Nuclear Science & the New Standard Model: Neutrinos & Fundamental Symmetries in the Next Decade

1. The next decade presents NP with a unique opportunity to build on this legacy in developing the “new Standard Model” The value of our contribution will be broadly recognized outside the field Nuclear physics studies of ns & fundamental symmetries played an essential role in developing & confirming the Standard Model Our role has been broadly recognized within and beyond NP Nuclear Science & the New Standard Model: Neutrinos & Fundamental Symmetries in the Next Decade Fifty years of PV in nuclear physics Solar ns & the neutrino revolution Michael Ramsey-Musolf, INPC 2007

2. Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History

3. Big Bang Nucleosynthesis (BBN) & light element abundances • Weak interactions in stars & solar burning • Supernovae & neutron stars It utilizes a simple and elegant symmetry principle SU(3)c x SU(2)L x U(1)Y to explain the microphysics of the present universe Standard Model puzzles Standard Model successes Fundamental Symmetries & Cosmic History

4. Electroweak symmetry breaking: Higgs ? • Supersymmetry ? • New gauge interactions? • Extra dimensions ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History Puzzles the Standard Model can’t solve Origin of matter Unification & gravity Weak scale stability Neutrinos What are the symmetries (forces) of the early universe beyond those of the SM?

5. Two frontiers in the search for new physics Collider experiments (pp, e+e-, etc) at higher energies (E >> MZ) Indirect searches at lower energies (E < MZ) but high precision Large Hadron Collider Ultra cold neutrons CERN Particle, nuclear & atomic physics High energy physics Opportunity: Unique role for low energy studies in the LHC era (and beyond!)

6. What are the masses of neutrinos and how have they shaped the evolution of the universe? 0nbb decay, q13, b decay,… • Why is there more matter than antimatter in the present universe? EDM, DM, LFV, 0nbb, q13 … • What are the unseen forces that disappeared from view as the universe cooled? Weak decays, PVES, gm-2,… Tribble report Primary Scientific Questions

7. Specific Opportunities • Major Discovery Potential: 0nbb-decay & EDM • Precision measurements Neutrino mixing & hierarchy Weak decays, PVES, gm-2 • Electroweak probes of QCD PVES, Hadronic PV, nN scatt…

8. Cosmic Energy Budget Electroweak symmetry breaking: Higgs ? Leptogenesis: discover the ingredients: LN- & CP-violation in neutrinos Weak scale baryogenesis: test experimentally: EDMs Nuclear Science mission: explain the origin, evolution, & structure of the baryonic component Beyond the SM SM symmetry (broken) The Origin of Matter & Energy Baryogenesis: When? CPV? SUSY? Neutrinos? ?

9. Present universe Early universe ? ? Weak scale Planck scale Baryogenesis: Ingredients Sakharov Criteria • B violation • C & CP violation • Nonequilibrium dynamics Sakharov, 1967

10. Present universe Early universe Key Ingredients • Heavy nR • mn spectrum • CP violation • L violation Leptogenesis Out of equilibrium decays Particle-Antiparticle asym L violation B violation 0n bb-decay,, b-decay, q13 ,… Weak scale Planck scale Leptogenesis

11. Theory Challenge: matrix elements+ mechanism Long baseline b-decay ? ? 0nbb-Decay: LNV? Mass Term? Dirac Majorana

12. 0nbb signal equivalent to degenerate hierarchy l111/ ~ 0.06 for mSUSY ~ 1 TeV Loop contribution to mn of inverted hierarchy scale 0nbb: Mechanism & mn Impt to know if RPV interactions exist and, if so, what magnitude

13. Present universe Early universe ? ? Bm!e R = Bm!eg Weak scale Planck scale Lepton Flavor & Number Violation MEG: Bm!eg ~ 5 x 10-14 Mu2e: Bm!e ~ 5 x 10-17 Also PRIME

14. 0nbb decay Light nM exchange ? m!eg m!e LFV Probes of RPV: LFV Probes of RPV: Heavy particle exchange ? lk11/ ~ 0.09 for mSUSY ~ 1 TeV lk11/ ~ 0.008 for mSUSY ~ 1 TeV Low scale LFV: R ~ O(1) GUT scale LFV: R ~ O(a) Lepton Flavor & Number Violation Raidal, Santamaria; Cirigliano, Kurylov, R-M, Vogel MEG: Bm!eg ~ 5 x 10-14 Logarithmic enhancements of R Mu2e: Bm!e ~ 5 x 10-17

