The Nu-SNS proposal - ORNL Physics Division - Oak Ridge ...

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SMMC - Shell Model Monte Carlo SNO - Sudbury Neutrino Observatory SNS - Spallation Neutron Source TDC - Time to Digital Converter TEC - Total Estimated Cost TPC - Total Project Cost UT - University of Tennessee WBS - Work Breakdown Structure WLS - Wavelength Shifting WW95 - Woosley and Weaver, 1995 ν-SNS Proposal xii 8/4/2005
1 EXECUTIVE SUMMARY Measurements during the last few decades have substantially improved our understanding of neutrino properties and reshaped the foundations of our understanding of nature. In spite of this remarkable progress several important questions still remain. Among these are the role that neutrino-nucleus interactions play in the supernova explosion process and subsequent nucleosynthesis. During these spectacular events 10 46 joules of gravitational energy are released into space. The resulting flash of visible light is as bright as an entire galaxy, yet this represents only a tiny fraction of the total energy in the explosion: ~99% of the energy is carried away by neutrinos. Accurate knowledge of neutrino-nucleus cross sections is important to understanding these important events. However, the reliability of theoretical models used to predict such cross sections is highly uncertain, and almost no data exist. This lack of knowledge significantly limits our understanding of supernovae and of terrestrial observations of cosmic neutrinos to probe the deepest layer of these powerful explosions. Broad agreement on the importance of neutrino measurements in general, and the relationship of neutrinos and supernovae in particular, are reflected in several recently published documents. These include the DOE Office of Science Strategic Plan [1], the National Academy of Science (NAS) Study Connecting Quarks with the Cosmos [2], and a report from the National Research Council (NRC) of the National Academies, Neutrinos and Beyond—New Windows on Nature [3]. Two of the seven highest priorities for the Office of Science listed in the Strategic Plan will impact our understanding of supernovae and heavy element nucleosynthesis where neutrinos play a key role. The NAS report lists eleven key questions that are of deep interest for science at the intersection of astronomy and physics, including “How were the heavy elements from Iron to Uranium made” and “How have neutrinos shaped the evolution of the Universe” That report notes “More realistic simulations of supernova explosions and neutron star mergers are essential. …In addition, better measurements are needed for both the inputs and outputs of these calculations.” The NRC report lists several questions that the authors believe the nuclear physics community is now poised to answer. Among those questions are “What causes the most powerful explosions in the universe” and “What role do neutrinos play in the synthesis of the elements in the periodic table” The report also supports building large underground supernova neutrino detectors. In response to the above studies and plans, and to the excitement over recent neutrino measurements, the American Physical Society Divisions of Particles and Fields, Nuclear Physics, Astrophysics, and the Physics of Beams, sponsored a year-long Study on the Physics of Neutrinos. The study lays the scientific groundwork for the choices for neutrino physics research to be made over the next few years. The Study Group recently published its final report, The Neutrino Matrix [4], which in Section 4, Recommendations, states: “The precise determination of neutrino cross sections is an essential ingredient in the interpretation of neutrino experiments and is, in addition, capable of revealing exotic and unexpected phenomena, such as the existence of a neutrino magnetic dipole moment. Interpretation of atmospheric and long-baseline accelerator-based neutrino experiments, understanding the role of neutrinos in supernova explosions, and predicting the abundances of events in those explosions all require knowledge of neutrino cross sections. ν-SNS Proposal 1 8/4/2005
Page 1: ν ν
Page 5 and 6: TABLE OF CONTENTS LIST OF FIGURES .
