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SNS 2 Meeting

SNS 2 Meeting. Opening Remarks, Purpose Glenn R. Young Physics Division, ORNL August 28, 2003. Why Are We Here?. SNS makes large flux of neutrinos These are in an interesting energy range for nuclear physics and astrophysics

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SNS 2 Meeting

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  1. SNS2 Meeting Opening Remarks, Purpose Glenn R. Young Physics Division, ORNL August 28, 2003

  2. Why Are We Here? • SNS makes large flux of neutrinos • These are in an interesting energy range for nuclear physics and astrophysics • Experimenters are obstreperous people who believe you should never take a theorist's word for it on cross sections

  3. Making the Science Case • Does this impact our understanding of • nuclear structure • neutrino cross sections • supernovae explosions • nucleosynthesis • Can you define science goals and a measurement program? • Which cross sections are most interesting? • Which provide the biggest "sensitivity" for our understanding of physics?

  4. Does It Pass the Ha Ha Test ? • Given the input parameters - neutrino flux - "1 year" of SNS running - reasonable volume of detector - expected cross sections - active fraction of volume • Do you get an interesting number of events? • How many cases can you handle in 10 years?

  5. Does It Pass Practical Factors Checks ? • Can it find a permanent home at the SNS? • Can you change the "target" in a reasonable length of time? - how long to run one target? - how long physically to change target material? • Can you allow for both segmented and homogenous detectors? • Can you load 2 targets simultaneously? i.e., run 2 detectors? • Can you stay under a few $M?

  6. Can You Define a Detector Suite? • What are the scales of the detectors? • Passive vs. active volume • Shape • Technology • ”Channel counts"

  7. Can You Handle Shielding? • Background rates and composition • Signatures of background events? • Shield concept? • Mass? • Floor loading? • Resultant errors on physics measurements?

  8. What are the Interfaces with the SNS? • Space • Services • People • Run cycle • Evolution of beam energy, intensity • Monitoring of power, neutrino flux and fluence

  9. How Long Do Things Take? • How long to design • to build • to commission • to do one target • to change targets

  10. Can a Collaboration Be Formed? • Who • How many people? • Tasks? • Universities? • Students? What are their projects? • Leadership? • R&D needed? or proof-of-concept

  11. What is it Going to Cost? • Initial cost - capitalization • Running cost - people, consumables, upgrades • Target change cost - an area for deferral to the future;-)

  12. How Do We Sell It? • Mentioned in LRP but not as a major item • Linkage to CPU report of M. Turner • DNP will have session on ‘how to respond’ at Tucson • Linkage to ongoing RIA, SciDAC, NASA efforts • People needed • Student opportunities • Cost • “Advertising”

  13. What is the Timeline from Today to Proposal to Construction? • Need ‘formal’ SNS approval (may have it) • Need White Paper on physics • Need Proposal • Need "friendly" DOE, NSF, DNP, LRP (next LRP in 2007 ;-( ) • “For information only” presentation to DOE and NSF by early 2004 • At least 2 years from proposal to funding

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