Nuclei & the Cosmos: Symmetries of the Standard Model & Beyond

1. M.J. Ramsey-Musolf Nuclei & the Cosmos: Symmetries of the Standard Model &Beyond S. Profumo S. Su S. Tulin P. Vogel P. Wang M. Wise N. Bell V. Cirigliano J. Erler R. Erwin J. Kile Kurylov C. Lee

2. Cosmic Energy Budget Dark Matter Dark Energy Baryons Nuclear Science The mission: Explain the origin, evolution, and structure of the baryonic matter of the Universe

3. Cosmic Energy Budget Dark Matter Dark Energy Baryons • Three frontiers: • Fundamental symmetries & neutrinos • Nuclei and nuclear astrophysics • QCD Nuclear Science

4. Fundamental Symmetries & Cosmic History • What were the fundamental symmetries that governed the microphysics of the early universe? • What insights can low energy (E << MZ) precision nuclear physics studies provide?

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

6. Electroweak symmetry breaking: Higgs ? 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?

7. Cosmic Energy Budget Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History Baryogenesis: When? CPV? SUSY? Neutrinos? WIMPy D.M.: Related to baryogenesis? “New gravity”? Lorentz violation? Effects on CMB? ?

8. Present universe Early universe Standard Model High energy desert Weak scale Planck scale Fundamental Symmetries & Cosmic History

9. Present universe Early universe Standard Model Gravity A “near miss” for grand unification Is there unification? What new forces are responsible ? High energy desert Weak scale Planck scale Fundamental Symmetries & Cosmic History

10. Present universe Early universe Unification Neutrino mass Origin of matter Standard Model Weak scale unstable: Why is GF so large? High energy desert Weak scale Planck scale Fundamental Symmetries & Cosmic History

11. Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History Neutrinos ? Are they their own antiparticles? Why are their masses so small? Can they have magnetic moments? Implications of mnfor neutrino interactions ?

12. Supersymmetry, GUT’s, extra dimensions… There must have been additional symmetries in the earlier Universe to • Unify all matter, space, & time • Stabilize the weak scale • Produce all the matter that exists • Account for neutrino properties • Give self-consistent quantum gravity

13. Large Hadron Collider Ultra cold neutrons LANSCE, NIST, SNS, ILL CERN What are the new fundamental symmetries? Two frontiers in the search Collider experiments (pp, e+e-, etc) at higher energies (E >> MZ) Indirect searches at lower energies (E < MZ) but high precision Particle, nuclear & atomic physics High energy physics

14. What are the new fundamental symmetries? • Why is there more matter than antimatter in the present universe? • What are the unseen forces that disappeared from view as the universe cooled? • What are the masses of neutrinos and how have they shaped the evolution of the universe? Electric dipole moment searches Precision electroweak: weak decays, scattering, LFV Neutrino oscillations, 0nbb-decay, q13 , … Tribble report

15. Cosmic Energy Budget Dark Matter BBN WMAP Searches for permanent electric dipole moments (EDMs) of the neutron, electron, and neutral atoms probe new CP-violation Dark Energy T-odd , CP-odd by CPT theorem Baryons What are the quantitative implications of new EDM experiments for explaining the origin of the baryonic component of the Universe ? What is the origin of baryonic matter ?

16. Present universe Early universe ? ? Weak scale baryogenesis can be tested experimentally Weak scale Planck scale EDMs & Baryogenesis Sakharov Criteria • B violation • C & CP violation • Nonequilibrium dynamics Sakharov, 1967

17. Present universe Early universe Key Ingredients • Heavy nR • mn spectrum • CP violation • L violation Leptogenesis b-decay, 0n bb-decay, q13 Weak scale Planck scale Leptogenesis

18. Weak Scale Baryogenesis • B violation • C & CP violation • Nonequilibrium dynamics Sakharov, 1967 Kuzmin, Rubakov, Shaposhnikov McLerran,… EW Baryogenesis: Standard Model Anomalous Processes Different vacua: D(B+L)= DNCS Sphaleron Transitions

19. Shaposhnikov Weak Scale Baryogenesis • B violation • C & CP violation • Nonequilibrium dynamics 1st order 2nd order Sakharov, 1967 • CP-violation too weak • EW PT too weak Increasing mh EW Baryogenesis: Standard Model

20. 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

21. CKM fdSM dexp dfuture 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

22. Better theory Present n-EDM limit Proposed n-EDM limit Matter-Antimatter Asymmetry in the Universe ? M. Pendlebury B. Filippone Riotto; Carena et al.; Lee, Cirigliano, R-M, Tulin “n-EDM has killed more theories than any other single experiment”

23. CPV phases Parameters in Lnew Bubble & PT dynamics Departure from equilibrium • Earliest work: QM scattering & stat mech • New developments: non-equilibrium QFT Systematic Baryogenesis Goal: Derive dependence of YB on parameters Lnew systematically (controlled approximations)

24. Unbroken phase Topological transitions Broken phase nL produced in wall & diffuses in front 1st order phase transition FWS(x) !0 deep inside bubble Systematic Baryogenesis Cohen, Kaplan, Nelson Joyce, Prokopec, Turok “snow”

