sufficient overburden to suppress cosmic muon induced backgrounds to less than 1% of the antineutrino signal. The detectors in each experimental hall are shielded by 2.5 m of water from radioactivity and spallation neutrons in the surrounding rock. The detector halls include a muon detector system, consisting of a tracker on top of the water pool and water Cherenkov counters in the water shield, for tagging the residual cosmic muons. With this experimental setup, the signal and background rates at the Daya Bay near hall, Ling Ao near III hall and the far hall are summarized in Table 0.2. Daya Bay Near Ling Ao Near Far Hall Baseline (m) 363 481 from Ling Ao 1985 from Daya Bay 526 from Ling Ao II 1615 from Ling Ao’s Overburden (m) 98 112 350 Radioactivity (Hz) <50 <50 <50 Muon rate (Hz) 36 22 1.2 Antineutrino Signal (events/day) 930 760 90 Accidental Background/Signal (%) <0.2 <0.2 <0.1 Fast neutron Background/Signal (%) 0.1 0.1 0.1 8He+9Li Background/Signal (%) 0.3 0.2 0.2 Table 0.2. Summary of signal and background rates for each detector module at the different experimental sites. Careful construction, filling, calibration and monitoring of the detectors will reduce detector-related systematic uncertainties to a level comparable to or below the statistical uncertainty. Table 0.3 is a summary of systematic uncertainties for the experiment. Source Uncertainty Reactor Power 0.087% (4 cores) 0.13% (6 cores) Detector (per module) 0.38% (baseline) 0.18% (goal) Signal Statistics 0.2% Table 0.3. Summary of uncertainties.
Load more

Recommended publications
  • A Measurement of the 2 Neutrino Double Beta Decay Rate of 130Te in the CUORICINO Experiment by Laura Katherine Kogler
    A measurement of the 2 neutrino double beta decay rate of 130Te in the CUORICINO experiment by Laura Katherine Kogler A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Physics in the Graduate Division of the University of California, Berkeley Committee in charge: Professor Stuart J. Freedman, Chair Professor Yury G. Kolomensky Professor Eric B. Norman Fall 2011 A measurement of the 2 neutrino double beta decay rate of 130Te in the CUORICINO experiment Copyright 2011 by Laura Katherine Kogler 1 Abstract A measurement of the 2 neutrino double beta decay rate of 130Te in the CUORICINO experiment by Laura Katherine Kogler Doctor of Philosophy in Physics University of California, Berkeley Professor Stuart J. Freedman, Chair CUORICINO was a cryogenic bolometer experiment designed to search for neutrinoless double beta decay and other rare processes, including double beta decay with two neutrinos (2νββ). The experiment was located at Laboratori Nazionali del Gran Sasso and ran for a period of about 5 years, from 2003 to 2008. The detector consisted of an array of 62 TeO2 crystals arranged in a tower and operated at a temperature of ∼10 mK. Events depositing energy in the detectors, such as radioactive decays or impinging particles, produced thermal pulses in the crystals which were read out using sensitive thermistors. The experiment included 4 enriched crystals, 2 enriched with 130Te and 2 with 128Te, in order to aid in the measurement of the 2νββ rate. The enriched crystals contained a total of ∼350 g 130Te. The 128-enriched (130-depleted) crystals were used as background monitors, so that the shared backgrounds could be subtracted from the energy spectrum of the 130- enriched crystals.
    [Show full text]
  • Full TIPP 2011 Program Book
    Second International Conference on Technology and Instrumentation in Particle Physics June 9-14, 2011 Program & Abstracts Sheraton Chicago Hotel and Towers, Chicago IL ii TIPP 2011 — June 9-14, 2011 Table of Contents Acknowledgements .................................................................................................................................... v Session Conveners ...................................................................................................................................vii Session Chairs .......................................................................................................................................... ix Agenda ....................................................................................................................................................... 1 Abstracts .................................................................................................................................................. 35 Poster Abstracts ..................................................................................................................................... 197 Abstract Index ........................................................................................................................................ 231 Poster Index ........................................................................................................................................... 247 Author List .............................................................................................................................................
