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Symmetries of the Early Universe and the Origin of Matter:

Symmetries of the Early Universe and the Origin of Matter:. M.J. Ramsey-Musolf Caltech Wisconsin-Madison. Fundamental Symmetries & Cosmic History. What were the fundamental symmetries that governed the microphysics of the early universe?.

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Symmetries of the Early Universe and the Origin of Matter:

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  1. Symmetries of the Early Universe and the Origin of Matter: M.J. Ramsey-Musolf Caltech Wisconsin-Madison

  2. Fundamental Symmetries & Cosmic History • What were the fundamental symmetries that governed the microphysics of the early universe? The (broken) symmetries of the Standard Model of particle physics work remarkably well at late times, but they leave many unsolved puzzles pertaining to the early universe • Can new symmetries at the weak scale account for the origin of matter and how can we find out? A combination of precise low-energy measurements, high energy collider experiments, dark matter searches, and theoretical advances will help us determine if new symmetries at the electroweak scale can account for the abundance of matter

  3. Outline Motivation: Why New Symmetries ?Why Low Energy Probes ? Brief Interlude: Supersymmetry Symmetries and the Origin of Matter • General Considerations • Theoretical challenges and developments • Phenomenology in the LHC era and beyond

  4. Motivation Why New Symmetries ?Why Low Energy Probes ?

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

  6. Big Bang Nucleosynthesis (BBN) & light element abundances • Weak interactions in stars & solar burning • Supernovae & neutron stars It utilizes a simple and elegant symmetry principle SU(3)c x SU(2)L x U(1)Y to explain the microphysics of the present universe Standard Model puzzles Standard Model successes Fundamental Symmetries & Cosmic History

  7. Non-zero vacuum expectation value of neutral Higgs breaks electroweak sym and gives mass: Electroweak symmetry breaking: Higgs ? • Where is the Higgs particle? • Is there more than one? Puzzles the St’d Model may or may not solve: U(1)EM SU(3)c x SU(2)L x U(1)Y How is electroweak symmetry broken? How do elementary particles get mass ? Standard Model puzzles Standard Model successes Fundamental Symmetries & Cosmic History

  8. 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?

  9. C:Charge Conjugation Cosmic Energy Budget Electroweak symmetry breaking: Higgs ? • P: Parity Beyond the SM SM symmetry (broken) Fundamental Symmetries & Cosmic History Baryogenesis: When? CPV? SUSY? Neutrinos? WIMPy D.M.: Related to baryogenesis? “New gravity”? Lorentz violation? Grav baryogen ? ?

  10. Unification? Use gauge coupling energy-dependence look back in time Present universe Early universe Standard Model High energy desert Energy Scale ~ T Weak scale Planck scale Fundamental Symmetries & Cosmic History

  11. Present universe Early universe Standard Model Gravity A “near miss” for grand unification Is there unification? What new forces are responsible ? High energy desert Weak scale Planck scale Fundamental Symmetries & Cosmic History

  12. Present universe Early universe Unification Neutrino mass Origin of matter Standard Model Weak Int Rates: Solar burning Element abundances Weak scale unstable: Why is GF so large? High energy desert Weak scale Planck scale Fundamental Symmetries & Cosmic History

  13. Supersymmetry, GUT’s, extra dimensions… There must have been additional symmetries in the earlier Universe to • Unify all matter, space, & time • Stabilize the weak scale • Produce all the matter that exists • Account for neutrino properties • Give self-consistent quantum gravity

  14. Large Hadron Collider Ultra cold neutrons LANSCE, NIST, SNS, ILL CERN What are the new fundamental symmetries? Two frontiers in the search Collider experiments (pp, e+e-, etc) at higher energies (E >> MZ) Indirect searches at lower energies (E < MZ) but high precision Particle, nuclear & atomic physics High energy physics

  15. Electroweak symmetry breaking: Higgs ? Beyond the SM SM symmetry (broken) Precision Probes of New Symmetries New Symmetries Origin of Matter Unification & gravity Weak scale stability Neutrinos

  16. Probing Fundamental Symmetries beyond the SM: Use precision low-energy measurements to probe virtual effects of new symmetries & compare with collider results • Precision measurements predicted a range for mt before top quark discovery • mt >> mb ! • mt is consistent with that range • It didn’t have to be that way Radiative corrections Direct Measurements Stunning SM Success Comparingloop effects in different processes canprobeparticle spectrum J. Ellison, UCI

  17. Precision ~ Mass Scale M=m~ 2 x 10-9 exp ~ 1 x 10-9 M=MW ~ 10-3 Interpretability • Precise, reliable SM predictions • Comparison of a variety of observables • Special cases: SM-forbidden or suppressed processes Precision, low energy measurements can probe for new symmetries in the desert

