DOCSLIB.ORG

Current Status of Neutrino Anomalies

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Current Status of Neutrino Anomalies Current Status of Neutrino Anomalies Srubabati Goswami Physical Research Laboratory, Ahmedabad, India Anomalies 2020 !1 Is it a monument, a madrasa or a market square? Charminar holds many mysteries within its fold https://www.thehindu.com/society/history-and-culture/the-very-many-mysteries-of-hyderabads-charminar/ article24311906.ece !2 Neutrino: many questions ❖ What Unknown oscillation parameters - hierarchy, octant of 2-3 mixing angle and CP phase ❖ Absolute neutrino masses — beta decay, cosmology ❖ Nature of neutrinos - Dirac or Majorana — neutrino less double beta decay ❖ Are there more than three flavours — sterile neutrinos ❖ Origin of neutrino masses and mixing — seesaw , flavour symmetry — physics beyond Standard Model !3 Neutrino Connections Baryogenesis via Collider leptogenesis Physics Dark Matter Higgs/Vacuum Cosmology stability Neutrinos Astrophysics/ CLFV Multimessenger Nucl. Physics/ interactions !4 Plan of talk New physics Neutrino Neutrinoless Ultra high In neutrino Oscillation double Energy neutrinos Parameters oscillation beta decay NSI Sterile Nus !5 Neutrino Oscillations Solar Atmospheric Reactor Accelerator !6 New result from Borexino !7 First detection of CNO neutrinos R(CNO) = 7.2 +2.9 -1.7 cpd/100ton Null hypothesis(CNO=0) rejected at 5.1 sigma. G. Ranucci , Neutrino 2020 !8 Three Neutrino Paradigm ❖ Measurement of non-zero in reactor experiments three neutrino picture !9 NOvA Results Joint analysis of disappearance and Appearance data in both neutrino and antineutrino channel ❖ P Preference for Neutrino 2020 !10 <latexit sha1_base64="YNe9BjUx7lO0i+8BBVI+kwZ9Qko=">AAAB7XicbVBNSwMxEJ2tX7V+tOrRS7AIXqy7paDeil48VrAf0C4lm2bb2GyyJFmhLP0PXjwo4tX/481/Y9ruQVsfDDzem2FmXhBzpo3rfju5tfWNza38dmFnd2+/WDo4bGmZKEKbRHKpOgHWlDNBm4YZTjuxojgKOG0H49uZ336iSjMpHswkpn6Eh4KFjGBjpdZ5L2YX1X6p7FbcOdAq8TJShgyNfumrN5AkiagwhGOtu54bGz/FyjDC6bTQSzSNMRnjIe1aKnBEtZ/Or52iU6sMUCiVLWHQXP09keJI60kU2M4Im5Fe9mbif143MeGVnzIRJ4YKslgUJhwZiWavowFTlBg+sQQTxeytiIywwsTYgAo2BG/55VXSqla8WuX6vlau32Rx5OEYTuAMPLiEOtxBA5pA4BGe4RXeHOm8OO/Ox6I152QzR/AHzucPnRyOhQ==</latexit> T2K Results Appearance channel Preference for NH CP phase close to ⇡/2 CP conserving values disfavoured− L. Muntaneu, Neutrino 2020 !11 Current Status ❖ Best-fit in second octant ❖ Preference for NO ❖ disfavoured at more than irrespective of mass ordering ❖ Oscillation experiments not sensitive to Majorana phases !12 Degeneracy problem ❖ The main problem in determination of hierarchy, octant and in LBL experiments is due to presence of degeneracies ❖ Degeneracy different set of parameters giving the same probability equally good fit to the data ❖ !13 Ongoing and planned experiments ORCA Daya-bay JUNO Dune T2K* SK* NOvA* T2HK HK INO Beam Reactor Atmospheric PINGU !14 Future Goals ❖ Determination of hierarchy, octant and CP phase ❖ Probing new physics in oscillation experiments ❖ Testing models of flavour symmetry ❖ Synergy between different experiments !15 Mass hierarchy and CP with DUNE Hierarchy sensitivity due Matter effects help in removing to enhanced matter effects wrong hierarchy-wrong CP solutions From: R. Patterson’s slides !16 Hierarchy: Juno+IceCube upgrade 8 core JUNO + IceCube upgrade/PINGU / (better efficiency