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Origin of Neutrino Mass: Will We Ever Know?

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Origin of Neutrino Mass: Will We Ever Know? Origin of neutrino mass: will we ever know? Ray Volkas School of Physics The University of Melbourne CERN Theory Colloquium at “Neutrinos: the quest for a new physics scale”, 29 March 2017. 1. What we know, don’t know and want to know. 2. Theνexperimental program. 3. Schemes for Majoranaνmass generation: A. Type-1,2,3 seesaw models. B. Inverse and linear seesaw mechanisms. C. Radiative neutrino mass models. 4. Beyond theνexperimental program. 5. Will we ever know? 1. What we know, don’t know and want to know. On the origin of mass in general: A. Nucleon mass QCD field energy. Non-perturbative. Dynamical chiral symmetry breaking. Fundamental parameter is ΛQCD ~ 220 MeV. Dimensional transmutation. Low masses of pions are Credit: universe-review.ca understood. B. Quark, charged-lepton, W, Z masses Higgs-induced spontaneous EW symmetry breaking. Tree-level perturbative. Fundamental parameter is Higgs VEV ~ 250 GeV. W, Z, t masses are near this scale. Others a lot smaller: ascribed to small Yukawa coupling constants. C. Dark matter mass(es) Unknown. Speculations range from 10-5 eV axions to 105 solar mass primordial black holes! But we do know that ρdark ≈ 5ρbaryon. If ρi= mi ni then this observation suggests ndark ~ nbaryon and mdark ~ mproton – asymmetric dark matter. Is mdark explained by strong QCD-like dynamics? D. Neutrino masses (and mixings) We have now measured some, but not all, neutrino parameters quite precisely. Review in coming slides. Credit: Mainz U The absolute neutrino mass scale has a lab upper limit of 2 eV and cosmo limit of about 0.2 eV. How do nu masses arise, and why are they so small? Credit: KATRIN Recent global fits to neutrino flavour-transformation data: Esteban+ 1611.01514, JHEP 1701 (2017) 087 Capozzi+ 1601.07777, NPB 908 (2016) 218 Forero+ 1405.7540, PRD90 (2014) 093006 Definition of PMNS matrix: ⌫e Ue1 Ue2 Ue3 ⌫1 ⌫1,2,3 mass Δm2 = solar ⌫ = U U U ⌫ 12 µ µ1 µ2 µ3 2 estates Δm2 ~Δm2 = atmos. 2 3 2 3 2 3 32 31 ⌫⌧ U⌧1 U⌧2 U⌧3 ⌫3 m1,2,3 4 5 4 5 4 5 Standard parameterisation: iδ c12c13 s12c13 s13e− 10 0 s c c s s eiδ c c s s s eiδ s c 0 ei↵1/2 0 2 − 12 23 − 12 23 13 12 23 − 12 23 13 23 13 3 2 3 s s c c s eiδ c s s c s eiδ c c 00ei↵2/2 12 23 − 12 23 13 − 12 23 − 12 23 13 23 13 4 5 4 5 ✓12 = solar angle δ = Dirac phase ✓ = atmospheric angle 23 ↵1,2 = Majorana phases ✓13 = reactor angle Oscillation probability formula: 2 2 ∆mijL P↵ β = δ↵ 4 Re(U↵⇤iUβiU↵jUβ⇤j)sin ! − 4E i>j ! X 2 ∆mijL +2 Im(U ⇤ U U U ⇤ )sin ↵i βi ↵j βj 2E i>j ! X ∆m2 m2 m2 ij ⌘ i − j ∆m2L ∆m2 L GeV 1.27 4E ' eV2 km E From the most recent global fit (Esteban+): Interesting preference for δ≈ 270°. A selection of what we don’t know: • Dirac or Majorana? • The value of absolute neutrino mass scale. • Leptonic CP violation not quite confirmed. • Normal or inverted ordering? • θ23 < π/4 or > π/4? • Whether or not the LSND/MiniBooNE, reactor and gallium anomalies are due to eV-scale sterile neutrinos. • The origin of the neutrino mass scale. • Are the mixing parameters and mass splittings free parameters, or is there a flavour symmetry or some other deep