Lecture V Electric Dipole Moments and the Baryon
Lecture V: Electric Dipole Moments and the Baryon Asymmetry M. J. Ramsey-Musolf U Mass Amherst http: //www. physics. umass. edu/acfi/ ACFI EDM School November 2016 1
Lecture V Outline I. General Considerations II. Electroweak Baryogenesis III. Electroweak Phase Transition IV. CPV & EDMs 2
I. General Considerations 3
The Origin of Matter Cosmic Energy Budget Dark Matter 27 % Baryons 5% 68 % Dark Energy Explaining the origin, identity, and relative fractions of the cosmic energy budget is one of the most compelling motivations for physics beyond the Standard Model
Symmetries & Cosmic History EW Symmetry Breaking: Higgs Standard Model Universe 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . .
Symmetries & Cosmic History EW Symmetry Breaking: Higgs BSM Physics? Standard Model Universe 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . .
Symmetries & Cosmic History EW Symmetry Breaking: Higgs Standard Model Universe How did we go from nothing to something ? 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . . 7
Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe ? 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . . 8
Cosmic Baryon Asymmetry Cosmic Microwave Bcknd: Big Bang Nucleosynthesis: Shape of anisotropies depends on YB Light element abundances depend on YB
Cosmic Baryon Asymmetry Big Bang Nucleosynthesis: Light element abundances depend on YB
Cosmic Baryon Asymmetry Cosmic Microwave Bcknd: Shape of anisotropies depends on YB
Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe ? ? • C: Charge Conjugation • P: Parity 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . . 12
Cosmic Baryon Asymmetry One number ! BSM Physics 13
Ingredients for Baryogenesis • B violation (sphalerons) • C & CP violation • Out-of-equilibrium or CPT violation
Ingredients for Baryogenesis Standard Model BSM • B violation (sphalerons) � � • C & CP violation � � • Out-of-equilibrium or CPT violation � �
Cosmic Baryon Asymmetry One number ! IIII … Explanations BARYOGENESIS THEORIES Theory 16
Cosmic Baryon Asymmetry One number ! IIII … Explanations Experiment can help: • Discover ingredients • Falsify candidates BARYOGENESIS THEORIES Theory 17
Ingredients for Baryogenesis Scenarios: leptogenesis, EW baryogenesis, Afflek. Dine, asymmetric DM, cold baryogenesis, postsphaleron baryogenesis… Standard Model BSM • B violation (sphalerons) � � • C & CP violation � � • Out-of-equilibrium or CPT violation � �
Ingredients for Baryogenesis Scenarios: leptogenesis, EW baryogenesis, Afflek. Dine, asymmetric DM, cold baryogenesis, postsphaleron baryogenesis… Ingredients? Standard Model BSM • B violation (sphalerons) � � • C & CP violation � � • Out-of-equilibrium or CPT violation � �
Ingredients for Baryogenesis Scenarios: leptogenesis, EW baryogenesis, Afflek. Dine, asymmetric DM, cold baryogenesis, postsphaleron baryogenesis… Testable Standard Model BSM • B violation (sphalerons) � � • C & CP violation � � • Out-of-equilibrium or CPT violation � �
Energy Scale (Ge. V) Baryogenesis Scenarios 1012 Standard thermal lepto 109 Affleck Dine 10 2 Electroweak, resonant lepto, WIMPY baryo, ARS lepto… 10 -1 Post-sphaleron, cold… 21
Energy Scale (Ge. V) Baryogenesis Scenarios 1012 Standard thermal lepto 109 Affleck Dine 10 2 Electroweak, resonant lepto, WIMPY baryo, ARS lepto… 10 -1 Post-sphaleron, cold… Most directly testable 22
Baryogenesis Scenarios Energy Scale (Ge. V) Discover (some) ingredients & possibly falsify 1012 Standard thermal lepto 109 Affleck Dine 10 2 Electroweak, resonant lepto, WIMPY baryo, ARS lepto… 10 -1 Post-sphaleron, cold… Most directly testable 23
Baryogenesis Scenarios Energy Scale (Ge. V) Discover (some) ingredients & possibly falsify 1012 Standard thermal lepto 109 Affleck Dine 10 2 Electroweak, resonant lepto, WIMPY baryo, ARS lepto… 10 -1 Post-sphaleron, cold… Most directly testable EDMs ! 24
