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PPC 2010 , 12 -16 July, 2010

PPC 2010 , 12 -16 July, 2010. Interconnections among Baryo / Leptogenesis models . Pasquale Di Bari. TexPoint fonts used in EMF. Read the TexPoint manual before you delete this box.: A A A A A A A A A A. Dark matter Matter - antimatter asymmetry Inflation Accelerating Universe.

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PPC 2010 , 12 -16 July, 2010

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  1. PPC 2010, 12-16 July, 2010 Interconnections among Baryo/Leptogenesis models Pasquale Di Bari TexPoint fonts used in EMF. Read the TexPoint manual before you delete this box.: AAAAAAAAAA

  2. Dark matter Matter - antimatter asymmetry Inflation Accelerating Universe Puzzles of Modern Cosmology Baryogenesis  clash between the SM and CDM !

  3. Primordial matter-antimatter asymmetry • Symmetric Universe with matter- anti matter domains ? Excluded by CMB + cosmic rays )B = (6.2 ± 0.15) x 10-10>> B • Pre-existing ? It conflicts with inflation ! (Dolgov ‘97) ) dynamical generation (baryogenesis) CMB (Sakharov ’67)

  4. From phase transitions: - ElectroweakBaryogenesis: * in the SM * in the MSSM * in the nMSSM * in the NMSSM * in the 2 Higgs model * at B-L symmetry breaking * in Technicolor (poster by Jarvinen) *.......................................................................... Affleck-Dine: - at preheating - Q-balls - ………..... From Black Hole evaporation Spontaneous Baryogenesis Gravitational Baryogenesis .................................................... From heavy particle decays: - maximons decays (Sakharov ‘67) - GUT Baryogenesis - LEPTOGENESIS Models of Baryogenesis

  5. Baryogenesis in the SM ? All 3 Sakharov conditions are fulfilled in the SM at some level: Baryon number violation if T  100 GeV (sphaleron transitions), 2) CP violation in the quark CKM matrix, 3) Departure from thermal equilibrium (an arrow of time) from the expansion of the Universe

  6. EWBG in the SM (Kuzmin,Rubakov,Shaposhnikov ’85; Kajantie,Laine,Shaposhnikov ‘97) If the EW phase transition (PT) is 1st order broken phase bubbles nucleate (Stephan Huber’s courtesy) In the SM the ratio vc/Tc is directly related to the Higgs massand only for Mh < 40 GeVone can have a strong PT  EW baryogenesis in the SM is ruled out by the LEP lower bound Mh 114 GeV !(also not enough CP)  New Physics is needed!

  7. EWBG in the MSSM (Carena, Quiros, Wagner ‘98) • Additional bosonic degrees of freedom(dominantly the lightstop • contribution)can make the EW phase transition more strongly first order if : LEP lower bound • Notice that there is a tension between the strong PT requirement and the • LEP lower bound on Mhand in particular one has to impose 5  tan   10 • In addition there are severe constraints from the simultaneous • requirement of CP violation in the bubble walls (mainly from charginos) • without generating too large electric dipole moment of the electron:

  8. Baryogenesisand the early Universe history TRH = ? ( 1014GeV) Inflation T 100 GeV EWBG “Cold” EWBG(Krauss,Trodden’99; Konstandinet al.‘10) 0.1- 1 MeV BBN 0.1- 1 eV Recombination

  9. Affleck-Dine Baryogenesis (Affleck, Dine ‘85) In the Supersymmetric SM there are many “flatdirections” in the spaceof a fieldcomposedofsquarks and/or sleptons F term D term A flat direction can beparametrized in termsof a complexfield (AD field) thatcarries a baryonnumber thatisviolateddynamicallyduringinflation The finalasymmetryis TRH and the observedone can bereproducedfor low values TRH  10 GeV !

  10. Baryogenesisand the early Universe history Inflation TRH10 GeV Affleck-Dine (at preheating) T 0.1- 1 MeV BBN 0.1- 1 eV Recombination

  11. GravitationalBaryogenesis (Davoudiasl,Kribs,Kitano,Murayama,Steinhardt ‘04) The key ingredientis a CP violatinginteractionbetween the derivative of the Ricci scalar curvature R and the baryonnumbercurrentJm: Cutoff scale of the effective theory Itisnatural tohavethisoperator in quantum gravity and in supergravity TRH Itworksefficiently and asymmetriesevenmuchlargerthan the observedone are generatedforTRH >> 100 GeV

  12. Baryogenesisand the early Universe history 1014GeV >> TRH >> 100 GeV Inflation Affleck-Dine (at preheating) Gravitationalbaryogenesis GUT baryogenesis T 100 GeV EWBG “Cold” EWBG 0.1- 1 MeV BBN 0.1- 1 eV Recombination