    [Show full text]
  • Pos(ICRC2017)1010 ∗ † G
    Search for GeV neutrinos associated with solar flares with IceCube PoS(ICRC2017)1010 The IceCube Collaboration† † http://icecube.wisc.edu/collaboration/authors/icrc17_icecube E-mail: [email protected] Since the end of the eighties and in response to a reported increase in the total neutrino flux in the Homestake experiment in coincidence with solar flares, solar neutrino detectors have searched for solar flare signals. Hadronic acceleration in the magnetic structures of such flares leads to meson production in the solar atmosphere. These mesons subsequently decay, resulting in gamma-rays and neutrinos of O(MeV-GeV) energies. The study of such neutrinos, combined with existing gamma-ray observations, would provide a novel window to the underlying physics of the acceleration process. The IceCube Neutrino Observatory may be sensitive to solar flare neutrinos and therefore provides a possibility to measure the signal or establish more stringent upper limits on the solar flare neutrino flux. We present an original search dedicated to low energy neutrinos coming from transient events. Combining a time profile analysis and an optimized selection of solar flare events, this research represents a new approach allowing to strongly lower the energy threshold of IceCube, which is initially foreseen to detect TeV neutrinos. Corresponding author: G. de Wasseige∗ IIHE-VUB, Pleinlaan 2, 1050 Brussels, Belgium 35th International Cosmic Ray Conference 10-20 July, 2017 Bexco, Busan, Korea ∗Speaker. c Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). http://pos.sissa.it/ Search for GeV neutrinos associated with solar flares with IceCube G.
    [Show full text]
  • Solar Neutrino Spectroscopy
    Solar Neutrino Spectroscopy Michael Wurm∗ PRISMA Cluster of Excellence and Institute of Physics, Johannes Gutenberg University, 55099 Mainz, Germany April 24, 2017 Abstract More than forty years after the first detection of neutrinos from the Sun, the spectroscopy of solar neutrinos has proven to be an on-going success story. The long-standing puzzle about the observed solar neutrino deficit has been resolved by the discovery of neutrino flavor oscillations. Today's experiments have been able to solidify the standard MSW-LMA oscillation scenario by performing precise measurements over the whole energy range of the solar neutrino spectrum. This article reviews the enabling experimental technologies: On the one hand mutli- kiloton-scale water Cherenkov detectors performing measurements in the high-energy regime of the spectrum, on the other end ultrapure liquid-scintillator detectors that allow for a low- threshold analysis. The current experimental results on the fluxes, spectra and time vari- ation of the different components of the solar neutrino spectrum will be presented, setting them in the context of both neutrino oscillation physics and the hydrogen fusion processes embedded in the Standard Solar Model. Finally, the physics potential of state-of-the-art detectors and a next-generation of ex- periments based on novel techniques will be assessed in the context of the most interesting open questions in solar neutrino physics: a precise measurement of the vacuum-matter transition curve of electron-neutrino oscillation probability that offers a definitive test of the basic MSW-LMA scenario or the appearance of new physics; and a first detection of neutrinos from the CNO cycle that will provide new information on solar metallicity and stellar physics.
    [Show full text]
  • Nov/Dec 2020
    CERNNovember/December 2020 cerncourier.com COURIERReporting on international high-energy physics WLCOMEE CERN Courier – digital edition ADVANCING Welcome to the digital edition of the November/December 2020 issue of CERN Courier. CAVITY Superconducting radio-frequency (SRF) cavities drive accelerators around the world, TECHNOLOGY transferring energy efficiently from high-power radio waves to beams of charged particles. Behind the march to higher SRF-cavity performance is the TESLA Technology Neutrinos for peace Collaboration (p35), which was established in 1990 to advance technology for a linear Feebly interacting particles electron–positron collider. Though the linear collider envisaged by TESLA is yet ALICE’s dark side to be built (p9), its cavity technology is already established at the European X-Ray Free-Electron Laser at DESY (a cavity string for which graces the cover of this edition) and is being applied at similar broad-user-base facilities in the US and China. Accelerator technology developed for fundamental physics also continues to impact the medical arena. Normal-conducting RF technology developed for the proposed Compact Linear Collider at CERN is now being applied to a first-of-a-kind “FLASH-therapy” facility that uses electrons to destroy deep-seated tumours (p7), while proton beams are being used for novel non-invasive treatments of cardiac arrhythmias (p49). Meanwhile, GANIL’s innovative new SPIRAL2 linac will advance a wide range of applications in nuclear physics (p39). Detector technology also continues to offer unpredictable benefits – a powerful example being the potential for detectors developed to search for sterile neutrinos to replace increasingly outmoded traditional approaches to nuclear nonproliferation (p30).