  18. II. Brief Interlude: Supersymmetry

  19. SUSY: a candidate symmetry of the early Universe • Unify all forces • Protect GF from shrinking • Produce all the matter that exists 3 of 4 Yes Maybe so Maybe Probably necessary • Account for neutrino properties • Give self-consistent quantum gravity

  20. Supersymmetry Fermions Bosons sfermions gauginos Higgsinos Charginos, neutralinos SUSY: a candidate symmetry of the early Universe

  21. If nature conserves vertices have even number of superpartners • Lightest SUSY particle is stable viable dark matter candidate • Proton is stable • Superpartners appear only in loops SUSY and R Parity Consequences

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

  23. III.Symmetries & the Origin of Matter • Baryogenesis: General Considerations • Theoretical challenges and developments • Phenomenology in the LHC era and beyond

  24. 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 T-odd , CP-odd by CPT theorem T-odd , CP-odd by CPT theorem 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 ?

  25. Anomalous B-violating processes Sakharov Criteria • B violation • C & CP violation • Nonequilibrium dynamics Prevent washout by inverse processes Sakharov, 1967 Ingredients for Baryogenesis

  26. Present universe Early universe ? ? Weak scale baryogenesis can be tested experimentally Weak scale Planck scale Ingredients for Baryogenesis Sakharov Criteria • B violation • C & CP violation • Nonequilibrium dynamics Sakharov, 1967

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

  28. Shaposhnikov Weak Scale Baryogenesis • B violation • C & CP violation • Nonequilibrium dynamics Quark mixing & CPV 1st order 2nd order Sakharov, 1967 • CP-violation too weak • EW PT too weak Increasing mh EW Baryogenesis: Standard Model

  29. 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

  30. 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

  31. Better theory Present n-EDM limit Proposed n-EDM limit Matter-Antimatter Asymmetry in the Universe ? M. Pendlebury B. Filippone Riotto; Carena et al.; Lee, Cirigliano, R-M, Tulin “n-EDM has killed more theories than any other single experiment”

  32. Weak Scale Baryogenesis • B violation • C & CP violation • Nonequilibrium dynamics Topological transitions Broken phase 1st order phase transition More Higgs? Sakharov, 1967 Ando,Barger, Langacker,O.Connell,Profumo, R-M, Shaugnessy, Tulin, Wise • 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 Theoretical Issues: Strength of phase transition (Higgs sector) Bubble dynamics (expansion rate) Transport at phase boundary (non-eq QFT) EDMs: many-body physics & QCD

  33. Need 1st order 2nd order So that Gsphaleron is not too fast Increasing mh Computed ESM! mH < 40 GeV Stop loops in VEff mh>114.4 GeV EMSSM ~ 10 ESM !mH < 120 GeV or ~ 90 GeV (SUSY) Electroweak Phase Transition & Higgs LEP EWWG

  34. sin2q Need 1st order 2nd order Singlet Higgs (SUSY or non-SUSY) So that Gsphaleron is not too fast Mixing Decay Increasing mH Computed ESM! mH < 40 GeV mh>114.4 GeV or ~ 90 GeV (SUSY) Electroweak Phase Transition & Higgs LEP EWWG

  35. Reduced SM Higgs branching ratios mH B.R. reduction Need 1st order 2nd order Singlet Higgs (SUSY or non-SUSY) Unusual final states So that Gsphaleron is not too fast O’Connell, R-M, Wise Mixing Decay Increasing mH How is electroweak symmetry broken? (LHC, ILC) Computed ESM! mH < 40 GeV mh>114.4 GeV or ~ 90 GeV (SUSY) Electroweak Phase Transition & Higgs LEP EWWG

  36. Weak Scale Baryogenesis • B violation • C & CP violation • Nonequilibrium dynamics Topological transitions Broken phase 1st order phase transition Sakharov, 1967 “Gentle” departure from equilibrium & scale hierarchy • Is it viable? • Can experiment constrain it? • How reliably can we compute it? Cirigliano, Lee, R-M,Tulin Baryogenesis: New Electroweak Physics 90’s: Cohen, Kaplan, NelsonJoyce, Prokopec, Turok Unbroken phase CP Violation Theoretical Issues: Strength of phase transition (Higgs sector) Bubble dynamics (expansion rate) Transport at phase boundary (non-eq QFT) EDMs: many-body physics & QCD

  37. Systematic treatment of transport with controlled approximations using non-equilibrium QFT Cirigliano, Lee, R-M, Tulin Quantum Transport & Baryogenesis Non-equilibrium quantum transport RHIC Violent departure from equilibrium Electroweak Baryogenesis “Gentle” departure from equilibrium & scale hierarchy