  13. From phase transitions: - ElectroweakBaryogenesis: * in the SM * in the MSSM * in the nMSSM * in the NMSSM * in the 2 Higgs model * at B-L symmetry breaking * in Technicolor (poster by Jarvinen) *.......................................................................... Affleck-Dine: - at preheating - Q-balls - ………..... From Black Hole evaporation Spontaneous Baryogenesis Gravitational Baryogenesis .................................................... From heavy particle decays: - maximons decays (Sakharov ‘67) - GUT Baryogenesis - LEPTOGENESIS Models of Baryogenesis

  14. Neutrino masses: m1 < m2 < m3 Tritium  decay :me<2.3 eV (Mainz 95% CL) 0:m< 0.3 – 1.0 eV (Heidelberg-Moscow 90% CL, similar result by CUORICINO ) using the flat prior (0=1): CMB+BAO :  mi < 0.61 eV (WMAP7+BAO+H0) CMB+LSS + Ly : mi <0.17 eV (Seljak et al.)

  15. Minimal scenario of Leptogenesis (Fukugita,Yanagida ’86) • Type I seesaw Total CP asymmetries • Thermal production of the RH neutrinos T  Mi/5

  16. The importance of leptogenesis for testing the seesaw Reconstructing MandmDwouldprovidea uniqueinformationon thenew model embeddingtheseesawaddressing fundamental questionslike majoranamass M ?flavour ? HowneutrinoandquarkYukawa‘s arerelated ? whythreefamilies? But: (Casas, Ibarra ‘01) Low energyneutrinoexperimentsgiveinformationonlyon the9 parameters in . The 6 parameters in theorthogonal matrixΩ(encodes the 3 life timesand the 3 total CP asymmetriesof the RH neutrinos and itis aninvariant(King ‘07) ) + the 3 masses Miescape the conventionalinvestigation !! Leptogenesiscomplements low energy neutrino experiments constrainingheavyneutrinosproperties

  17. Vanilla leptogenesis 1) Flavorcompositionof final leptonsisneglected Total CP asymmetries If i≠ 0 alepton asymmetryis generated from Ni decays and partly converted into a baryon asymmetry by sphaleron processesif Treh 100 GeV ! (Kuzmin,Rubakov,Shaposhnikov, ’85) baryon-to -photon number ratio efficiency factors# of Ni decaying out-of-equilibrium CMB Successfulleptogenesis : B = B =(6.2 ± 0.15) x 10-10

  18. Neutrino mass bounds in vanilla leptog. (Davidson,Ibarra‘02;Buchmüller,PDB,Plümacher ’02,’03,’04; Giudice et al. ‘04) 2) N1 – dominated scenario Vanilla leptogenesisisnot compatiblewith quasi-deg. neutrinos Imposing: No dipendence on the leptonic mixing matrix U ! Theselarge temperatures in gravitymediated SUSY models sufferfrom the gravitino problem

  19. SO(10)-inspired leptogenesis ( Branco et al. ’02; Nezri, Orloff ’02; Akhmedov, Frigerio, Smirnov ‘03) (bi-unitary parametrization) assuming: 1) 2) One typically has (there are some fine-tuned exceptions): since M1 << 109GeVB(N1) << BCMB!  failureofthe N1-dominated scenario !

  20. Independence of the initial conditions The earlyUniverse „knows“ neutrinomasses ... (Buchmüller,PDB,Plümacher ’04) decayparameter wash-out of a pre-existing asymmetry

  21. Beyond vanilla Leptogenesis Non minimal Leptogenesis (in type II seesaw, non thermal,….) The degenerate limit Improved Kineticdescription (momentumdependence, quantum kineticeffects,finite temperature effects,…….) Vanilla Leptogenesis FlavourEffects (heavyflavoureffects, light flavoureffects, light+heavyflavoureffects)

  22. Light flavour effects (Nardi,Nir,Roulet,Racker ’06;Abada,Davidson,Losada,Josse-Michaux,Riotto’06; Blanchet, PDB, Raffelt ‘06; Riotto, De Simone ‘06) Flavorcomposition of lepton quantum states: Itdoes not playanyrolefor But for M1  1012 GeV-Yukawa interactions are fast enough to break the coherent evolution of and become an incoherentmixtureof a andof+e  IfM1 109GeVthen also- Yukawasin equilibrium 3-flavor regime heavy neutrino flavor index lepton flavor index

  23. The additional contribution to CP violation: depends on U ! 1) N1 2) +   N1  

  24. Low energy phases as the only source of CP violation (Nardi et al; Blanchet,PDB, ’06; Pascoli, Petcov, Riotto; Anisimov, Blanchet, PDB ’08) The whole CP violation can stems just from low energyphases (Dirac, Majoranaphases) and stillitispossibletohavesuccessfulleptogenesis ! independentofinitial N1 abundance Green points: only Dirac phase with sin 13= 0.2 Red points: onlyMajorana phases initialthermal N1abundance (Blanchet, PDB ’09) However, in general, wecannotconstraint the low energyphaseswithleptogenesis and viceversa wecannot test leptogenesis just measuring CP violation at low energies: weneedtoadd some furthercondition !