for lower energy neutrinos) 5<latexit sha1_base64="WWseafwUHEZgzwBdIiAoiyqhv3M=">AAAB73icbVBNSwMxEJ2tX7V+VT16CRbBU9nVFj0WvXisYD+gXUo2zbahSXZNskJZ+ie8eFDEq3/Hm//GbLsHbX0w8Hhvhpl5QcyZNq777RTW1jc2t4rbpZ3dvf2D8uFRW0eJIrRFIh6pboA15UzSlmGG026sKBYBp51gcpv5nSeqNIvkg5nG1Bd4JFnICDZW6tb7mo0ELg3KFbfqzoFWiZeTCuRoDspf/WFEEkGlIRxr3fPc2PgpVoYRTmelfqJpjMkEj2jPUokF1X46v3eGzqwyRGGkbEmD5urviRQLracisJ0Cm7Fe9jLxP6+XmPDaT5mME0MlWSwKE45MhLLn0ZApSgyfWoKJYvZWRMZYYWJsRFkI3vLLq6R9UfUuq/X7WqVxk8dRhBM4hXPw4AoacAdNaAEBDs/wCm/Oo/PivDsfi9aCk88cwx84nz9L7I99</latexit> σ sensitivity in 4(6) years NO (IO) IceCube : earth matter effect of atmospheric neutrinos Synergy JUNO: interference effect in vacuum oscillation <latexit sha1_base64="hvoHiL5R/EOWhKvJ1YWzZXB1/eg=">AAAB6XicbVDLSgNBEOyNrxhfUY9eBoPgKez6QI9BLx6jmAckS5idzCZDZmeXmV4hLPkDLx4U8eofefNvnCR70MSChqKqm+6uIJHCoOt+O4WV1bX1jeJmaWt7Z3evvH/QNHGqGW+wWMa6HVDDpVC8gQIlbyea0yiQvBWMbqd+64lrI2L1iOOE+xEdKBEKRtFKD91Jr1xxq+4MZJl4OalAjnqv/NXtxyyNuEImqTEdz03Qz6hGwSSflLqp4QllIzrgHUsVjbjxs9mlE3JilT4JY21LIZmpvycyGhkzjgLbGVEcmkVvKv7ndVIMr/1MqCRFrth8UZhKgjGZvk36QnOGcmwJZVrYWwkbUk0Z2nBKNgRv8eVl0jyreufVy/uLSu0mj6MIR3AMp+DBFdTgDurQAAYhPMMrvDkj58V5dz7mrQUnnzmEP3A+fwCg0I1u</latexit> hep-ex} 1911.06745 !17 New Physics ❖ Sterile Neutrinos Two appoaches ❖ Non-standard Interactions (NSI) ❖ Non-unitary mixing ❖ CPT and Lorentz symmetry violation Impact on the standard Constraining new ❖ Long range forces Three neutrino picture physics parameters ❖ Neutrino decay !18 Non-standard interactions !19 Non-standard interactions Standard-NC interaction Non-Standard NC interaction !20 NSI and mass hierarchy Fit to T2K and NOvA data assuming NSI IO prefers non-zero NSI IO no longer disfavoured Capozzi, Chatterjee, Palazzo 1908.06992 !21 Degeneracies due to diagonal NSI ❖ New degeneracies with NSI ❖ Coloma, Schwetz, PRD 2016 In matter potential K.N. Deepthi, S.Goswami, N. Nath, PRD 2016 Spoils the hierarchy sensitivity of Dune !22 NSI and CP sensitivity Mehta, Masood, 1603.01380 NSI can spoil CP sensitivity !23 Dark-LMA solution ❖ Degenerate solution to the solar neutrinos problem ❖ 2 o sin<latexit sha1_base64="EnZeoJ7ILbb1GK81eZCTuIIAY50=">AAACAXicbVDLSgNBEJyNrxhfq14EL4NB8BR2Y4KeJOjFYwTzgOwmzE4myZDZ2WWmVwhLvPgrXjwo4tW/8ObfOHkcNLGgoajqprsriAXX4DjfVmZldW19I7uZ29re2d2z9w/qOkoUZTUaiUg1A6KZ4JLVgINgzVgxEgaCNYLhzcRvPDCleSTvYRQzPyR9yXucEjBSxz7yNJftogcDBqSTusUxvsKlcjvq2Hmn4EyBl4k7J3k0R7Vjf3ndiCYhk0AF0brlOjH4KVHAqWDjnJdoFhM6JH3WMlSSkGk/nX4wxqdG6eJepExJwFP190RKQq1HYWA6QwIDvehNxP+8VgK9Sz/lMk6ASTpb1EsEhghP4sBdrhgFMTKEUMXNrZgOiCIUTGg5E4K7+PIyqRcL7nmhfFfKV67ncWTRMTpBZ8hFF6iCblEV1RBFj+gZvaI368l6sd6tj1lrxprPHKI/sD5/AKTblbg=</latexit> ✓ 12 > 45 Miranda, Tortola, Valle ,JHEP. 10 (2006) 008. !24 COHERENT constraints Nucleus recoils as a whole Coherent upto 50 MeV ❖ Highly constrained by COHERENT using energy spectrum information Coloma, Esteban,Gonzalez-Garcia, Maltoni 1911.09109 !25 Neutrinoless double beta decay ❖ Standard picture mediated 0<latexit sha1_base64="dsoZ9MQG/Iqc6tMM/Q62LR3ISAE=">AAAB+HicbVDLSsNAFL3xWeujUZduBovgqiQ+0GXRjcsK9gFNKJPppB06mYSZiVBDv8SNC0Xc+inu/BsnaRbaeuBeDufcy9w5QcKZ0o7zba2srq1vbFa2qts7u3s1e/+go+JUEtomMY9lL8CKciZoWzPNaS+RFEcBp91gcpv73UcqFYvFg54m1I/wSLCQEayNNLBrjidSL6AaF606sOtOwymAlolbkjqUaA3sL28YkzSiQhOOleq7TqL9DEvNCKezqpcqmmAywSPaN1TgiCo/Kw6foROjDFEYS1NCo0L9vZHhSKlpFJjJCOuxWvRy8T+vn+rw2s+YSFJNBZk/FKYc6RjlKaAhk5RoPjUEE8nMrYiMscREm6zyENzFLy+TzlnDPW9c3l/UmzdlHBU4gmM4BReuoAl30II2EEjhGV7hzXqyXqx362M+umKVO4fwB9bnDwo0krE=</latexit> ⌫β