dynamics? • Is lepton mass/mixing connected to quark mass/mixing? • Is neutrino mass tree-level or radiative? • What role does the 126 GeV Higgs play in neutrino mass? • Are there other as-yet undiscovered particles that play a role in neutrino mass generation? • Is dark matter a 10 keV-scale sterile neutrino? • Did leptogenesis seed baryogenesis? • And so on. Ultimate goal has to be = + + LBSM LSM L⌫ mass LDM,Bgen,inflation,... where “ν mass” may contain DM and/or Bgen. All we can put in current textbooks is a bunch of empirical facts and a plethora of theoretical speculations. By the way, just in case it is necessary, I want to ν convince you of something: The discovery of mass is most certainly the discovery of new physics. Sometimes you hear the view, “We always expected neutrinos to have mass, so what’s the big deal?” As everyone knows, the original SM has no RH neutrinos, no Y=2 Higgs triplet, and nothing else that breaks Le,μ,τor Ltot, so neutrinos are exactly massless.1 Massive neutrinos may be Dirac or Majorana. If neutrinos are Majorana, they are the first such states to be discovered: new physics. If neutrinos are Dirac, then the gauge-invariant RH neutrino Majorana mass terms must be omitted. This means a global symmetry – U(1)L – must be imposed: a new principle, hence new physics. Also: RH neutrinos are new dofs, like any new particles: new physics. Majorana mass generation requires RH neutrinos or a Y=2 Higgs triplet, or any of a bunch of other new particles: new physics. 1. Exercise for the listener: do sphalerons generate neutrino masses? 2. The neutrino experimental program NEMO Double Beta Decay (82Se, 100Mo, 150Nd) (Home, INSPIRE) References Experiments FNAL-E-0531 Accelerator SBL Oscillations (INSPIRE) References NEOS Reactor Short-Baseline Oscillations (INSPIRE) References FNAL-E-0613 Accelerator SBL Oscillations (INSPIRE) References Filter this page Neutrino-4 Reactor SBL Oscillations (INSPIRE) References (Note: The process can take some time.) Frejus Atmospheric Neutrinos, Proton Decay (INSPIRE) References 136 51 NEXT Double Beta Decay ( Xe) (Home) References Search Reset GALLEX Solar Neutrinos, SBL Oscillations with Cr Neutrino Source (Home, INSPIRE) Thanks to Carlo References NOMAD Accelerator SBL Oscillations (Home, INSPIRE) References Types of Neutrino Experiments Gargamelle Accelerator SBL Oscillations, Neutrino Interactions (INSPIRE) References NOVA Accelerator Long Baseline Oscillations (Home, INSPIRE) References Giunti for keeping Accelerator Beam Dump Astrophysical Neutrinos Atmospheric Neutrinos 187 Genova Re Electron Neutrino Mass (Home, INSPIRE) References Nucifer Reactor SBL Oscillations (INSPIRE, Wikipedia) References Electron Neutrino Long-Baseline Neutrino Oscillations Muon Neutrino GERDA Double Beta Decay (76Ge) (Home) References NUSEX Atmospheric Neutrinos, Proton Decay (INSPIRE) References a nice … long list! Neutrinoless Double Beta Decay Short-Baseline Neutrino Oscillations Solar Neutrinos GEMMA Reactor Electron Antineutrino - Electron Scattering References NuTeV Accelerator Muon Neutrino - Nucleon Scattering (Home, INSPIRE) References Supernova Neutrinos Tau Neutrino GLUE High-Energy Astrophysical Neutrinos (Home, INSPIRE) References OPERA Accelerator Long Baseline Oscillations (Home, INSPIRE) References EXPAND ALL COMPRESS ALL GNO Solar Neutrinos (Home, INSPIRE) References Palo Verde Reactor Long Baseline Oscillations (Home, INSPIRE) References Neutrino Experiments Gosgen Reactor SBL Oscillations (INSPIRE) References RENO Reactor LBL Oscillations (Home) References Future experiments AMANDA High-Energy Astrophysical Neutrinos, Supernova Neutrinos (Home, INSPIRE) Gotthard Double Beta Decay (136Xe) (Home) References References RICE High-Energy Astrophysical Neutrinos, Supernova Neutrinos (Home, INSPIRE) References Heidelberg-Moscow Double Beta Decay (76Ge) (Home) References ANTARES High-Energy Astrophysical Neutrinos (Home, INSPIRE) References constitute another Rovno Reactor SBL Oscillations (INSPIRE) References Solar Neutrinos (INSPIRE) References ARIANNA High-Energy Astrophysical Neutrinos (Home, INSPIRE) References Homestake SAGE Solar Neutrinos (Home, INSPIRE) References ArgoNeuT Neutrino Interactions (INSPIRE) References ICARUS Accelerator Long Baseline Oscillations, Supernova Neutrinos, Proton Decay (Home, long, but shorter, list. INSPIRE) References Reactor SBL Oscillations (INSPIRE) References Baikal High-Energy Astrophysical Neutrinos, Supernova Neutrinos (Home, INSPIRE) Savannah River References IceCube High-Energy Astrophysical Neutrinos (Home, INSPIRE) References SciBooNE Accelerator Muon Neutrino - Nucleon Scattering (Home, INSPIRE) Baksan Atmospheric and Supernova SN1987A Neutrinos (Home, INSPIRE) References IGEX Double Beta Decay (76Ge) (INSPIRE) References References BOREXino Solar Neutrinos (Home, INSPIRE) References IHEP-JINR Accelerator SBL Oscillations, Neutrino-Nucleon Interactions (INSPIRE) SKAT Accelerator SBL Oscillations, Neutrino-Nucleon Interactions (INSPIRE) References References BEBC Accelerator SBL Oscillations, Neutrino Interactions (INSPIRE) References ILL Reactor SBL Oscillations (INSPIRE) References SNO Solar and Supernova Neutrinos (Home, INSPIRE) References BNL-E-734 Neutrino Interactions (INSPIRE) References 150 IMB Atmospheric Neutrinos, Supernova SN1987A Neutrinos, Proton Decay (Home, INSPIRE) SNO+ Neutrinoless Double Beta Decay ( Nd), Solar, Reactor, Geo and Supernova Neutrinos BNL-E-776 Accelerator SBL Oscillations (INSPIRE) References References (Home) References 116116 BNL-E-816 Accelerator SBL Oscillations (INSPIRE) References K2K Accelerator Long Baseline Oscillations (Home, INSPIRE) References Solotvina Double Double Beta Beta Decay Decay ( ( Cd)Cd) References References Kamiokande Solar, Atmospheric and Supernova SN1987A Neutrinos, Proton Decay (Home, Soudan 2 Atmospheric Neutrinos, Proton Decay (Home, INSPIRE) References Bugey Reactor SBL Oscillations (INSPIRE) References INSPIRE) References Super-Kamiokande Solar and Atmospheric Neutrinos, Proton Decay (Home, INSPIRE) Accelerator SBL Oscillations, Muon Neutrino - Nucleon Scattering (Home, INSPIRE) KamLAND Reactor Long Baseline Oscillations, Supernova Neutrinos (Home, INSPIRE) CCFR References References References KamLAND-Zen Double Beta Decay (136Xe) (Home) References T2K Accelerator Long Baseline Oscillations (Home, INSPIRE) References CDHSW Accelerator SBL Oscillations, Muon Neutrino - Nucleon Scattering (INSPIRE) References KARMEN Accelerator SBL
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