15. Weak Scale Baryogenesis • B violation • C & CP violation • Nonequilibrium dynamics Topological transitions Broken phase 1st order phase transition Sakharov, 1967 • Is it viable? • Can experiment constrain it? • How reliably can we compute it? Baryogenesis: New Electroweak Physics 90’s: Cohen, Kaplan, NelsonJoyce, Prokopec, Turok Unbroken phase CP Violation

16. Yale, Indiana, Amherst ANL, Princeton, TRIUMF, KVI… SNS, ILL, PSI CKM fdSM dexp dfuture BNL Also 225Ra, 129Xe, d If new EWK CP violation is responsible for abundance of matter, will these experiments see an EDM? EDM Probes of New CP Violation

17. QCD QCD QCD EDMs: New CPV? Improvements of 102 to 103 Electron Neutron Neutral Atoms Deuteron

18. dn similar Theory progress & challenge: refined computations of baryon asymmetry & EDMs baryogenesis LHC reach LHC reach ILC reach LEP II excl Present de Present de Present de Prospective de Prospective de Prospective de Baryogenesis: EDMs & Colliders

19. Electroweak symmetry breaking: Higgs ? ? Beyond the SM SM symmetry (broken) Precision Probes of New Symmetries New Symmetries Origin of Matter Unification & gravity Weak scale stability Neutrinos

20. Daya Bay T2K Double Chooz Mini Boone Precision Neutrino Property Studies Mixing, hierarchy, & CPV Long baseline oscillation studies: CPV? Normal or Inverted ?

21. EM vs. n luminosity: MNSP unitarity? Solar model? High energy solar ns DM + EWB Ice Cube Precision Neutrino Property Studies Solar Neutrinos KamLAND Borexino CLEAN LENS

22. mn< 10-14mB Dirac mnem< 10-9-10-12mB Majorana Neutrino Mass & Magnetic Moments Bell, Cirigliano, Gorshteyn,R-M, Vogel, Wang, Wise Davidson, Gorbahn, Santamaria How large is mn ? Experiment: mn< (10-10 - 10-12) mB e scattering, astro limits Radiatively-induced mn Both operators chiral odd

23. Correlations b-decay SUSY models Vud from neutron decay: ILL, LANSCE, SNS, NIST Similarly unique probes of new physics in muon and pion decay TRIUMF & PSI CKM, (g-2)m, MW, Mt Non (V-A) x (V-A) interactions: me/E New physics SUSY SNS, NIST, LANSCE, RIA? Weak decays & new physics

24. mn MPs Constraints on non-SM Higgs production at ILC: mn , m- and b-decay corr constrained by mn Also b-decay, Higgs production Erwin, Kile, Peng, R-M 06 Prezeau, Kurylov 05 First row CKM Correlations in Muon Decay & mn Model Independent Analysis 2005 Global fit: Gagliardi et al. Model Dependent Analysis

25. JLab Future SLAC Moller Z0 pole tension Parity-violating electron scattering Scale-dependence of Weak Mixing Weak Mixing in the Standard Model

26. Moller (ee) RPV: No SUSY DM Majorana n s SUSY Loops Q-Weak (ep) d QWP, SUSY / QWP, SM d QWe, SUSY / QWe, SM gm-2 12 GeV 6 GeV E158 Probing SUSY with PV Electron Scattering

27. p g Z m m Had VP Had LbL QED Weak SUSY Loops SM Loops Future goal Muon Anomalous Magnetic Moment ~ 3.4 s !

28. Critical role for the international NP community ! 0nbb: Cuore Majorana Moon GERDA… EDM: nEDM atomic dEDM Neutrinos: b-decay Reactor n’s n mag mom Precision:Muon g-2 PVES b,m decay Baryon asymmetry? Uncovering the New Standard Model Lepton Number Violation ? Neutrino Mass ? Mixing ? Sterile n’s ? What is the New Standard Model ? New Forces? Weak Scale CP- Violation ? Supersymmetry ? Extra Dimensions ? Baryon asymmetry?

29. Back Matter

30. Flavor Sym Flavor Antisym Neutrino Mass & Magnetic Moments Majorana vs Dirac mn ? Effective theory for E < L Dirac: Majorana:

31. Anom Dim Antisym in Yukawas Neutrino Mass & Magnetic Moments Majorana vs Dirac mn ? Naturalness bounds on CW,B Dirac: Majorana: 7D mixing 5D matching