NNN2011 � Short and long baseline oscillations with DAR sources and status of DAE δ ALUS Sanjib Kumar Agarwalla Sanjib.Agarwalla@ific.uv.es IFIC/CSIC, University of Valencia, Spain Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Stopped Pion Source 1/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Decay At Rest (DAR) Source 2/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Proton Source 3/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Physics Goals 4/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � What do we want and what helps? We want 1 MW sources of protons with energy of 800 MeV for a reasonable price What are the factors that are going to help us? Ø No fancy beam structure – Continuous source (CW) is fine run 100 ms on and 400 ms off for CP violation running longer periods may be fine for short baseline Ø No need to inject into another accelerator Ø Constant energy -- no need for an energy upgrade path Unlike Project-X or SNS, which need all of the above 5/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � The world-wide cyclotron industry Others are also looking for ~ 1 GeV Machines for various applications “ADS’’ – Accelerator driven systems for subcritical reactors “DTRA’’ – Defense Threat Reduction Agency Both applications & others are of interest to industry 6/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Various Types of Proton Accelerators Janet Conrad, Frontiers in Neutrino Physics, 2011 7/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Approaches using Cyclotrons Proposed by Carlo Rubbia, 1994 Initial design by L. Calabretta Janet Conrad, Frontiers in Neutrino Physics, 2011 8/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Cyclotron@PSI 9/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Working Examples u The ion source: prototype built at Catania u The injector cyclotron: modest modification to off-shelf model from, e.g., BEST Cyclotron Systems Inc. u The main cyclotron: smaller, simpler version of Riken (Japan) u The extraction foils: well tested at many cyclotron facilities, including PSI and TRIUMF u The target/dumps: At present we have multiple extraction lines but can be avoided by spreading beam Now, we need to optimize all the above components 10/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Current Progress and Future Plans Ø We have a 1st generation design Ø We have a prototype ion source, which produced 20 mA immediately Ø The large magnet specifications are nearly complete, and we expect to go to engineers for first costing within 2 months. This will help us to estimate the cost Ø We have first funding from NSF for our development experiments 11/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Leptonic CP violation The discovery of CP violation in the lepton sector would constitute a smoking gun for leptogenesis to explain the baryon asymmetry of the Universe Can we study CPV using DAR neutrino sources? The effort of DAE δ ALUS collaboration Conrad & Shaevitz, PRL 104:141802 (2010) See also, arXiv:1006.0260, 1008.4967, 1012.4853 Add LBNE (Neutrino Run) + DAR (Anti-neutrino Run) SKA, Huber, Link, Mohapatra, arXiv:1005.4055 12/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Want to measure but not known 13/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � DAE δ ALUS setup Janet Conrad, Frontiers in Neutrino Physics, 2011 14/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Signal .vs. Background 15/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � CP Measurement Normal Inverted 16/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � DAE δ ALUS + LBNE Ø DAE δ ALUS baseline: 20 to 1.5 km Ø LBNE baseline: 1300 km Ø DAE δ ALUS has no matter effects Ø LBNE has matter effects Ø DAE δ ALUS Energy is low (20 to 53 MeV) Ø LBNE Energy is high (0.5 to 6 GeV) Ø DAE δ ALUS is a anti-neutrino experiment Ø LBNE is mainly a neutrino expt (anti-neutrino rates are lower) Ø DAE δ ALUS varies beam distance Ø LBNE varies beam energy Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011 17/31
NNN2011 � LBNE Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011 18/31
NNN2011 � New Approach New Approach : DAR + HFN LBNE : HFA + HFN 4 P roton Accelerators � 1 MW, 1 GeV µ � e Low − cost, High − pow er � µ 4 . 10 22 0 10 20 30 40 50 neutrinos/flavor/year/accelerator DAR E [MeV] � � DAR : e µ 20 − 55 MeV 2 0 k m I B D DUSEL 1300 km CC QE w / Gd FNAL � � HFN : e µ 100 − 300 kton 0.5 − 6 GeV Wide Band Beam � � HFA : e µ 700 kW, 120 GeV 20 6.2 . 10 protons/year SKA, Huber, Link, Mohapatra, arXiv:1005.4055 19/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Signal .vs. Background SKA, Huber, Link, Mohapatra, arXiv:1005.4055 20/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Discovery Potential � 13 discovery MH discovery CPV discovery 1 GLoBES 2010 DAR+HFN, NH 300 kt WC Fraction of � cp (true) DAR+HFN, IH 0.8 HFA+HFN, NH HFA+HFN, IH 0.6 0.4 0.2 (a) (b) (c) 0 0.001 0.01 0.1 0.001 0.01 0.1 0.001 0.01 0.1 sin 2 2 � 13 (true) sin 2 2 � 13 (true) sin 2 2 � 13 (true) SKA, Huber, Link, Mohapatra, arXiv:1005.4055 21/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Short-baseline ν oscillations 22/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � How to solve the short-baseline puzzle? 23/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Cyclotron : Proton Source 24/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � Neutrino Source Details 25/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � DAR beam interactions 26/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � DAR + LENA Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011 27/31
NNN2011 � Appearance Wave in LENA 28/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � DAR-LENA Sterile Sensitivity 29/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � NO ν A : Coming Soon 30/31 Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
NNN2011 � DAR-LAr Sterile Sensitivity Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011 31/31
NNN2011 � Concluding Remarks Ø A stopped pion source provides neutrino beams with energy of a few tens of MeV from pion and muon decay-at-rest Ø A rich physics program can be accomplished with such a neutrino source Ø Low-cost, multi-MW proton cyclotrons needed Ø 5 kt LENA combined with a small 10 kW DAR source can test the LSND/MiniBooNE anti-neutrino signal at 5 sigma in 3+1 model in 1 year Ø DAR neutrino sources together with LBNE can accelerate the discovery reach of CP violation Stay Tuned for exciting physics with DAR beam Thank You ! Sanjib Kumar Agarwalla, NNN11, Zurich, Switzerland, 9 th November, 2011
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