by light neutrinos ❖ G contains the phase space factor M<latexit sha1_base64="P8rlATgstvISNqWOzm/6YrXHzN4=">AAAB8HicbVBNSwMxEJ2tX7V+VT16CRbBU9nVih6LXrwIFeyHtEvJptk2NMkuSVYoS3+FFw+KePXnePPfmG33oK0PBh7vzTAzL4g508Z1v53Cyura+kZxs7S1vbO7V94/aOkoUYQ2ScQj1QmwppxJ2jTMcNqJFcUi4LQdjG8yv/1ElWaRfDCTmPoCDyULGcHGSo/p3bTfkwkq9csVt+rOgJaJl5MK5Gj0y1+9QUQSQaUhHGvd9dzY+ClWhhFOp6VeommMyRgPaddSiQXVfjo7eIpOrDJAYaRsSYNm6u+JFAutJyKwnQKbkV70MvE/r5uY8MpPmYwTQyWZLwoTjkyEsu/RgClKDJ9Ygoli9lZERlhhYmxGWQje4svLpHVW9c6rF/e1Sv06j6MIR3AMp+DBJdThFhrQBAICnuEV3hzlvDjvzse8teDkM4fwB87nDwiDj+g=</latexit> ⌫ is the nuclear matrix elements !26 Current and future sensitivity Current Sensitivity KamLAND-ZEN : 61-165 meV EXO 200 : 93-286 meV GERDA : 110-260 meV CUORE : 110-520 meV Future sensitivity 0.008 - 0.3 eV : IH can be confirmed 0.003 - .008 eV : 1-10 ton detector 0.001 - .003 eV : 10-100 ton detector ultimate sensitivity Barabash, 1901.11342 !27 NSI and Neutrinoless double beta decay ❖ New predictions in presence of NSI for NH ❖ Within reach of 10 kt detectors ❖ New sensitivity goal ❖ For NH degeneracy between LMA and DLMA can be broken for lower values of lightest neutrino mass ❖ Model independent Vishnudath, Choubey, Goswami, Phys, Rev. D. (2019) !28 Are there more than 3 neutrinos ? Extra sterile neutrino ? Light or heavy or both ? !29 Sterile Neutrinos : indications LSND Ga Anomaly Lavedar et al 2017 SAGE PRC 2007 LSND PRL 1995, GALLEX PRC 2007 PRD 2001 Mueller et al PRC 2011 Huber PRC 2011 Mention et al PRD 2011 Reactor Anomaly !30 Very short baseline reactor experiments ❖ B L<latexit sha1_base64="VBv8G0FEYbbSCi88bKw/KVe2XsE=">AAAB9XicbVC5TgMxEJ3lDOEKUNJYREg0RLshHGUEDQVFkMghJUvkdbyJFdu7sr2gaBW+g4YChGj5Fzr+BucoIOFJIz29N6OZeUHMmTau++0sLC4tr6xm1rLrG5tb27md3ZqOEkVolUQ8Uo0Aa8qZpFXDDKeNWFEsAk7rQf9q5NcfqNIskndmEFNf4K5kISPYWOn+BrU0E+jsuFh6QqKdy7sFdww0T7wpycMUlXbuq9WJSCKoNIRjrZueGxs/xcowwukw20o0jTHp4y5tWiqxoNpPx1cP0aFVOiiMlC1p0Fj9PZFiofVABLZTYNPTs95I/M9rJia88FMm48RQSSaLwoQjE6FRBKjDFCWGDyzBRDF7KyI9rDAxNqisDcGbfXme1IoF76RwelvKly+ncWRgHw7gCDw4hzJcQwWqQEDBM7zCm/PovDjvzsekdcGZzuzBHzifP0VFkRI=</latexit> 6 24 m ⇠ − !31 NEOS and DANSS Neos Collaboration PRL 2016 Danss collaboration, PLB 2018 Comparison of measured spectra at different baselines Insensitive to flux calculation uncertainty !32 Bounds from reactor searches Dentler et al. JHEP 2018 Blue shaded regions allowed by fitting all reactor data with free fluxes ∆m2 DANSS 2019 results give a lower <latexit sha1_base64="CPsfgjCCu1Qq20Zhwqf5pj0NEVs=">AAAB+XicbVBNS8NAEJ3Ur1q/oh69LBbBU0lqRY9FPXisYD+gjWGz3bRLd5OwuymU0H/ixYMiXv0n3vw3btsctPXBwOO9GWbmBQlnSjvOt1VYW9/Y3Cpul3Z29/YP7MOjlopTSWiTxDyWnQAryllEm5ppTjuJpFgEnLaD0e3Mb4+pVCyOHvUkoZ7Ag4iFjGBtJN+2e3eUa4zEU9XPau4U+XbZqThzoFXi5qQMORq+/dXrxyQVNNKEY6W6rpNoL8NSM8LptNRLFU0wGeEB7RoaYUGVl80vn6Izo/RRGEtTkUZz9fdEhoVSExGYToH1UC17M/E/r5vq8NrLWJSkmkZksShMOdIxmsWA+kxSovnEEEwkM7ciMsQSE23CKpkQ3OWXV0mrWnEvKpcPtXL9Jo+jCCdwCufgwhXU4R4a0AQCY3iGV3izMuvFerc+Fq0FK585hj+wPn8A8kySkQ==</latexit>
Load more

Recommended publications
  • Arxiv:1812.08768V2 [Hep-Ph] 3 Dec 2019