  38. Dine et al, St’d Model Free energy pressure Reflection pressure vw increasing mH p > pmin : transmitted Particles with M(f1) Particles with M(f2) p < pmin : reflected SUSY or other models ? mt Higgs pressure Boost pressure Fewer particles with p > pmin in wall rest frame; more reflection Bubble Wall Dynamics V (f2) < V (f1)

  39. Assumptions: LI Evolution is adiabatic Spectrum is non-degenerate Density is zero Evolution is non-adiabatic: vwall > 0 !decoherence Spectrum is degenerate: T > 0 ! Quasiparticles mix Density is non-zero Quantum Transport & Baryogenesis Electroweak Baryogenesis Particle Propagation: Beyond familiar (Peskin) QFT

  40. Fast, but not too fast Work to lowest, non-trivial order in e’s Error is O (e) ~ 0.1 ed =vw (k / w ) << 1 Hot, but not too hot Cirigliano, Lee, R-M ep = Gp / w << 1 Dense, but not too dense em = m / T << 1 Systematically derive transport eq’s from Lnew Evolution is non-adiabatic: vwall > 0 !decoherence Spectrum is degenerate: T > 0 ! Quasiparticles mix Density is non-zero Competing Dynamics CPV Det bal Cirigliano, Lee,Tulin, R-M Quantum Transport & Baryogenesis Electroweak Baryogenesis Scale Hierarchy:

  41. M1 0 -mZ cosb sinqW mZ cosb cosqW T ~TEW : scattering of H,W from background field MN = ~ ~ T ~ TEW mZ sinb sinqW M2 -mZ sinb sinqW 0 CPV 0 -m -mZ cosb sinqW mZ cosb cosqW -m T << TEW : mixing of H,W to c+, c0 mZ sinb sinqW -mZ sinb sinqW 0 ~ ~ ~ ~ M2 MC = m SUSY CPV & Quantum Transport Chargino Mass Matrix Neutralino Mass Matrix Resonant CPV: M1,2 ~ m

  42. Weak Scale Baryogenesis • B violation • C & CP violation • Nonequilibrium dynamics Topological transitions Broken phase 1st order phase transition Elementary particle EDMs: N!1 Sakharov, 1967 Many-body EDMs: • Is it viable? • Can experiment constrain it? • How reliably can we compute it? Engel,Flambaum, Haxton, Henley, Khriplovich,Liu, R-M Baryogenesis: New Electroweak Physics 90’s: Cohen, Kaplan, NelsonJoyce, Prokopec, Turok Unbroken phase CP Violation Theoretical Issues: Strength of phase transition (Higgs sector) Bubble dynamics (expansion rate) Transport at phase boundary (non-eq QFT) EDMs: many-body physics & QCD

  43. Dominant in nuclei & atoms EDMs in SUSY One-loop EDM: q, l, n… Chromo-EDM: q, n…

  44. T ~ TEW Future de dn dA Cirigliano, Lee, Tulin, R-M Resonant Non-resonant EDMs & Baryogenesis

  45. Decouple in large limit Dominant in nuclei & atoms Two-loop EDM only: no chromo-EDM Weinberg: small matrix el’s EDMs in SUSY One-loop EDM: q, l, n… Chromo-EDM: q, n…

  46. Baryogenesis | sin fm | > 0.02 | de , dn | > 10-28 e-cm Mc < 1 TeV Future de, dn LEP II Exclusion Two loop de Cirigliano, Profumo, R-M SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 EDMs & Baryogenesis

  47. LHC reach LHC reach ILC reach Present de Present de Present de Prospective de Prospective de Prospective de SUSY Baryogenesis & Colliders

  48. M1 0 -mZ cosb sinqW mZ cosb cosqW T ~TEW : scattering of H,W from background field MN = ~ ~ mZ sinb sinqW M2 -mZ sinb sinqW 0 CPV 0 -m -mZ cosb sinqW mZ cosb cosqW -m T << TEW : mixing of H,W to c+, c0 mZ sinb sinqW -mZ sinb sinqW 0 What role can the precursors of the neutralinos play in baryogenesis? ~ ~ ~ ~ M2 • = N11B 0 + N12W 0 + N13Hd0 + N14Hu0 MC = m T << TEW BINO WINO HIGGSINO SUSY CPV & Dark Matter Chargino Mass Matrix Neutralino Mass Matrix

  49. Neutralino-driven baryogenesis Charginos & neutralinos Baryogenesis LEP II Exclusion Two loop de Cirigliano, Profumo, R-M SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 SUSY Baryogenesis & Dark Matter

  50. Neutralino-driven baryogenesis suppressed too fast LEP II Exclusion Non-thermal c0 SUGRA: M2 ~ 2M1 AMSB: M1 ~ 3M2 Dark Matter: Relic Abundance

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