    [Show full text]
  • The Variation of the Solar Neutrino Fluxes Over Time in the Homestake, GALLEX(GNO) and Super-Kamiokande Experiments
    The Variation of the Solar Neutrino Fluxes over Time in the Homestake, GALLEX(GNO) and Super-Kamiokande Experiments K. Sakurai1,3, H. J. Haubold2 and T. Shirai1 1. Institute of Physics, Kanagawa University, Yokohama 221-8686, Japan 2. Office for Outer Space Affairs, United Nations, P. O. Box 500, A-1400, Vienna, Austria 3. Advanced Research Institute for Science and Engineering, Waseda University, Shinjuku, Tokyo 169-8555, Japan Abstract Using the records of the fluxes of solar neutrinos from the Homestake, GALLEX (GNO), and Super-Kamiokande experiments, their statistical analyses were performed to search for whether there existed a time variation of these fluxes. The results of the analysis for the three experiments indicate that these fluxes are varying quasi-biennially. This means that both efficiencies of the initial p-p and the PP-III reactions of the proton-proton chain are varying quasi-biennially together with a period of about 26 months. Since this time variation prospectively generated by these two reactions strongly suggests that the efficiency of the proton-proton chain as the main energy source of the Sun has a tendency to vary quasi-biennially due to some chaotic or non-linear process taking place inside the gravitationally stabilized solar fusion reactor. It should be, however, remarked that, at the present moment, we have no theoretical reasoning to resolve this mysterious result generally referred to as the quasi-biennial periodicity in the time variation of the fluxes of solar neutrinos. There is an urgent need to search for the reason why such a quasi-biennial periodicity is caused through some physical process as related to nuclear fusion deep inside the Sun.
    [Show full text]
  • Sudbury Neutrino Observatory Energy Calibration Using Gamma-Ray Sources By
    AN ABSTRACT OF THE DISSERTATION OF Michael Raymond Dragowsky for the degree of Doctor of Philosophy in Physics presented on 28 June 1999. Title: Sudbury Neutrino Observatory Energy Calibration using Gamma-Ray Sources. Redacted for privacy Abstract approved: _____ Kenneth S. Krane Redacted for privacy Eric B. Norman The long-standing Solar Neutrino Problem describes the disagreement between the observed and predicted solar neutrino flux. An extension to the electroweak model of particle physics predicts that neutrino flavor may change as a neutrino propagates from its source, and may account for the Solar Neutrino Problem. The Sudbury Neutrino Observatory will make two measurements of the 8B neutrino flux from the Sun. The first is independent of neutrino flavor, allowing for the first time a definitive measurement of the total 8B neutrino flux. The second measurement will be sensitive only to the 8B electron-neutrino flux. Comparison of these two measurements will allow a determination of whether the electron-neutrinos produced in the Sun change their flavor as they propagate to the Earth. Precise energy calibration is required to ensure accurate measurements. Two energy calibration sources will be described that rely on the coincident emission of a {3 particle and a 'Y-ray. The sources make use of 4 4 16N and 2 Na {3-decay. In addition to energy calibration, the 2 Na source provides an assessment of the rate of photodissociation of deuterium that is important in understanding backgrounds for both solar neutrino measurements. Sudbury
    [Show full text]
  • Solar Neutrinos
    Neutrino physics: Theory and experiment (SS2021) Solar neutrinos Teresa Marrod´anUndagoitia Max-Planck-Institut f¨urKernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany E-mail: [email protected] Contents 1 Lecture 3: Solar neutrinos2 1.1 Standard solar model.............................2 1.2 Neutrino production.............................3 1.3 Radiochemical experiments..........................5 1.4 Real time experiments............................8 1.5 Reminder: Neutrino oscillations in matter................. 14 1.6 Summary................................... 15 1 LECTURE 3: SOLAR NEUTRINOS 1. Lecture 3: Solar neutrinos This lecture discusses the emission of neutrinos by the Sun and some of the measurements performed so far. Solar neutrinos help to understand better the Sun itself but they also provide an intense source of ν's to investigate their properties. Indeed solar neutrinos have played a key role to understand neutrino oscillations. 1.1. Standard solar model Our Sun is in the most stable and long evolutionary phase of a star where hydrogen is consumed in its core (in the main sequence). A common tool to learn about the interior of the Sun is helioseismology, a methodology which employs oscillation frequencies (many modes, more than 1015) to determine the internal structure of the Sun, specifically: • density profiles • constraints on solar composition • the extension of the convective envelope ... The standard solar model (SSM) results from all these observations. Nuclear reactions in the Sun: Typically the reaction in the Sun are of the type: T1 + T2 ! T3 + T4 or T1 + T2 ! T3 + T4 + T5: (1) The temperature in the solar core is ∼ (10 -15)×106 eV corresponding to keV energies. The Coulomb barriers for nuclear reactions are however of ∼ MeV energies.