    IPPP/18/113/FERMILAB-PUB-18-686-A-ND-PPD-T Testing New Physics Explanations of MiniBooNE Anomaly at Neutrino Scattering Experiments 1, 2, 3, Carlos A. Argüelles, ∗ Matheus Hostert, y and Yu-Dai Tsai z 1Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA 2Institute for Particle Physics Phenomenology, Department of Physics, Durham University, South Road, Durham DH1 3LE, United Kingdom 3Fermilab, Fermi National Accelerator Laboratory, Batavia, IL 60510, USA (Dated: December 5, 2019) Heavy neutrinos with additional interactions have recently been proposed as an explanation to the MiniBooNE excess. These scenarios often rely on marginally boosted particles to explain the excess angular spectrum, thus predicting large rates at higher-energy neutrino-electron scattering experiments. We place new constraints on this class of models based on neutrino-electron scattering sideband measurements performed at MINERνA and CHARM-II. A simultaneous explanation of the angular and energy distributions of the MiniBooNE excess in terms of heavy neutrinos with light mediators is severely constrained by our analysis. In general, high-energy neutrino-electron scattering experiments provide strong constraints on explanations of the MiniBooNE observation involving light mediators. Introduction – Non-zero neutrino masses have been the experiment has observed an excess of νe-like events established in the last twenty years by measurements of that is currently in tension with the standard three- neutrino flavor conversion in natural and human-made neutrino prediction and is beyond statistical doubt at the sources, including long- and short-baseline experiments. 4:7σ level [5]. While it is possible that the excess is fully The overwhelming majority of data supports the three- or partially due to systematic uncertainties or SM back- neutrino framework.
    [Show full text]
  • Miniboone Anomaly and Nuclear Physics 4
    1. MiniBooNE 2. Beam 3. Detector MiniBooNE Anomaly and Nuclear physics 4. Oscillation 5. Discussion PRL121(2018)221801 outline 1. MiniBooNE neutrino experiment 2. Nucleon correlations 3. Pion puzzle 4. NC single photon production 5. Conclusions Teppei Katori Queen Mary University of London ECT* workshop, Trento, Italy, April 15, 2019 Teppei Katori, [email protected] 15/04/19 1 1. MiniBooNE 2. Beam 3. Detector 4. Oscillation 5. Discussion 1. MiniBooNE neutrino experiment 2. Nucleon correlations 3. Pion puzzle 4. NC single photon production 5. Discussions Teppei Katori, [email protected] 15/04/19 2 1. MiniBooNE 2. Beam 3. Detector 4. Oscillation 5. Discussion Teppei Katori, [email protected] 15/04/19 3 1. MiniBooNE 2. Beam 3. Detector 4. Oscillation 5. Discussion The most visible particle physics result of the year Teppei Katori, [email protected] 15/04/19 4 https://physics.aps.org/articles/v11/122 PHYSICAL REVIEW LETTERS 120, 141802 (2018) signature of dark matter annihilation in the Sun [5,6]. 1. MiniBooNE Despite the importance of the KDAR neutrino, it has never MiniBooNE 2. Beam been isolated and identified. 3. Detector 86 m 4. Oscillation In the charged current (CC) interaction of a 236 MeV νμ background KDAR 12 − NuMI 5. Discussion (νμ C → μ X), the muon kinetic energy (Tμ) and closely beam decay pipe related neutrino-nucleus energy transfer (ω E − E ) horns ν μ target distributions are of particular interest for benchmarking¼ absorber neutrino interaction models and generators, which report widely varying predictions for kinematics at these tran- 5 m 675 m sition-region energies [7–14].
