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Nuclei as Laboratories: Nuclear Tests of Fundamental Symmetries

This article discusses the use of nuclei as laboratories to test fundamental symmetries, such as electroweak symmetry breaking and the origin of baryonic matter. It also explores the cosmic energy budget, dark matter, dark energy, and the role of baryons in the universe.

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Nuclei as Laboratories: Nuclear Tests of Fundamental Symmetries

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  1. M.J. Ramsey-Musolf Nuclei as Laboratories: Nuclear Tests of Fundamental Symmetries 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. 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. Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History

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

  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. 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

  8. 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 ?

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

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

  11. 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

  12. 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

  13. If an EDM is seen, can we identify the new physics? 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

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

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

  16. CKM unitarity ? 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 New physics Kurylov, R-M RPV SUSY Weak decays & new physics

  17. Nuclear structure effects? b-decay SM theory input Recent Marciano & Sirlin Weak decays

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

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

  20. Light nM : Nuclear matrix elements difficult to compute 0n bb - decay probes the charge conjugation properties of the neutrino

  21. How do we compute & separate heavy particle exchange effects? 0n bb - decay: heavy particle exchange

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

  23. 0nbb decay Electroweak symmetry breaking: Higgs ? Light nM exchange ? Heavy particle exchange ? Beyond the SM SM symmetry (broken) Low scale LFV: R ~ O(1) GUT scale LFV: R ~ O(a) LF and LN: symmetries of the early universe? MEG: Bm!eg ~ 5 x 10-14 ? MECO: Bm!e ~ 5 x 10-17 Logarithmic enhancements of R Also PRIME

  24. How do we compute & separate heavy particle exchange effects? 4 quark operator, as in hadronic PV 0n bb - decay: heavy particle exchange

  25. L-violating new physics Non-perturbative QCD Nuclear dynamics 0n bb - decay: effective field theory We have a clear separation of scales

  26. L(q,e)! L(p,N,e) Spacetime & chiral transformation properties 0n bb - decay in effective field theory Operator classification

  27. L(q,e) = 0n bb - decay in effective field theory Operator classification e.g. 0n bb - decay: a = b = +

  28. 0n bb - decay in effective field theory Operator classification Chiral transformations: SU(2)L x SU(2)R Parity transformations: qL $ qR 0n bb - decay:a = b = +

  29. Systematic operator classification Enhanced effects for some models ? O(p-2) for O(p0) for Kpp, KpNN , KNNNN can be O( p0 ), O( p1 ), etc. 0n bb - decay in effective field theory

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

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

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

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

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

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

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

  37. Anapole moment Boulder, atomic PV hp~ 10 gp T=1 force T=0 force Is the weak NN force short range ?

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

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

  40. Done LANSCE HARD* NIST † *HIGS A program of few-body measurements Pionless theory Ab initio few-body calcs

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

  42. O( p -1 ) O( p) Hadronic PV as a probe • Determine VPV through O (p) from PV low-energy few-body studies where power counting works • Re-analyze nuclear PV observables using this VPV • If successful, we would have some indication that operator power counting works in nuclei • Apply to 0nbb-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

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