Electroweak Baryogenesis Was YB generated in conjunction with electroweak symmetry-breaking? 25
Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe ? EW Baryogenesis: testable w/ EDMs + colliders Leptogenesis: look for ingred’s w/ s: DBD, osc 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . . 26
II. Electroweak Baryogenesis 27
Electroweak Baryogenesis Ingredients • Baryon number violation • Strong first order electroweak phase transition • Effective CPV 28
Electroweak Baryogenesis: Ingredients Sakharov Criteria Anomalous B-violating processes SM Sphalerons: � • B violation • C & CP violation • Nonequilibrium dynamics Sakharov, 1967 EDMs SM CKM CPV: � Prevent washout by inverse processes LHC: Scalars SM EWPT: �
Electroweak Baryogenesis Ingredients • Baryon number violation • Strong first order electroweak phase transition • Effective CPV 30
Electroweak Sphalerons Al Sphaleron Configuration 31
Electroweak Sphalerons Al Sphaleron Configuration Anomaly (B+L) / NF 32
Electroweak Baryogenesis Ingredients • Baryon number violation • Strong first order electroweak phase transition • Effective CPV 33
Symmetries & Cosmic History What is the nature of the EW phase transition ? EW Symmetry Breaking: Higgs Standard Model Universe 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . . 34
BEH-like Boson Observation
EWSB: The Scalar Potential From Nature What was thermal history of EWSB ? 36
EWSB: The Scalar Potential From Nature What was thermal history of EWSB ? 37
Scalar Potential: Thermal History Single-Step EWSB Constrained by experiment, but not the only possibility 38
EW Phase Transition: New Scalars & CPV 1 st order 2 nd order 39
EW Phase Transition: New Scalars & CPV 1 st order 2 nd order Increasing mh 40
EW Phase Transition: New Scalars 1 st order 2 nd order “Strong” 1 st order EWPT Bubble nucleation Increasing mh SM: 1 st order EWPT endpoint EWSB
EW Phase Transition: St’d Model 2 nd order Temperature 1 st order Increasing mh 125 Ge. V Higgs Mass EW Phase Diagram How does this picture change in presence of new Te. V scale physics ? What is the phase diagram ? SM EW: Cross over transition 42
EW Phase Transition: New Scalars 1 st order 2 nd order “Strong” 1 st order EWPT Bubble nucleation Increasing mh New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches • Novel EWSB patterns • New states • Higgs prop’s EWSB
Electroweak Baryogenesis Ingredients • Baryon number violation • Strong first order electroweak phase transition • Effective CPV 44
EW Phase Transition: New Scalars & CPV 1 st order 2 nd order “Strong” 1 st order EWPT Bubble nucleation Increasing mh New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches YB : CPV & EW sphalerons EWSB 45
EW Phase Transition: New Scalars & CPV 1 st order 2 nd order “Strong” 1 st order EWPT Bubble nucleation Increasing mh New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches YB : CPV & EW sphalerons EWSB BSM 46
EW Phase Transition: New Scalars & CPV 1 st order 2 nd order “Strong” 1 st order EWPT Bubble nucleation Increasing mh New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches YB : diffuses into interiors EWSB 47
EW Phase Transition: New Scalars & CPV 1 st order 2 nd order “Strong” 1 st order EWPT Preserve YBinitial Bubble nucleation Quench EW sph Increasing mh New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches YB : diffuses into interiors EWSB 48
III. Electroweak Phase Transition Did the conditions for EWBG exist ? 49
The Higgs Portal
Portals & Early Universe Standard Model Hidden Sector “Singlets”
EW Phase Transition: Higgs Portal 1 st order 2 nd order < > Increasing mh “Higgs Portal” New scalars +… New scalars that interact with SM via the Higgs +…
EW Phase Transition: New Scalars 1 st order 2 nd order <S > Increasing mh New scalars Real Singlet: f ! S Simplest Extension: two states h 1 & h 2 Profumo, R-M, Shaugnessy JHEP 0708 (2007) 010 Scan: EWPT-viable model parameters Light: all models Black: LEP allowed