    [Show full text]
  • Icecube Sterile Neutrino Searches
    EPJ Web of Conferences 207, 04005 (2019) https://doi.org/10.1051/epjconf/201920704005 VLVnT-2018 IceCube Sterile Neutrino Searches 1, B.J.P. Jones ∗ For the IceCube Collaboration 1University of Texas at Arlington, 108 Science Hall, 502 Yates St, Arlington, TX Abstract. Anomalies in short baseline experiments have been interpreted as evidence for additional neutrino mass states with large mass splittings from the known, active flavors. This explanation mandates a corresponding signa- ture in the muon neutrino disappearance channel, which has yet to be observed. Searches for muon neutrino disappearance at the IceCube neutrino telescope presently provide the strongest limits in the space of mixing angles for eV- scale sterile neutrinos. This proceeding for the Very Large Volume Neutrino Telescopes (VLVnT) Workshop summarizes the IceCube analyses that have searched for sterile neutrinos and describes ongoing work toward enhanced, high-statistics sterile neutrino searches. 1 Introduction Sterile neutrinos are hypothetical particles that have been invoked to explain anomalies in short baseline accelerator decay-at-rest [1] and decay-in-flight experiments [2], reactor neu- trino fluxes [3, 4] and radioactive source experiments [5]. In low-energy, short baseline exper- iments that are sensitive to νe appearance, matter effects can be neglected and an oscillation of the form: 2 2 2 ∆m L Pν ν = sin 2θµe sin (1) µ→ e 4E is predicted. A large ∆m2 thus introduces an oscillation at a small characteristic L/E, with 2 the effective mixing parameter, sin 2θµe governing the amplitude of oscillation. To introduce flavor-change at similar L/E as exhibited in the MiniBooNE and LSND experiments, mixing 2 3 parameters sin 2θµe of 10− or larger are required, with favored parameter space in the one- to-few eV2 mass splittings.
    [Show full text]
  • “ Chamber” Neutrino Physi Years After Gargamelle
    35 years after Gargamelle: the Renaissance of the “ Bubble chamber” neutrino physics Carlo Rubbia CERN, Geneva, Switzerland INFN-Assergi, Italy C. Rubbia, CERN, 0ct09 111 A Gargamelle neutrino event QuickTime™ and a decompressor are needed to see this picture. Charm production in a neutrino interaction The total visible energy is 3.58 GeV. C. Rubbia, CERN, 0ct09 Slide: 2 The path to massive liquid Argon detectors CERN 1 2 Laboratory work CERN CERN 3 T600 detector 4 2001: First T600 module 5 20 m Cooperation with industry C. Rubbia, CERN, 0ct09 Slide: 3 T600 in hall B (CNGS2 -2009) QuickTime™ and a decompressor are needed to see this picture. C. Rubbia, CERN, 0ct09 Slide: 4 Thirty years of progress........ LAr is a cheap liquid Bubble diameter ≈ 3 mm (≈1CHF/litre), vastly (diffraction limited) produced by industry Gargamelle bubble chamber ICARUS electronic chamber “Bubble” size 3 x 3 x 0.3 mm3 T300 real event Medium Heavy freon Medium Liquid Argon Sensitive mass 3.0 ton Sensitive mass Many ktons Density 1.5 g/cm3 Density 1.4 g/cm3 Radiation length 11.0 cm Radiation length 14.0 cm Collision length 49.5 cm Collision length 54.8 cm dE/dx 2.3 MeV/cm dE/dx 2.1 MeV/cm C. Rubbia, CERN, 0ct09 Slide: 5 Summary of LAr TPC performances l Tracking device ØPrecise event topology ØMomentum via multiple scattering l Measurement of local energy deposition dE/dx T300 real event Øe / γ separation (2%X 0 sampling) ØParticle ID by means of dE/dx vs range l Total energy reconstruction of the events from charge integration ØFull sampling, homogeneous calorimeter with excellent accuracy for contained events RESOLUTIONS Low energy electrons: σ(E)/E = 11% / √ E(MeV)+2% Electromagn.