Page 7 and 8: APPENDIX 1 ν-SNS INSTRUMENT DEVELO
Page 9 and 10: LIST OF FIGURES Figure Page 2.1 Dia
Page 11 and 12: 4.44 Block diagram of the ν-SNS fr
Page 13 and 14: LIST OF TABLES Table Page 1.1 Insti
Page 15: ACRONYM LIST ADC - Analog to Digita
Page 19 and 20: Our present cost estimate for the s
Page 21 and 22: 2 PROJECT OVERVIEW 2.1 Scientific M
Page 23 and 24: the detailed structure of the induc
Page 25 and 26: Figure 2.3 Time and energy distribu
Page 27 and 28: Proton Beamline ν-SNS Beamline 18
Page 29 and 30: detectors. Simultaneous operation a
Page 31 and 32: 3500 3000 2500 Escalated TPC (in as
Page 33 and 34: 3 SCIENTIFIC MOTIVATION There are m
Page 35 and 36: The neutrino energy deposition behi
Page 37 and 38: Figure 3.2 Energy scales and compos
Page 39 and 40: (LMS) calculated electron capture r
Page 41 and 42: Figure 3.5 Comparison of the core v
Page 43 and 44: composition and spatial distributio
Page 45 and 46: supernova is initiated [62]. Other
Page 47 and 48: In addition, the appearance of back
Page 49 and 50: differential cross sections can pro
Page 51 and 52: Another example of the impact that
Page 53 and 54: sensitivity achieved by ν−SNS fo
Page 55 and 56: References for Section 3: 1. “Con
Page 57 and 58: 60. W.C. Haxton, Neutrinos In Physi
Page 59 and 60: 4 PROJECT DESCRIPTION The Spallatio
Page 61 and 62: 4.1.1 Neutrons Escaping from the Sp
Page 63 and 64: Flux (in n/cm 2 /s) Figure 4.3 Back
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Vertical Distance from Beam (cm) Ho
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4.1.5 Cosmic Ray Backgrounds The co
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• All backgrounds by utilizing pa
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eamline will be removable, with the
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Table 4.1 Cost breakdown for the sh
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4.3.3 Simulated Performance In orde
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(0.005%). Using current neutron flu
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Figure 4.15 Conceptual design of on
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Table 4.2 Cost breakdown for the co
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4.4 Segmented Detector 4.4.1 Requir
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Counts (arbitrarily normalized ) Fi
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As expected, thinner targets allow
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Counts (arbitrary normalization) Ne
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Counts (normalized for one year ful
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Counts (normalized for one year ful
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In conclusion, Monte Carlo studies
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Sense wires are held at high voltag
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Table 4.5 Cost breakdown for the se
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4.5 Homogeneous Detector 4.5.1 Requ
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A candidate for the PMTs to be used
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from control samples recorded durin
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The visible light signal recorded i
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Figure 4.43 Relative PMT light coll
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Table 4.6 Cost breakdown for the ho
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4.6 Common Data Acquisition System
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Table 4.7 Cost breakdown for the co
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Section 4 References: 1. MCNPX Team
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5 COST AND SCHEDULE 5.1 Work Breakd
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Example: Machining Bunker Steel Pla
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Table 5.4 Proposed ν-SNS budget pr
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6 MANAGEMENT PLAN AND PROJECT CONTR
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We respond to these special charact
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6.5 Quality Assurance and Control T
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see Appendix 5 for details. The lar
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APPENDIX 1 ν-SNS INSTRUMENT DEVELO
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APPENDIX 2 CURRICULUM VITAE OF ν-S
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Professional Vitae Summary Fred E.
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JEFF C. BLACKMON Physics Division,
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Vince Cianciolo Physics Division, O
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Biographical Sketch YURI EFREMENKO
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Curriculum Vitae TONY A. GABRIEL Ex
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• Past Member, Organizing Committ
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Dr. rer. nat. Uwe Greife, Associate
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Physics Division Oak Ridge National
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Biographical Sketch Gail C. McLaugh
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ION STANCU Department of Physics an
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21. D.V. Ahluwalia, Y. Liu and I. S
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APPENDIX 3 SNS REVIEW RESULTS In Su
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ν-SNS Proposal A-29 8/4/2005
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poorly known neutrino-nucleus cross
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APPENDIX 4 SNS TARGET HALL FLOOR LO
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APPENDIX 5 ν-SNS R&D PROGRAM Detec
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Segmented Detector Mechanics The se
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