Leptogenesis and Neutrino Physics

1. Leptogenesis and Neutrino Physics 2011.4.7 연세대학교 강신규(서울과학기술대)

2. Outline • Introduction - baryogenesis • Baryogenesis in some models • Leptogenesis • Informations on neutrino masses from leptogenesis • Neutrinoless double beta decay • Connection between leptogenesis and neutrinoless double beta decay • Summary

3. Introduction • Inflation explains r=rcr • Big-bang explains ne=np, n4He/np=0.125, • nD/np=1.5x10-5, nn/ng=3/22 , etc. • We do not understand nB/ng

4. Measuring nB/ng= 6 · 10−10 • - Tnow ~ 3K directly tells ng~ T3now ~ 400/cm3. • - nB ~ 1/m3 follows from • Anisotropies in the cosmic microwave background: • nB/ng= (6.3±0.3)x10−10. (2) Big Bang Nucleosynthesis: the D abundancy implies nB/ng= (6.1±0.5)x10−10. arisen from many g push in the direction reactions like p n D g (1) and (2) are indirect but different: their agreement makes the result trustable.

5. nB/ng= 6 · 10−10 is a strange number, because means that when the universe cooled below T ~ mp , we survived to nucleon/antinucleon annihilations as 10,000,000,001 nucleons 10,000,000,000 anti-nucleons Nucleons and anti-nucleons got together…

6. They have all annihilated away except for the tiny • difference. 1 nucleon • That created tiny excess of matter in the present • universe (unnatural !!!) nB/ng = 6 · 10−10

7. Can a asymmetry can be generated dynamically from nothing? Yes, if 3 Sakharov conditions are satisfied • Necessary requirements for baryogenesis: • Baryon number violation : • C & CP violation : • Non-equilibrium

8. Out-of-Equilibrium Decay Out-of Equilibrium obtained due to expansion of the Universe as a background for heavy decaying particles. Condition for out-of-equilibrium decay

9. Boltzmann Equation If interactions becomes too slow to catch up with expanding Universe, NX start to become overabundant. We must consider inverse decays, scatterings and annihilations RHS  NXvariation due to all elementary processes for X

10. Abundance as a function of temperature

11. Coupled Equations for nX and nB-L CP asymmetry washout at T<M In the SM not all of the dynamics is described by perturbative effects; There are non-perturbative interactions that violate B+L.

12. Sphaleron Non-perturbative finite temperature interactions, involving all left chiral fermions (due to chiral nature of weak interactions) Above EW-scale sphaleron processes (violating B+L) are in equilibrium and conserve B-L. Below EW-scale Higgs vev suppresses sphaleron rates  constrains models of EW Baryogenesis.

13. Baryogenesis in the standard model • Sakharov’s conditions • B violation EW anomaly (Sphaleron) • CP violation KM phase • Non-equilibrium 1st order phase trans. • Standard Model may satisfy all 3 conditions! • Electroweak Baryogenesis(Kuzmin, Rubakov, Shaposhnikov) • Two big problems in the Standard Model • 1st order phase transition requires mH < 60GeV • CP violation too small because • J  det[Yu†Yu, Yd†Yd]~ 10–20<< 10–10

14. Original GUT Baryogenesis • GUT necessarily breaks B. • (there exist several B violating interactions) • A GUT-scale particle X decays out-of-equilibrium with direct CP violation • But keeps B–L0  “anomaly washout” • Monopole problem • Alternative scenarios required (B-L violation)

15. Leptogenesis: role of neutrinos in baryogenesis

16. Seesaw MechanismPrerequisite for Leptogenesis • Why is neutrino mass so small? • Need right-handed neutrinos to generate tiny neutrino mass, but nR SM neutral • Majorana neutrinos: violate lepton number (B-L violation) To obtain m3~(Dm2atm)1/2, mD~mt, M3~1015GeV (GUT!)

17. (SM) Basic Leptogenesis Mechanism • Fukugita and Yanagida ’86 • Based on standard out-of-equilibrium decay of a heavy particle: • 1. CP violating decay of a heavy particle through an L-violating interaction can produce a lepton asymmetry. • 2. This lepton asymmetry is transformed into a • baryon asymmetry through sphaleroninteractions :

18. CP Asymmetry • CP violation through phases in neutrino sector. • CP asymmetry produced through interference of tree and one-loop contribution of decay rate.

19. abundance at eq. • Decay rate : • Lepton number asymmetry • e : CP asymmetry determined by the particle physics model that • produces couplings and masses for NR • k (efficiency) : incorporates washout effects by L-violating interactions • after the RH neutrinos decay.