    [Show full text]
  • HARP Targets Pion Production Cross Section and Yield Measurements: Implications for Miniboone Neutrino Flux
    HARP targets pion production cross section and yield measurements: Implications for MiniBooNE neutrino flux A Dissertation Submitted to the Graduate School of the University of Cincinnati in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Department of Physic of the College of Arts and Sciences July 2015 by Don Athula Abeyarathna Wickremasinghe M.Sc., University of Cincinnati, 2011 M.Sc., Norwegian University of Science and Technology (NTNU), 2008 B.Sc., University of Peradeniya, 2002 Committee Chair: Professor Randy A. Johnson © 2015 Don Athula A. Wickremasinghe All Rights Reserved HARP targets pion production cross section and yield measurements: Implications for MiniBooNE neutrino flux Don Athula Abeyarathna Wickremasinghe Abstract The prediction of the muon neutrino flux from a 71.0 cm long beryllium target for the MiniBooNE experiment is based on a measured pion production cross section which was taken from a short beryllium target (2.0 cm thick - 5% nuclear interaction length) in the Hadron Production (HARP) experiment at CERN. To verify the extrapolation to our longer target, HARP also measured the pion production from 20.0 cm and 40.0 cm beryllium targets. The measured production yields, d2N π± (p; θ)=dpdΩ, on targets of 50% and 100% nuclear interaction lengths in the kinematic rage of momentum from 0.75 GeV/c to 6.5 GeV/c and the range of angle from 30 mrad to 210 mrad are presented along with an update of the short target cross sections. The best fitted extended Sanford-Wang (SW) model parameterization for updated short beryllium target π+ production cross section is presented.
    [Show full text]
  • Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory
    Lawrence Berkeley National Laboratory Lawrence Berkeley National Laboratory Title Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory Permalink https://escholarship.org/uc/item/6nk6379r Author Aharmim, B. Publication Date 2009-08-01 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory ! ! ! ! The SNO Collaboration ! ! ! ! ! ! This work was supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. DISCLAIMER This document was prepared as an account of work sponsored by the United States Government. While this document is believed to contain correct information, neither the United States Government nor any agency thereof, nor The Regents of the University of California, nor any of their employees, makes any warranty, express or implied, or assumes any legal responsibility for the accuracy, completeness, or usefulness of any information, apparatus, product, or process disclosed, or represents that its use would not infringe privately owned rights. Reference herein to any specific commercial product, process, or service by its trade name, trademark, manufacturer, or otherwise, does not necessarily constitute or imply its endorsement, recommendation, or favoring by the United States Government or any agency thereof, or The Regents of the University of California. The views and opinions of authors expressed herein do not necessarily state or reflect those of the United States Government or any agency thereof or The Regents of the University of California. Measurement of the Cosmic Ray and Neutrino-Induced Muon Flux at the Sudbury Neutrino Observatory B.
    [Show full text]
  • Miniboone, LSND, and Future Very-Short Baseline Experiments
    1 MiniBooNE, LSND, and Future Very-Short Baseline Experiments Mike Shaevitz - Columbia University BLV2011 - September, 2011 - Gatlinburg, Tennessee Neutrino Oscillation Summary 2 ! µ " ! Sterile " ! e New MiniBooNEνµ consistent OPERA : νµ→ντ ⇒ & ICARUS Confirmed by K2K and Minos accelerator neutrino exps New θ13 Information! νe→νµ / ντ ⇒ Confirmed by Kamland reactor neutrino exp Possible Oscillations to Sterile Neutrinos 3 Sterile neutrinos – Partners to the three standard neutrinos – Have no weak interactions (through the standard W/Z bosons) – Would be produced and decay through mixing with the standard model neutrinos – Are postulated in see-saw models to explain small neutrino masses – Can affect oscillations through mixing Cosmological Constraints NS = # of Thermalized Sterile ν States Oscillation Patterns with Sterile Neutrinos 3 + 1 3 + 2 68%, 95%, 99% CL 4 LSND νµ →νe Signal + + " # µ ! µ + e ! e! µ Saw an excess of: Oscillations? ! e 87.9 ± 22.4 ± 6.0 events. With an oscillation probability of (0.264 ± 0.067 ± 0.045)%. LSND in conjunction with the atmospheric and solar oscillation results needs more than 3 ν’s 3.8 σ evidence for oscillation. ⇒ Models developed with 1 or 2 sterile ν’s The MiniBooNE Experiment 5 at Fermilab LMC + ? K+ µ 8GeV π+ νµ νµ→νe Booster magnetic horn decay pipe absorber 450 m dirt detector and target 25 or 50 m • Goal to confirm or exclude the LSND result - Similar L/E as LSND – Different energy, beam and detector systematics – Event signatures and backgrounds different from LSND • Since August 2002 have
    [Show full text]
  • Neutrino-Nucleus Interactions U
