1. Carolina Neutrino Workshop 20041 Prospects for Neutrino Physics at the Spallation Neutron Source Vince Cianciolo, ORNL for the SNS Collaboration

2. Carolina Neutrino Workshop 20042 The Spallation Neutron Source Proton beam current:1 mA Proton beam energy:1 GeV Protons/pulse:~1.6  10 14 Pulse rate: 60 Hz Pulse length:380 ns (FWHM) Operating hours/year:5000 Proton target material: Mercury Neutrinos/pulse/flavor: ~1.6  10 13 Neutrino-target interactions/year:few thousand Neutrino! Repeat 60/sec.  x ~1000  LINAC: Accumulator Ring: A ++ -- ~99% ++   e e+e+ p

3. Carolina Neutrino Workshop 20043 Time Structure Decays with t 1/2 = t 1/2 = 26 ns  Next pulse arrives in 16,000,000 ns! Turning the detector on for only a few  s after each pulse reduces cosmic- ray background by ~ x2,500. 2.3 km water-equivalent. Leaving the detector off for the first  s after a pulse effectively eliminates machine-related backgrounds. –Also eliminates clean neutral- current events. –Whether sufficient background rejection can be achieved w/o this cut (through shielding and detector techniques) is under study. Decays with t 1/2 = t 1/2 = 2.2  s 

4. Carolina Neutrino Workshop 20044 Energy Spectra Neutrino spectra at stopped-pion facilities have significant overlap with the spectra of neutrinos generated in a supernova explosion! SNS neutrino spectraSupernova neutrino spectra, 100 ms post-bounce

5. Carolina Neutrino Workshop 20045 Scientific Motivation Core-collapse supernovae. Neutrino detector calibration. Nuclear structure (complement to RIA). National Research Council Report by the Committee on the Physics of the Universe

6. Carolina Neutrino Workshop 20046 Core Collapse Supernovae Most spectacular explosions in the universe. (R. Hix) Birthplace of most “heavy” elements – we are stardust. The core of a supernova is so dense it is black to neutrinos. Since there are so many of them they play a crucial role in the explosion and the accompanying nucleosynthesis. Knowledge of A cross-sections for A<120 is crucial when attempting to make accurate supernova models.

7. Carolina Neutrino Workshop 20047 Neutrino Detector Calibration Large-scale detectors exist or are proposed to measure supernovae neutrinos. In order to make full use of their data, calibrations of neutrino interactions in the detector materials are required. Integral cross-sections insufficient. –Differential cross-sections (vs. energy, angle) are crucial. –Neutral-current interactions also very important.

8. Carolina Neutrino Workshop 20048 Nuclear Structure A cross section measurements provide important information to constrain nuclear structure models. Reasonable extrapolations away from measured nuclei can be made for ~  N<8,  P<8 (up to shell boundaries). The plot shows extrapolation regions relative to 8 of the ~36 feasible target materials. –Rather complete coverage in a few years!

9. Carolina Neutrino Workshop 20049 SNS Goal: Precision A Cross Section Measurements Build a facility that will allow a total cross section measurement with  <10% in one year.

10. Carolina Neutrino Workshop 200410 Feasibility A suitable location has been identified. Floor-loading calculations have been performed. Total capacity = 545 tons. –Allows for 1 meter ceiling, ½ meter walls. –Together with SNS time structure, active veto provides sufficient rejection of cosmic-ray background. SNS management has provided encouraging response and is empanelling a review committee.

11. Carolina Neutrino Workshop 200411 Bunker, Active Veto Active veto (  > 99%) required to reduce cosmic muons. Time structure plus passive shield reduces cosmogenic and machine- related neutron backgrounds sufficiently. –1m thick ceiling;½-m thick walls –4.5 x 4.5 x 6.5 m 3 total vol.  3.5 x 3.5 x 5.5 m 3 inside shield. Remaining volume large enough to house two 10-ton fiducial target/detectors. S Detector 1 20 t Detector 2 20 t Shielding Veto

12. Carolina Neutrino Workshop 200412 Segmented Detector Designed to handle metals or other solid targets. Targets – thin wall pipes, easily replaced. Active detector – straw gas tubes. Mass of the sensitive part of the detector is less than target mass. Reconstruct tracks and count # of fired tubes: –  E ~ 30% –   ~ 15 degrees Particle ID through e.g., # of fired tubes, track linearity, energy deposition. e

13. Carolina Neutrino Workshop 200413 Homogeneous Detector “Standard” technology –  Boone Suitable for transparent liquid targets, e.g., d, C, N, O, I, Br, Pb Light detection by PMT or PD ~38% PMT coverage allows for either scintillator or Cerenkov detection.

14. Carolina Neutrino Workshop 200414 Timescale Commissioning could reasonably begin when machine power approaches design value (end of CY08).

15. Carolina Neutrino Workshop 200415 http://www.phy.ornl.gov/workshops/nusns/vSNSstudy.pdf Collaboration Robust collaboration. –>30 members, more welcome! –Next collaboration meeting to be held June 11-12 at ORNL. Assembled study report that discusses all elements of this talk in greater detail. –Will form the basis for input to the APS Neutrino Working Group –Copies available at back of room, on the web.

16. Carolina Neutrino Workshop 200416 Conclusions The SNS provides a unique opportunity to study low- energy (10’s of MeV) A interactions. –Pulsed time structure. –Intensity. Building a A facility at the SNS is feasible. –Sufficient intensity. –Suitable location. –SNS Management encouragement. Addresses broad range of physics interests. –Understanding the supernova explosion mechanism. –Calibration of neutrino detectors. –Nuclear structure complementary to RIA.

17. Carolina Neutrino Workshop 200417 Neutrino oscillations at the SNS ORLAND Redux If MiniBoone confirms LSND result, the SNS would be a logical place to follow up. Low backgrounds due to absorption of the vast majority of e s in mercury target. If nSNS goes forward there will already be a near detector to quantify the remaining backgrounds. Very precise measurement of oscillation parameters possible.