  25. The lower bounds on M1 and on Trehget relaxed: (Blanchet,PDB ’08) The usual lowerbound gets relaxed

  26. Heavy flavour effects:N2-dominated scenario ( PDB ’05; Vives’05; Blanchet, PDB ’06; Blanchet, PDB ’08) If light flavoureffects are neglected the asymmetryfrom the next-to-lightest (N2) RH neutrinosistypicallynegligible: ...except for a special choice of =R23 when K1= m1/m* << 1 and ε1=0: The lower bound on M1 disappears and is replaced by a lower bound on M2 … that however stillimplies a lower bound on Treh!

  27. N2-flavored leptogenesis (Vives’05; Blanchet, PDB ’06; Blanchet, PDB ’08) If light and heavyflavoureffects are combinedtogether: Wash-out isneglected Wash-out and flavor effects are both taken into account Unflavored case Thankstoflavoreffectsthedomainofapplicability extendsmuchbeyondtheparticularchoice=R23!

  28. The N2-dominated scenario rescues SO(10) inspiredmodels ! (PDB, Riotto ’08) The greenpointscorrespondtoat 2σ: Θ13 2=5 VL= I A lowerbound on ? Θ13 Θ23 An upper bound on ? Θ23

  29. Forthesolutionwithm1  3x10-3 eV theasymmetryis dominantlyproduced in thetauonflavoursince2,,e  (mt,c,u)2 2 2 2e

  30. Baryogenesisand the early Universe history Inflation TRH = ? Affleck-Dine (at preheating) Gravitationalbaryogenesis GUT baryogenesis T Leptogenesis (minimal) 108GeV 100 GeV EWBG 0.1- 1 MeV BBN 0.1- 1 eV Recombination

  31. (Bertuzzo,PDB,Marzola‘10) The problemof the initialconditions in flavouredleptogenesis Asymmetrygenerated fromleptogenesis Residual “pre-existing” asymmetrypossibly generatedby some externalmechanism Onehastodistinguish 10 different RH neutrino mass patterns: ……… ……… The wash-out of a pre-existingasymmetryis guaranteedonly in a tauon N2-dominated scenario! Importantloophole:in supersymmetricmodels(Antusch,King,Riotto‘06) also in N1dominatedscenarioswithtan2  20

  32. Flavour coupling (Buchmuller, Plumacher ’01; Barbieri et al.’01; Nardi et al.’06;Blanchet, PDB ‘08) TakingintoaccountsthatanHiggsbosonasymmetryisalsoproduced in the decaysof the RH neutrinos and that the leptonasymmetries are redistributedbygaugeinteractionsintoquarks and chargedleptonsaswell, the set ofkineticequationsbecomes: The flavoredasymmetriesdynamicscouple ! Flavorcouplingdoesnotrelevantlyaffect the finalasymmetry In N 1 –leptogenesis (Abada, Josse-Michaux ‘07) but a strong enhancementispossible in N 2 –leptogenesis ! (Antusch, PDB, Jones, King ‘10)

  33. Leptogenesis and discrete flavour symmetries: A4 (Ma ’04; Altarelli, Feruglio ’05; Bertuzzo, Di Bari, Feruglio, Nardi’09;Hagedorn,Molinaro,Petcov ‘09 ) The situation islessattractivethan in SO(10) inspiredmodelsbecause the RH neutrino mass spectrum first requiresvery high temperatures, seconditdoesnotallow a wash-out of a pre-existingasymmetry

  34. Leptogenesis in A4 models (Ma ’04; Altarelli, Feruglio ’05; Bertuzzo, Di Bari, Feruglio, Nardi ‘09) Howeversuccessfulleptogenesisseemstobepossible (better in thenormal hierarchicalcase) just forthebest valuesofthesymmetrybreakingparameters Normalordering Invertedordering Symmetry Breaking parameter The differentlinescorrespondtovaluesof y between 0.3 and 3

  35. Conclusions Baryogenesis is not only a missing stage in the early Universe history but also an important tool for BSM investigation. A very long list of proposed models, some of which even able to produce much larger asymmetries than the observed one. EWB seems at the moment in “stand by” but it could become again a viable solution if e.g. supersymmetry is discovered. In Leptogenesis on the other hand the necessary BSM condition has been already found (neutrino masses) and we are seeking a way to (dis)prove it ! In minimal leptogenesis (type I + thermal), flavour effects make the N2 dominated scenarioas quite an attractive option: it rescues SO(10)-inspired scenarios providing a well motivated framework testable (to some extent) at future low energy neutrino experiments. It is quite intriguing that SO(10)-inspired leptogenesis fulfil those quite specific requirements necessary for a complete independence of the initial conditions! Constraints on low energy neutrino parameters become then more robust Leptogenesis is an interesting guidance for the identification of the theory responsible for neutrino masses and mixing underlying the seesaw mechanism (GUT’s ? Flavor symmetries ? Either ? Neither ?)

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