    Neutrino-nucleus interactions U. Mosel and O. Lalakulich Institut für Theoretische Physik, Universität Giessen, Germany Abstract. Interactions of neutrinos with nuclei in the energy ranges relevant for the MiniBooNE, T2K, NOnA, MINERnA and MINOS experiments are discussed. It is stressed that any theoretical treatment must involve all the relevant reaction mechanisms: quasielastic scattering, pion production and DIS. In addition, also many-body interactions play a role. In this talk we show how a misidentification of the reaction mechanism can affect the energy reconstruction. We also discuss how the newly measured pion production cross sections, as reported recently by the MiniBooNE collaboration, can be related to the old cross sections obtained on elementary targets. The MiniBooNE data seem to be compatible only with the old BNL data. Even then crucial features of the nucleon-pion-Delta interaction are missing in the experimental pion kinetic energy spectra. We also discuss the meson production processes at the higher energies of the NOnA, MINERnA and MINOS experiments. Here final state interactions make it impossible to gain knowledge about the elementary reaction amplitudes. Finally, we briefly explore the problems due to inaccuracies in the energy reconstruction that LBL experiments face in their extraction of oscillation parameters. Keywords: Neutrino interactions, Pions, Energy reconstruction PACS: 24.10.Jv,25.30.Pt INTRODUCTION However, the actual reaction mechanism may be sig- nificantly more complicated. There can be events in Investigations of neutrino interactions with nucleons can which first a pion was produced which then got stuck in on one hand give valuable information on the axial prop- the nucleus due to FSI and thus did not get out to the de- erties of the nucleon.
    [Show full text]
  • Arxiv:2008.11851V1 [Hep-Ph] 26 Aug 2020
    FTPI-MINN-20-28 Constraints on Decaying Sterile Neutrinos from Solar Antineutrinos 1, 2, 3, 1, 2 Matheus Hostert ∗ and Maxim Pospelov 1School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA 2William I. Fine Theoretical Physics Institute, School of Physics and Astronomy, University of Minnesota, Minneapolis, MN 55455, USA 3Perimeter Institute for Theoretical Physics, Waterloo, ON N2J 2W9, Canada (Dated: September 9, 2021) Solar neutrino experiments are highly sensitive to sources of ν ν conversions in the 8B neutrino flux. In this work we adapt these searches to non-minimal sterile! neutrino models recently proposed to explain the LSND, MiniBooNE, and reactor anomalies. The production of such sterile neutrinos in the Sun, followed the decay chain ν4 ν' ννν with a new scalar ' results in upper limits 2 ! ! for the neutrino mixing Ue4 at the per mille level. We conclude that a simultaneous explanations of all anomalies is in tensionj j with KamLAND, Super-Kamiokande, and Borexino constraints on the flux of solar antineutrinos. We then present other minimal models that violate parity or lepton number, and discuss the applicability of our constraints in each case. Future improvements can be expected from existing Borexino data as well as from future searches at Super-Kamiokande with added Gd. I. INTRODUCTION The flux of antineutrinos from the Sun at the MeV energies is negligible [18], which remains an excellent ap- Beyond neutrino mixing, the study of solar neutrinos proximation down to tens of keV in energy [19]. Com- provides important input to the standard solar Model bined with the fact that the detection cross section for (SSM) [1,2] and has been used to search for several phe- νe is much larger and easier to measure compared to nomena beyond the SM of particle physics.
    [Show full text]
  • Neutrino Observatory Management & Operations Plan
    IceCube Neutrino Observatory Management & Operations Plan Neutrino Observatory Management & Operations Plan December 2019 Revision 4.0 December 2019 1 IceCube Neutrino Observatory Management & Operations Plan IceCube MANAGEMENT & OPERATIONS PLAN SUBMITTED BY: Francis Halzen Kael Hanson IceCube Principal Investigator Co-PI and IceCube Director of Operations University of Wisconsin–Madison University of Wisconsin–Madison Albrecht Karle Co-PI and Associate Director for Science and Instrumentation University of Wisconsin–Madison James Madsen Associate Director for Education and Outreach University of Wisconsin–River Falls Catherine Vakhnina Resource Coordinator Paolo Desiati Coordination Committee Chair John Kelley Detector Operations Manager Benedikt Riedel Computing and Data Management Services Manager Juan Carlos Diaz-Velez Data Processing and Simulation Services Manager Alex Olivas Software Coordinator Summer Blot, Keiichi Mase Calibration Coordinator December 2019 2 IceCube Neutrino Observatory Management & Operations Plan Revision History Date Section Revision Action Revised Revised 1.0 06/9/2016 First version 2.0 05/31/2017 Updated for M&O PY2 3.0 12/12/2018 Updated for M&O PY3 4.0 03/20/2020 Updated PY4 plan w new Org Chart December 2019 1 IceCube Neutrino Observatory Management & Operations Plan Table of Contents List of Acronyms and Terms ........................................................................................................................ 5 1 Preface .................................................................................................................................................
