1. Future Directions in Parity Violation: From Quarks to the Cosmos M.J. Ramsey-Musolf + many students, post- docs, collaborators, and colleagues PAVI ‘06 

2. Fundamental Symmetries & Cosmic History What are the fundamental symmetries that have governed the microphysics of the evolving universe? Parity violation as a probe of the proton’s internal structure (sea quarks, twist) Parity violation as probe of the hadronic weak interaction Parity violation as a probe of additional symmetries of the early universe

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

4. Fundamental Symmetries & Cosmic History Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? SM “unfinished business”: What is the internal landscape of the proton? Sea quarks, gluons, & qq, qqg correllations

5. Preliminary Probing the strange sea with PV World Data 4/24/06 G M s = 0.28 +/- 0.20 G E s = -0.006 +/- 0.016 ~3% +/- 2.3% of proton magnetic moment ~20% +/- 15% of isoscalar magnetic moment ~0.2 +/- 0.5% of Electric distribution Courtesy of Kent Pashke (U Mass) Consistent with s-quark contributions to m P & J P but smaller than early theoretical expectations Not surprising: m s /   ~ 0.15 Challenge for lattice: Unquenched, light chiral quarks

6. Probing Higher Twist: Beyond the Parton Model Alekhin NNLO MRST NNLO MRST NNLO with Barbieri Target Mass Corrections Smooth transition from DIS (solid squares) to resonance region Resonances oscillate about perturbative curves (quark- hadron duality in transverse channel) - all Q 2 Target mass corrections large and important 2xF 1 Experimental Status Data from JLab E94-110 (nucl-ex/0410027, submitted to PRL) Courtesy C Keppel ~ 50% fluctuations about leading twist

7. n = 2 Cornwall-Norton Moments FLFLFLFL 2xF 1 F 2, F 1 in excellent agreement with NNLO + TM above Q 2 = 2 GeV 2 No (or canceling) higher twists Yet, dominated by large x and resonance region Remove known HT (a bit novel), the elastic, and there is no more down to Q 2 = 0.5 GeV2 The case looks different for F L (data or curve?) F2F2F2F2 Where are the qq and qqg correlations ?

8. Probing Higher Twist with PV Sacco, R-M preliminary Looking beyond the parton descriptionPV Deep Ineslastic eD (J Lab 12 GeV) ~0.4% E=11 GeV  =12.5 0 Different PDF fits Theoretical Challenges pQCD evolution of twist four moments Lattice QCD for  =4 matrix elements Organizing the program: what kinematics, complementarity with PC F 1,2, …

9. Fundamental Symmetries & Cosmic History Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? SM “unfinished business”: How do weak interactions of hadrons reflect the weak qq force ? Are QCD symmetries (chiral, large N C,…) applicable? Is there a long range weak NN interaction?

10. Weak Interactions of Hadrons: Strange? Hyperon weak decays S-Wave: Parity-violating P-Wave: Parity- conserving  symmetry not sufficient

11. Weak Interactions of Hadrons: Strange? M1 (PC) Th’y Exp’t Breaking of SU(3) sym E1 (PV) Are weak interactions of s-quarks a “un-natural” ? Or are their deeper puzzles with the HWI involving all light flavors ?

12. Weak Interactions of S=0 Hadrons: Strange? PV Asymmetry Q 2 =0: Nonzero PVES: G0, Q WEAK enhanced d  “natural” d  What does QCD predict ?  S=0 analog of  BB’ : PV E1 N-  transition Zhu, Puglia, Holstein, R-M

13. Weak Interactions of S=0 Hadrons: Strange? Use parity-violation to filter out EM & strong interactions Meson-exchange model Seven PV meson- nucleon couplings Desplanques, Donoghue, & Holstein (DDH) Nuclear effects: W,Z ~ 0.002 fm << R core

14. Is the weak NN force short range ? T=1 force T=0 force Long range:  -exchange? Analog 2-body matrix elements Model independent h   ~0 Boulder, atomic PV Anapole moment h   ~ 10 g 

15. Is the weak NN force short range ? T=1 force T=0 force Problem with expt’s Problem with nuc th’y Problem with model No problem (1  ) EFT

16. Hadronic PV: Effective Field Theory PV Potential Long RangeShort RangeMedium Range O (p -1 ) O (p) Six constants to O(p) Zhu, Maekawa, Holstein, R-M, van Kolck ‘05R-M & Page ‘06

17. Hadronic PV: Effective Field Theory PV Current Operators Long RangeMedium Range O (p -1 ) O (p) Short Range One new O(p) constant

18. Hadronic PV: Few-Body Systems  Pionless theory Done NIST,SNS LANSCE, SNSHARD* Ab initio few-body calcs New few-body calcs needed Pionless th’y: 5 exp’ts Dynamical pions: 7 exp’ts

19. Hadronic PV: Theoretical Challenges Attempt to understand the i, h  etc. from QCD Attempt to understand nuclear PV observables systematically Are the PV LEC’s “natural” from QCD standpoint? Does EFT power counting work in nuclei ? Complete determination of PV NN &  NN interactions through O (p) Implications for 0  -decay

20. Hadronic PV &  - decay How do we compute & separate heavy particle exchange effects? Light M : 0  -decay rate may yield scale of m

21. Hadronic PV &  - decay 4 quark operator, as in hadronic PV How do we compute & separate heavy particle exchange effects?