    [Show full text]
  • Neutrino Sources and Detectors
    Neutrino Detectors and Sources November 25, 2020 Contents 1 Introduction 3 2 Methods of Neutrino Detection 3 2.1 TheRadiochemicalTechnique . .... 3 2.1.1 TheHomestakeExperiment . 4 2.1.2 SAGE,GallexandGNO .............................. 4 2.1.3 Whatyouneedtoknow .............................. 4 2.2 WaterCerenkovTechnique. ..... 4 2.2.1 SuperKamiokande.................................. 7 2.2.2 SudburyNeutrinoObservatory,SNO . .... 7 2.2.3 Whatyouneedtoknow .............................. 8 2.3 Scintillation Technique . .. 8 2.3.1 KamLAND ..................................... 9 2.3.2 Whatyouneedtoknow .............................. 9 2.4 TrackingandHybridDetectors . ..... 9 2.4.1 Whatyouneedtoknow .............................. 12 3 Natural Neutrino Sources 12 3.1 RelicNeutrinos ...................................... 12 3.1.1 Whatyouneedtoknow .............................. 13 3.2 SolarNeutrinos ..................................... .. 13 3.2.1 The Solar Neutrino Detectors and the Solar Neutrino Problem . ....... 15 3.2.2 Whatyouneedtoknow .............................. 16 3.3 NeutrinosFromSupernovae . ..... 17 3.3.1 The evolution of massive stars . .. 18 3.3.2 CoreCollapse.................................... 19 3.3.3 SupernovaSN1987A ................................ 20 3.3.4 Whatyouneedtoknow .............................. 21 3.4 Other Astrophysical Neutrinos Sources . ......... 21 3.4.1 Neutrinos produced in acceleration processes . ....... 22 3.4.2 ANTARES,NESTORandBaikal . .. .. 23 3.4.3 ICECUBE...................................... 24
    [Show full text]
  • TWAS Fellows by Residence with Nationality and Membership Section Fellows by Residence
    TWAS Fellows by residence with nationality and membership section Fellows by residence Algeria (1) Benmouna Mustapha Algeria 05-Chemical Sciences Argentina (28) Andreo Carlos Santiago Argentina 02-Structural, Cell and Molecular Biology Arvia Alejandro Jorge Argentina 05-Chemical Sciences Balseiro Carlos Antonio Argentina 09-Physics Baran Enrique J. Argentina 05-Chemical Sciences Barrantes Francisco José Argentina 02-Structural, Cell and Molecular Biology Bes Daniel Raul Argentina 09-Physics Cazzulo Juan José Argentina 02-Structural, Cell and Molecular Biology de la Cruz Francisco Argentina 09-Physics Diaz Sandra Myrna Argentina 03-Biological Systems and Organisms Elgoyhen Ana Belen Argentina 04-Medical and Health Sciences incl. Neurosciences Erra-Balsells Rosa Argentina 05-Chemical Sciences Flawiá de Torres Mirtha María Argentina 02-Structural, Cell and Molecular Biology Gasparini Zulma N. Argentina 07-Astronomy, Space and Earth Sciences Litter Marta Irene Argentina 05-Chemical Sciences Maccioni Hugo J.F. Argentina 02-Structural, Cell and Molecular Biology Mandrini Cristina Hemilse Argentina 07-Astronomy, Space and Earth Sciences Mariscotti Mario Alberto Juan Argentina 09-Physics Miatello Roberto Jorge Argentina 08-Mathematical Sciences Mirabel Igor-Felix Uruguay, Argentina 07-Astronomy, Space and Earth Sciences Parodi Armando J. Argentina 02-Structural, Cell and Molecular Biology Pignotti Alberto Argentina 06-Engineering Sciences Rabinovich Gabriel Adrián Argentina 04-Medical and Health Sciences incl. Neurosciences Ramos Victor Alberto Argentina 07-Astronomy, Space and Earth Sciences Rapoport Eduardo Hugo Argentina 03-Biological Systems and Organisms Rubinstein Marcelo Argentina 02-Structural, Cell and Molecular Biology Tirao Juan Argentina 08-Mathematical Sciences Williams Roberto Juan José Argentina 06-Engineering Sciences Zaritzky Noemí Elisabet Argentina 06-Engineering Sciences Australia (4) Alpers Michael Philip Australia 04-Medical and Health Sciences incl.
