1. Sub Z Supersymmetry M.J. Ramsey-Musolf Precision Electroweak Studies in Nuclear Physics

2. NSAC Long Range Plan What is the structure of the nucleon? What is the structure of nucleonic matter? What are the properties of hot nuclear matter? What is the nuclear microphysics of the universe? What is to be the new Standard Model? Neutrino physics Precision measurements:  -decay,  -decay, parity violating electron scattering, EDM’s… What can they teach us about the new Standard Model?

3. The Standard Model of particle physics is a triumph of late 20th century physics It provides a unified framework for 3 of 4 (known) forces of nature in context of renormalizable gauge theory

4. The Standard Model of particle physics is a triumph of late 20th century physics Utilizes a simple & elegant symmetry principle to organize what we’ve observed

5. The Standard Model of particle physics is a triumph of late 20th century physics Utilizes a simple & elegant symmetry principle to organize what we’ve observed Strong (QCD) Scaling violations in DIS Asymptotic freedom R(e + e - ) Heavy quark systems Drell-Yan

6. The Standard Model of particle physics is a triumph of late 20th century physics Utilizes a simple & elegant symmetry principle to organize what we’ve observed Electroweak (=weak + QED) “Maximal” parity violation Conserved Vector Current CP-Violation in K, B mesons Quark flavor mixing Lepton universality…..

7. The Standard Model of particle physics is a triumph of late 20th century physics Most of its predictions have been confirmed Parity violation in neutral current processes: deep inelastic scattering, atomic transitions

8. The Standard Model of particle physics is a triumph of late 20th century physics Most of its predictions have been confirmed Neutral currents mix J 0 J Y J  J Z sin 2  W

9. The Standard Model of particle physics is a triumph of late 20th century physics Most of its predictions have been confirmed New particles should be found W, Z 0 3rd fermion generation (CP violation, anomaly) Higgs bosonNot yet!

10. We need a new Standard Model Two frontiers in the search Collider experiments (pp, e + e -, etc) at higher energies (E >> M Z ) Indirect searches at lower energies (E < M Z ) but high precision High energy physics Particle, nuclear & atomic physics CERNUltra cold neutronsLarge Hadron ColliderLANSCE, SNS, NIST

11. Outline I.SM Radiative Corrections & Precision Measurements II.Defects in the Standard Model III.An Example Scenario: Supersymmetry IV.Low-energy Probes of Supersymmetry Precision measurements “Forbidden processes” Weak decays lepton scattering

12. Outline I.SM Radiative Corrections & Precision Measurements II.Defects in the Standard Model III.An Example Scenario: Supersymmetry IV.Low-energy Probes of Supersymmetry Precision measurements “Forbidden processes” EDM’s 0  decay  !e,  !e  …

13. I. Radiative Corrections & Precision Measurements in the SM

14. The Fermi Theory of weak decays gave a successful, leading-order account

15. Fermi’s theory could incorporate higher order QED contributions QED radiative corrections: finite

16. The Fermi theory has trouble with higher order weak contributions Weak radiative corrections: infinite Can’t be absorbed through suitable re-definition of G F in H EFF

17. All radiative corrections can be incorporated in the Standard Model with a finite number of terms ggg Re-define g Finite

18. G F encodes the effects of all higher order weak radiative corrections gg  r  depends on parameters of particles inside loops

19. Comparing radiative corrections in different processes can probe particle spectrum  r  differs from  r Z gg

20. Comparing radiative corrections in different processes can probe particle spectrum

21. Precision measurements predicted a range for m t before top quark discovery m t >> m b ! m t is consistent with that range It didn’t have to be that way Radiative corrections Direct Measurements Stunning SM Success J. Ellison, UCI

22. Global Analysis   per dof = 25.5 / 15 M. Grunenwald Agreement with SM at level of loop effects ~ 0.1%

23. Collider Studies R. Clare, UCR LEP SLD Tevatron

24. Collider Studies

25. MWMW MtMt AA  had Tevatron

26. Collider Studies

28. “Blue Band”

29. Global Fit: Winter 2004   per dof = 16.3 / 13

30. II. Why a “New Standard Model”? There is no unification in the early SM Universe The Fermi constant is inexplicably large There shouldn’t be this much visible matter There shouldn’t be this much invisible matter

31. The early SM Universe had no unification Couplings depend on scale Energy Scale ~ T

32. Standard Model Present universe Early universe Weak scalePlanck scale High energy desert The early SM Universe had no unification

33. Standard Model Present universe Early universe Weak scalePlanck scale High energy desert A “near miss” for grand unification The early SM Universe had no unification Gravity

34. Standard Model Present universe Early universe Planck scale High energy desert The Fermi constant is too large Weak scale G F would shrink Unification Neutrino mass Dark Matter

35. The Fermi constant is too large  WEAK ~ 250 GeV G F ~ 10 -5 /M P 2

36. A smaller G F would mean disaster The Sun would burn less brightly  ~ G F 2 Elemental abundances would change T freeze out ~ G F -2/3 Smaller G F More 4 He, C, O…

37. There is too much matter - visible & invisible - in the SM Universe Visible Matter from Big Bang Nucleosynthesis Measured abundances SM baryogenesis Insufficient CP violation in SM

38. There is too much matter - visible & invisible - in the SM Universe Invisible Matter VisibleDark Insufficient SM CP violation No SM candidate S. Perlmutter

39. There must have been additional symmetries in the earlier Universe to Unify all forces Protect G F from shrinking Produce all the matter that exists Account for neutrino properties Give self-consistent quantum gravity

40. III. Supersymmetry Unify all forces Protect G F from shrinking Produce all the matter that exists Account for neutrino properties Give self-consistent quantum gravity 3 of 4 Yes Maybe so Maybe Probably necessary

41. SUSY may be one of the symmetries of the early Universe Supersymmetry Charginos, neutralinos FermionsBosons sfermions gauginos Higgsinos

42. Standard Model Present universe Early universe Weak scalePlanck scale Couplings unify with SUSY Supersymmetry High energy desert

43. SUSY protects G F from shrinking =0 if SUSY is exact

44. SUSY may help explain observed abundance of matter Cold Dark Matter Candidate  0 Lightest SUSY particle Baryonic matter Unbroken phase Broken phase CP Violation

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

46. Minimal Supersymmetric Standard Model (MSSM) L soft gives contains 105 new parameters How is SUSY broken? L SM L SUSY + L soft +

47. How is SUSY broken? Flavor-blind mediation Visible Sector: Hidden Sector: SUSY-breaking MSSM Gravity-Mediated (mSUGRA)

48. How is SUSY broken? Flavor-blind mediation Visible Sector: Hidden Sector: SUSY-breaking MSSM Gauge-Mediated (GMSB) messengers

49. Mass evolution gaugino mass group structure ln increases asdecreases increases faster than at the weak scale

50. Sfermion Mixing Q f < 0 Q f > 0

51. MSSM and R Parity Matter Parity: An exact symmetry of the SM SM Particles: Superpartners:

52. MSSM and R Parity MSSM conservesvertices have even number of superpartners Consequences  Lightest SUSY particle is stable viable dark matter candidate  Proton is stable  Superpartners appear only in loops