25. Unbroken phase Topological transitions … + Compute from first principles given Lnew Broken phase 1st order phase transition = + + Expansion in scale ratios Systematic Baryogenesis Riotto Carena et al Lee, Cirigliano, Tulin, R-M Quantum Transport Equation Schwinger-Dyson Equations

26. Fermions Bosons sfermions gauginos Higgsinos Charginos, neutralinos SUSY: a candidate symmetry of the early Universe Supersymmetry

27. SUSY and R Parity If nature conserves vertices have even number of superpartners • Lightest SUSY particle is stable viable dark matter candidate • Proton is stable • Superpartners appear only in loops Consequences

28. 1st order 2nd order Increasing mh How is electroweak symmetry broken? (LCH, ILC) 1st order PT in MSSM: mh < 120 GeV mh>114.4 GeV Constraint on mhrelaxed for larger gauge/Higgs sector (NMSSM, etc.) or ~ 90 GeV (SUSY) Systematic Baryogenesis: MSSM LEP EWWG See, e.g., Kang et al for U(1)’

29. fm , fA Systematic Baryogenesis: MSSM SUSY mass parameter MSSM EWB: Higgsino-Gaugino driven Soft SUSY-breaking mass parameters

30. M1 0 -mZ cosb sinqW mZ cosb cosqW T ~TEW : scattering of H,W from background field MN = ~ ~ mZ sinb sinqW M2 -mZ sinb sinqW 0 0 -m -mZ cosb sinqW mZ cosb cosqW -m T << TEW : mixing of H,W to c+, c0 mZ sinb sinqW -mZ sinb sinqW 0 ~ ~ ~ ~ M2 MC = m Systematic Baryogenesis: MSSM Chargino Mass Matrix Neutralino Mass Matrix

31. Near degeneracies resonances BBN WMAP de de 199Hg 199Hg BAU BAU Lee et al EDM constraints & SUSY CPV Different choices for SUSY parameters

32. Dark Matter Constraints Future: EDMs & LHC de dn BBN WMAP Disfavored Large Hadron Collider Large Hadron Collider Lee, Cirigliano, R-M EDM constraints & SUSY CPV Non-equilibrium QFT

33. Neutralino-driven baryogenesis Baryogenesis LEP II Exclusion Two loop de Cirigliano, Profumo, R-M SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 EDM constraints & SUSY CPV

34. M1 0 -mZ cosb sinqW mZ cosb cosqW MN = mZ sinb sinqW M2 -mZ sinb sinqW 0 0 -m -mZ cosb sinqW mZ cosb cosqW -m T << TEW : mixing of H,W to c+, c0 mZ sinb sinqW -mZ sinb sinqW 0 ~ ~ ~ ~ • = N11B 0 + N12W 0 + N13Hd0 + N14Hu0 BINO WINO HIGGSINO + res + coannihilation Relic Abundance of SUSY DM Neutralino Mass Matrix

35. Neutralino-driven baryogenesis suppressed too fast LEP II Exclusion Non-thermal c0 Cirigliano, Profumo, R-M SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 Dark Matter: Relic Abundance

36. Neutralino-driven baryogenesis Cirigliano, Profumo, R-M SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 Dark Matter: Neutrinos in the Sun

37. Cirigliano, Profumo, R-M Dark Matter: Future Experiments

38. Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History New “Hidden” Forces: Supersymmetry ? Unification & gravity Weak scale stability Origin of matter Neutrinos

39. = 1 SM Expt Weak decays

40. LANSCE, NIST, SNS, ILL, LBL, TAMU, PSI, ANL,…. b-decay SUSY Loops Weak decays

41. Details: question period kaon decay Value of Vusimportant New physics: too small Weak decays

42. b-decay SUSY loops SUSY Weak decays & SUSY

43. Vertex & External leg Kurylov, R-M Drm SUSY Radiative Corrections Propagator Box

44. SUSY Breaking Superpartners have not been seen Theoretical models of SUSY breaking Visible World Hidden World Flavor-blind mediation Can we test models of SUSY breaking mediation ? SUSY must be a broken symmetry

45. Flavor-blind SUSY-breaking 12k R ParityViolation Kurylov, R-M, Su CKM Unitarity MW CKM, (g-2)m, MW, Mt ,… APV l2 b-decay 12k 1j1 1j1 No long-lived LSP or SUSY DM SUSY loops Kurylov, R-M RPV SUSY Weak decays & SUSY

46. CKM Summary: PDG04 UCNA

47. Vus & Vud theory ? New 0+ info CKM Summary: New Vus & tn ? New tn !! UCNA

48. “Weak Charge” ~ 1 - 4 sin2 qW ~ 0.1 Probing SUSY with Lepton Scattering Parity-Violating electron scattering

49. Atomic PV N deep inelastic sin2W e+e- LEP, SLD SLAC E158 (ee) JLab Q-Weak (ep) (GeV) Weak Mixing Angle: Scale Dependence Czarnecki, Marciano Erler, Kurylov, MR-M

50. Vertex & External leg Kurylov, R-M, Su SUSY Radiative Corrections Propagator Box