    [Show full text]
  • Evidence for the Existence of Neutrinos and Neutrino Mass
    Amelia Perry Advanced Particle Physics Techniques Friday 5th December 2008 The existence of neutrinos from theory of β decay Theoretical ideas: Neutrino oscillation Cerenkov radiation Experimental evidence Homestake experiment Super Kamiokande Solar neutrinos Neutrinos formed in supernovae Reactor neutrinos Atmospheric neutrinos Geological Neutrinos Cosmic background neutrinos Existence of neutrino first predicted by Pauli in 1931 when looking at plots for beta decay There are issues with the plots which break conservation laws: Expect a unique value for energy released in beta decay, instead see a range of energies In the absence of a neutrino, angular momentum is not conserved Also, images from cloud chambers showed that linear momentum was not conserved Therefore the properties of the neutrino were chosen to remove these problems It was initially suggested that the neutrino has zero mass (But later found to be incorrect) It can be seen from these results that amendments needed to be made to theory The Homestake experiment was performed in the late 1960s by Ray Davis and John N. Bahcall and used a detector filled with a chlorine-based compound which measured solar neutrino flux 37 37 - νe + Cl Ar + e The detector was situated in the Homestake Gold Mine in South Dakota It could be seen that there was a discrepancy in the number of neutrinos detected (about ⅓ to ½) compared to that predicted by the solar model The suggested theory to solve this problem, known as the solar neutrino problem, was the idea of neutrino
    [Show full text]
  • The Search for 0Νββ Decay in 130Te with CUORE-0 by Jonathan
    The Search for 0νββ Decay in 130Te with CUORE-0 by Jonathan Loren Ouellet A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in Physics in the Graduate Division of the University of California, Berkeley Committee in charge: Professor Yury Kolomensky, Chair Professor Gabriel Orebi Gann Professor Eric B. Norman Spring 2015 The Search for 0νββ Decay in 130Te with CUORE-0 Copyright 2015 by Jonathan Loren Ouellet 1 Abstract The Search for 0νββ Decay in 130Te with CUORE-0 by Jonathan Loren Ouellet Doctor of Philosophy in Physics University of California, Berkeley Professor Yury Kolomensky, Chair This thesis describes the design, operation and results of an experimental search for neutri- noless double beta decay (0νββ) of 130Te using the CUORE-0 detector. The discovery of 0νββ would have profound implications for particle physics and our un- derstanding of the Universe. Its discovery would demonstrate the violation of lepton number and imply that neutrinos are Majorana fermions and therefore their own anti-particles. Com- bined with other experimental results, the discovery of 0νββ could also have implications for understanding the absolute neutrino mass scale as well as the presently unknown neutrino mass hierarchy. The CUORE experiment is a ton-scale search for 0νββ in 130Te expected to begin oper- ation in late 2015. The first stage of this experiment is a smaller 39-kg active-mass detector called CUORE-0. This detector contains 11 kg of 130Te and operates in the Laboratori Nazionali del Gran Sasso lab in Italy from 2013 { 2015. nat The results presented here are based on a TeO2 exposure of 35.2 kg·yr, or 9.8 kg·yr exposure of 130Te collected between 2013 { 2015.
    [Show full text]