    [Show full text]
  • Short-Baseline Electron Neutrino Disappearance, Tritium Beta Decay
    arXiv:1005.4599 [hep-ph] Phys.Rev.D82:053005,2010 Short-Baseline Electron Neutrino Disappearance, Tritium Beta Decay and Neutrinoless Double-Beta Decay Carlo Giunti∗ INFN, Sezione di Torino, Via P. Giuria 1, I–10125 Torino, Italy Marco Laveder† Dipartimento di Fisica “G. Galilei”, Universit`adi Padova, and INFN, Sezione di Padova, Via F. Marzolo 8, I–35131 Padova, Italy (Dated: September 26, 2018) We consider the interpretation of the MiniBooNE low-energy anomaly and the Gallium radioac- tive source experiments anomaly in terms of short-baseline electron neutrino disappearance in the framework of 3+1 four-neutrino mixing schemes. The separate fits of MiniBooNE and Gallium data are highly compatible, with close best-fit values of the effective oscillation parameters ∆m2 and sin2 2ϑ. The combined fit gives ∆m2 & 0.1 eV2 and 0.11 sin2 2ϑ 0.48 at 2σ. We consider also the data of the Bugey and Chooz reactor antineutrino≤ oscillation≤ experiments and the limits on the effective electron antineutrino mass in β-decay obtained in the Mainz and Troitsk Tritium experiments. The fit of the data of these experiments limits the value of sin2 2ϑ below 0.10 at 2σ. Considering the tension between the neutrino MiniBooNE and Gallium data and the antineu- trino reactor and Tritium data as a statistical fluctuation, we perform a combined fit which gives 2 2 ∆m 2 eV and 0.01 sin 2ϑ 0.13 at 2σ. Assuming a hierarchy of masses m1,m2,m3 m4, the ≃ ≤ ≤ ≪ predicted contributions of m4 to the effective neutrino masses in β-decay and neutrinoless double- β-decay are, respectively, between about 0.06 and 0.49 and between about 0.003 and 0.07 eV at 2σ.
    [Show full text]
  • Nucleon Correlations in Neutrino Oscillation Experiments
    Nucleon correlations in neutrino oscillation experiments 1. Introduction 2. 2-body current in neutrino interactions 3. Neutrino oscillation experiments 4. Neutrino interaction measurements 5. Conclusion Teppei Katori Queen Mary University of London CLAS data mining group meeting, MIT, MA, USA, Aug. 9, 2014 Teppei Katori 08/09/14 1 Hen et al., arXiv:1407.8175 1. Introduction 2. 2 body current 3. Neutrino oscillation 4. Neutrino interaction 1. Unexpected connection... 5. Conclusion Atomic gas and nuclear gas - They share same property in terms of “contact”. Short range correlation and neutrino oscillation experiments - Significant fraction of interaction(?) - A correct model must be in our simulation Teppei Katori 08/09/14 Formaggio and Zeller, Rev.Mod.Phys.84(2012)1307 1. Introduction 2. 2 body current 3. Neutrino oscillation 4. Neutrino interaction 1. Next generation neutrino oscillation experiments 5. Conclusion Neutrino oscillation experiments - Past to Present: K2K, MiniBooNE, MINOS, T2K - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF T2K MINOS K2K MiniBooNE νµCC cross section per nucleon 2 2 # 2 2 L(km) & Pµ→e (L / E) = sin 2θ sin %1.27Δm (eV ) ( Teppei Katori $08/09/14 E(GeV)' Formaggio and Zeller, Rev.Mod.Phys.84(2012)1307 1. Introduction 2. 2 body current 3. Neutrino oscillation 4. Neutrino interaction 1. Next generation neutrino oscillation experiments 5. Conclusion Typical oscillation experiment Neutrino oscillation experiments (L~100-1000km) always choose - Past to Present: K2K, MiniBooNE, MINOS, T2K 1-10 GeV energy region (only - Present to Future: T2K, NOvA, PINGU, JUNO, HyperK, LBNF exception is reactor neutrino experiment) T2K HyperK NOvA LBNF PINGU νµCC cross section per nucleon 2 2 # 2 2 L(km) & Pµ→e (L / E) = sin 2θ sin %1.27Δm (eV ) ( Teppei Katori $08/09/14 E(G4 eV)' 1.
    [Show full text]