1. Nuclei as Laboratories: Nuclear Tests of Fundamental Symmetries M.J. Ramsey-Musolf N. Bell V. Cirigliano J. Erler B. Holstein A. Kurylov C. Lee C. Maekawa S. Page G. Prezeau S. Profumo S. Tulin B. Van Kolck P. Vogel S. Zhu

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

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

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

5. Fundamental Symmetries & Cosmic History Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? Standard Model “unfinished business” How does QCD affect the weak qq interaction? Is there a long range weak NN interaction?

6. 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?

7. 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, 0  -decay,  13, … Tribble report

8. 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

9. What is the origin of baryonic matter? Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? Cosmic Energy Budget ? Baryogenesis: When? SUSY? Neutrinos? CPV? Weak scale baryogenesis can be tested by exp’t If ruled out: more speculative ideas ( ’s) ?

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

11. EW Baryogenesis: Standard Model Weak Scale Baryogenesis B violation C & CP violation Nonequilibrium dynamics Sakharov, 1967 Increasing m h 1st order2nd order CP-violation too weak EW PT too weak Shaposhnikov

12. 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

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

14. BAU dede dede 199 Hg WMAP BBN Different choices for SUSY parameters Lee et al EDM constraints & SUSY CPV EDMs of different systems provide complementary probes: more atomic experiments (RIA) Nuclear theory: reliable calc’s of atomic EDM dependence on  CPV and other new physics parameters (RIA?) Nuclear theory: reliable calcs of Y B

15. Fundamental Symmetries & Cosmic History 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

16. 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 ?

17. Weak decays   -decay SM theory input Recent Marciano & SirlinNuclear structure effects?

18. Weak decays & new physics SUSY Correlations Non (V-A) x (V-A) interactions: m e /E  -decay at RIA?

19. Fundamental Symmetries & Cosmic History Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? Neutrinos ? Are they their own antiparticles? Why are their masses so small? Can they have magnetic moments? Implications of m  for neutrino interactions ? LFV & LNV ? What is m  ?

20.  - decay probes the charge conjugation properties of the neutrino Light M : Nuclear matrix elements difficult to compute

21.  - decay: heavy particle exchange How do we compute & separate heavy particle exchange effects?

22. LF and LN: symmetries of the early universe? Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? MEG: B  !e  ~ 5 x 10 -14 MECO: B  !e ~ 5 x 10 -17 Also PRIME ? R = B!eB!e B!eB!e Lepton flavor: “accidental” symmetry of the SM LFV initimately connected with LNV in most models

23. LF and LN: symmetries of the early universe? Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? MEG: B  !e  ~ 5 x 10 -14 MECO: B  !e ~ 5 x 10 -17 Also PRIME ? 0  decay Light M exchange ? Heavy particle exchange ? Logarithmic enhancements of R Low scale LFV: R ~ O(1) GUT scale LFV: R ~ O 

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

25.  - decay: effective field theory We have a clear separation of scales L-violating new physics Non-perturbative QCD Nuclear dynamics

26.  - decay in effective field theory Operator classification L (q,e) ! L ,N,e  Spacetime & chiral transformation properties

27.  - decay in effective field theory Operator classification L (q,e) = e.g.  - decay: a = b = +

28.  - decay in effective field theory Operator classification Chiral transformations: SU(2) L x SU(2) R Parity transformations: q L $ q R  - decay: a = b = +

29.  - decay in effective field theory Systematic operator classification K  , K  NN, K NNNN can be O ( p 0 ), O ( p 1 ), etc. O (p -2 ) for O (p 0 ) for Enhanced effects for some models ?

30. An open question Is the power counting of operators sufficient to understand weak matrix elements in nuclei ? 76 Ge 76 Se

31. An open question Is the power counting of operators sufficient to understand weak matrix elements in nuclei ? naive etc.

32. An open question Complications: Bound state wavefunctions (e.g., h.o.) don’t obey simple power counting Configuration mixing is important in heavy nuclei More theoretical study required (RIA) Hadronic PV may provide an empirical test Is the power counting of operators sufficient to understand weak matrix elements in nuclei ?

33. Fundamental Symmetries & Cosmic History Beyond the SMSM symmetry (broken) Electroweak symmetry breaking: Higgs ? Standard Model “unfinished business” How does QCD affect the weak qq interaction? Is there a long range weak NN interaction?

34. The weak qq force is short range Use parity-violation to filter out EM & strong interactions Meson-exchange model Seven PV meson- nucleon couplings Desplanques, Donoghue, &Holstein (DDH)

35. Is the weak NN force short range ? T=1 force T=0 force Long range:  -exchange?

36. Is the weak NN force short range ? T=1 force T=0 force Analog 2-body matrix elements Model independent

37. Is the weak NN force short range ? Boulder, atomic PV Anapole moment T=1 force T=0 force h   ~ 10 g 

38. 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

39. Hadronic PV: Effective Field Theory PV Potential Long RangeShort RangeMedium Range O (p -1 ) O (p)

40. A program of few-body measurements  Pionless theory Done NIST LANSCEHARD**HIGS Ab initio few-body calcs

41. A program of few-body measurements Attempt to understand the i, h  etc. from QCD Attempt to understand nuclear PV observables systematically Are the PV LEC’s “natural”? Does EFT power counting work in nuclei ? Complete determination of PV NN &  NN interactions through O (p) Hadronic PV in n-rich nuclei ?

42. 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

43. Conclusions Nuclei provide unique and powerful laboratories in which to probe the fundamental symmetries of the early universe RIA will provide opportunities to carry out new and complementary experiments whose impact can live on well into the LHC era A number of theoretical challenges remain to be addressed at the level of field theory, QCD, and nuclear structure New experimental and theoretical efforts in nuclear structure physics are a key component of this quest