22. Hadronic PV as a probe O ( p -1 ) O ( p ) Determine V PV through O (p) from PV low-energy few-body studies where power counting works Re-analyze nuclear PV observables using this V PV If successful, we would have some indication that operator power counting works in nuclei Apply to  -decay Prezeau, R-M, & Vogel

23. Fundamental Symmetries & Cosmic History Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? Puzzles the Standard Model can’t solve 1.Origin of matter 2.Unification & gravity 3.Weak scale stability 4.Neutrinos What are the symmetries (forces) of the early universe beyond those of the SM?

24. PV as a Probe of New Symmetries Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? Puzzles the Standard Model can’t solve 1.Origin of matter 2.Unification & gravity 3.Weak scale stability 4.Neutrinos What are the implications of m  and PV expts for possible new symmetries & forces?

25. PV as a Probe of New Symmetries Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? Unseen Forces: Supersymmetry ? 1.Unification & gravity 2.Weak scale stability 3.Origin of matter 4.Neutrinos

26. PV Correlations in Muon Decay & m 3/4 0 3/4 1 TWIST (TRIUMF)

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

28. Weak decays & new physics   -decay New physics SUSY Flavor-blind SUSY- breaking CKM, (g-2)   M W, M t,… Kurylov, R-M RPV 12k  1j1 No long-lived LSP or SUSY DM MWMW R Parity Violation CKM Unitarity APV  l2 Kurylov, R-M, Su CKM unitarity ?

29. Weak decays & PV   -decay Liquid N 2 Be reflector Solid D 2 77 K poly Tungsten Target 58 Ni coated stainless guide UCN Detector Flapper valve LHe Ultra cold neutrons LANSCE: UCN “A” NIST, ILL:  n Future SNS:  n, a,b,A,… Future LANSCE:  n Lifetime & correlations

30. Weak decays & PV SUSY Correlations Non (V-A) x (V-A) interactions: m e /E  -decay at “RIAcino”?

31. Weak decays & PV: Correlations  -decay correlations  -decay  - parameter  Fierz int (current)  G F from   Profumo, R-M, Tulin PV w/ radioactive isotopes ?

32. Probing SUSY with PV eN Interactions SUSY loops   -> e  + e   SUSY dark matter Kurylov, Su, MR-M is Majorana RPV 95% CL fit to weak decays, M W, etc. 12k

33. Probing SUSY with PV eN Interactions e p RPV Loops SUSY effects Deep Inelastic eD vs elastic ef

34. Probing SUSY with PV eN Interactions  SUSY dark matter Kurylov, R-M, Su SUSY loops RPV 95% CL E158 &Q- Weak JLab Moller Linear collider “DIS Parity”

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

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

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

38. EDM Probes of New CP Violation f d SM d exp d future CKM If new EWK CP violation is responsible for abundance of matter, will these experiments see an EDM? Also 225 Ra, 129 Xe, d

39. Baryogenesis & Dark Matter: MSSM Neutralino Mass Matrix M1M1 -- M2M2 -m Z cos  sin  W m Z cos  cos  W m Z sin  sin  W -m Z sin  sin  W 0 0 0 0 -- -m Z cos  sin  W m Z cos  cos  W m Z sin  sin  W -m Z sin  sin  W M N = Chargino Mass Matrix M2M2  M C = T << T EW : mixing of H,W to     ~~ ~~ T ~T EW : scattering of H,W from background field ~~ T ~ T EW CPV   B    W    H d    H u   BINOWINOHIGGSINO T << T EW

40. EDM constraints & SUSY CPV AMSB: M 1 ~ 3M 2 Neutralino-driven baryogenesis BaryogenesisLEP II ExclusionTwo loop d e Cirigliano, Profumo, R-M SUGRA: M 2 ~ 2M 1

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

42. EDMs, Baryogenesis, & Dark Matter Continued progress in performing systematic computations of the baryon asymmetry Continued scrutiny of QCD & nuclear structure uncertainties in EDM computations Comprehensive phenomenology with other models of new CPV (extended Higgs sector) Funding for experiments !

43. Future Directions: Parity violation in electron scattering and hadronic interactions will continue to provide new insights into proton’s internal structure and weak qq interactions PV in weak decays and electron scattering will continue to provide insights into new physics (SUSY, ’s, Higgs) that will complement LHC, ILC probes PVTV will provide powerful probe of the origin of baryonic matter and non-baryonic dark matter Considerable theoretical and experimental challenges and opportunities remain: PAVI must go on!