20. Baryon asymmetry determined by 4 parameters • CP asymmetry e1 • Mass of decaying neutrino M1 • Effective light neutrino mass (coupling strength of N1) • Light neutrino masses

21. k(efficiency) as function of

22. Maximalefficiency :

23. Some constraints from Leptogenesis (1) Heavy neutrino mass  depends on the NR mass hierarchy (i) Very hierarchical Assuming • When vertex diagram becomes dominant • (Davidson & Ibarra)

24. implying that N1 cannot be too light & mnnot be too heavy • for hierarchical mn,

25. (ii) hierarchical M2,3~10-100M1 small can be large For example) are compatible with successful leptogenesis with special Yukawa matrix

26. (iii) Quasi-degenerate case M1~M2 Huge resonance peak if • No more mn constraints on leptogenesis • No more lower limit on heavy Majorana mass •  TeV scale leptogenesis possible •  Resonant leptogenesis

27. (2) Light neutrino masses • mnconstraints on the size of e

28. Refinement by Buchmuller et al. for constraint on ε Considering the efficiency k which depends on

29. Thermal leptogenesis fails if ns are too heavy and degenerate due to: the domain shirnks to zero yields upper limits on mi

30. Nodependence on intial abundance of N1 for

31. Since , leptogenesis window for neutrino mass compatible with neutrino oscillation

32. Can we prove it experimentally? • Unfortunately, no: it is difficult to reconstruct relevant CP-violating phases from neutrino data • But: we will probably believe it if • 0nbband/or LNV processesfound • CP violation found in neutrino oscillation • EW baryogenesis ruled out

33. CP Violation • Possible only if: • Dm122, s12 large enough (LMA) • q13 large enough • Can we see CP violation?  KamLAND  Reactor Exp. ?  ? It may need better parameter determination using solar pp neutrinos

34. Neutrinoless double beta decay and Leptogenesis

35. With the discovery that neutrinos are not massless, there is intense interest in neutrinoless double-beta decay (0nbb) measurements. • 0nbb decay probes fundamental questions : • Lepton number violation : leptogenesis might be the • explanantion for the observed matter-antimatter • asymmetry. • Neutrino properties : the practical technique to • determine if neutrinos are their own anti-particle : • Majorana particles.

36. If 0nbb decay observed : • Violates lepton number : • Neutrino is a Majorana particle. • Provides a promising lab. method for determining the absolute neutrino mass scale that is complementary to other measurement techniques • Measurements in a series of different isotopes potentially can reveal the underlying interaction processes. • Establishing that neutrinos are Majorana particles would be as important as the discovery of neutrino oscillations

37. Neutrinoless double beta decay Lepton number violation Baryon asymmetry  Leptogenesis due to violation of B-L number

38. The half-life time, , of the 0nbbdecay can be factorized as : : phase space factor : Nuclear matrix element :depends on neutrino mass hierarchy

39. Best present bound : Heidel-Moscow Half-life Consistent with cosmological bound

40. Neutrino mass spectrum

41. If neutrinos are Majorana particles • Neutrino oscillations : - not sensitive to the nature of neutrinos - provide information on , but not on the absolute values of neutrino masses.

42. Neutrino mass scale and its property can be probed • by 0nbb • Prediction of depends on neutrino mass hierarchy

43. Normal hierarchy: • Inverted hierarchy

44. Quasi-degenerate • Estimate by using the best fit values of parameters including uncertainties in Majorana phases

45. ( Hirsch et al. , hep-ph/0609146 ) For inverted hierarchy, a lower limit on <mn> obtained 8 meV

46. In principle, a measurement of |<m>| combined with a measurement of m1(mass scale) • (in tritium beta-decay exp. and/or cosmology) • would allow to establish if CP is violated. • To constrain the CPV phases, • once the neutrino mass spectrum is known

47. Due to the experimental errors on the parameters and nuclear matrix elements uncertainties, determining that CP is violated in the lepton sector due to Majorana CPV phases is challenging. • Given the predicted values of , it might be possible only for IH or QD sepctra. In these two cases, the CPV region is inversely proportional to • Establishing CPV due to Majorana CP phases requires • Small experimental errors on and neutrino masses • Small values of • depends on the CPV phases :

48. Connection between low energy CPV and leptogenesis • High energy parameters Low energy parameters • 9 parameters are lost, of which 3 phases. • In a model-independent way there is no direct connection between the low-energy phases and the ones entering leptogenesis.

49. Using the biunitary parameterization, • depends only on the mixing in RH sector. • mndepends on all the parameters in Yn . • If there is CPV in VR, we can expect to have CPV in mn. • In models witha reduced number of model parameters, • it is possible to link directly the Dirac and Majorana phases to the leptogenesis one. • Additional information can be obtained in LFV charged lepton decays which depend on VL.

50. Existence of a correlation between • In minimal seesaw with two heavy Majorana neutrinos • (Glashow, Frampton, Yanagida,02) •  mDcontains 3 phases (Endo,Kaneko,SK,Morozumi,Tanimoto) (2002)