EW Phase Transition: St’d Model 2 nd order Singlets Temperature 1 st order Increasing mh 125 Ge. V Higgs Mass EW Phase Diagram How does this picture change in presence of new Te. V scale physics ? What is the phase diagram ? SM EW: Cross over transition 54
Experimental Probes: Energy Frontier LHC International Linear Collider ATLAS CMS Future Circular e+e- & pp Thanks: S. Gascon. Shotkin
EW Phase Transition: New Scalars 1 st order 2 nd order <S > Increasing mh m 2 > 2 m 1 New scalars Real Singlet: Mixed States: Precision $ ILC, CPEC, FCC-ee f ! S Simplest Extension: two states h 1 & h 2 Profumo, R-M, Shaugnessy JHEP 0708 (2007) 010 m 1 > 2 m 2
EW Phase Transition: New Scalars 1 st order 2 nd order <S > Increasing mh m 2 > 2 m 1 New scalars Novel signatures: Mixed States: Precision $ ILC, CPEC, FCC-ee Simplest Extension: ttwo states h 1 & h 2 t+ No & RM, ar. Xiv: 1310. 6035 : LHC Discovery w/ 100 fb-1 m 1 > 2 m 2
EW Phase Transition: New Scalars 1 st order 2 nd order <S > Increasing. Next mhgen pp m 2 > 2 m 1 New scalars Novel signatures: Simplest LHC Extension: ttwo states h 1 & h 2 t+ Mixed States: Precision $ ILC, CPEC, FCC-ee m 2 ! Next gen pp: Kotwal, No, R-M, Winslow 1604. XXXX m 1 > 2 m 2
EW Phase Transition: New Scalars 1 st order 2 nd order <S > Modified Higgs Self-Coupling m 2 > 2 m 1 h 1 Mixed States: Precision $ ILC, CPEC, FCC-ee h 1 m 1 > 2 m 2
EW Phase Transition: New Scalars 1 st order 2 nd order <S > Modified Higgs Self-Coupling Increasing mh New scalars Profumo, R-M, Wainwright, Winslow: 1407. 5342 m 2 > 2 m 1 Mixed States: Precision $ ILC, CPEC, FCC-ee m 1 > 2 m 2
EW Phase Transition: New Scalars 1 st order 2 nd order <S > Modified Higgs Self-Coupling ILC HL-LHC Increasing mh New scalars m 2 > 2 m 1 Mixed States: Precision $ ILC, CPEC, FCC-ee/ CEPC FCC-hh/SPPC Profumo, R-M, Wainwright, Winslow: 1407. 5342 m 1 > 2 m 2
IV. CPV & EDMs Did sufficiently effective CPV interactions occur ? 62
CPV in EW Baryogenesis LH leptons Bubble interior Unbroken phase LH quarks Topological transitions LH fermions Bubble exterior BSM CPV MSSM: Chung, Garbrecht, R-M, Tulin ‘ 09 Broken phase CP Violation & Transport MSSM: ~ 30 Coupled Eqns Transport: A Competition R-M et al CPV Chem Eq Diffusion Thanks: B. Garbrecht
EDMs & EWBG: MSSM & Beyond g ~ f f ~ V f Heavy sfermions: LHC consistent & suppress 1 -loop EDMs Sub-Te. V EW-inos: LHC & EWB viable but non-universal phases Compatible with observed BAU sin( M 1 b*) dn = 10 -27 e cm sin( M 1 b*) de = 10 -28 e cm dn = 10 -28 e cm ACME: Th. O de = 10 -29 e cm Next gen de Next gen dn Li, Profumo, RM ‘ 09 -’ 10 Compressed spectrum 64
Origin of the resonant behavior VC, C. Lee, MJRM, S. Tulin, 0912. 3523, 1106. 0747 Particles involved in EWB mix through v(x) When m 1 ~ m 2 one has maximal mixing and maximal Losc Behavior controlled by Lw vs Losc = 2π vrel/(ω1 - ω2) vs Lcoll Resonant enhancement due to non-adiabatic evolution (Losc/Lw >> 1) Analogy with spin 1/2 in external t-dependent magnetic field. B BROKEN PHASE x(T-1) UNBROKEN right-moving modes PHASE y x 65
EDMs: What We May Learn Present n-EDM limit Proposed n-EDM limit Matter-Antimatter Asymmetry in the Universe: “n-EDM has killed more theories than any other single experiment” ? MSSM Theory: How robust ? Can EDMs kill EW baryogenesis ?
CPV for EWBG EDM Theoretical creativity EDM EWBG Back up slides & discussion 67
Back Up Slides 68
Did EWSB Happen Only Once ? Not necessarily BSM “non-singlets” ! Multi-step EWSB
EW Phase Transition: New Scalars 1 st order 2 nd order < > Increasing mh New scalars Real Triplet Two-step EWPT & dark matter Patel, R-M, PRD 88 (2013) 035013 ; Fileviez-Perez, Patel, RM, Wang, PRD 79 (2009) 055024
EW Phase Transition: New Scalars 1 st order 2 nd order < > Increasing mh Quench sphalerons Small entropy dilution New scalars Real Triplet Two-step EWPT & dark matter Baryogenesis dark Patel, R-M, PRD 88 (2013) 035013 matter
LHC Tests: Modified Higgs Properties 1 st order 2 nd order < > Mass (Ge. V) Two-step EWB favorable H Coupling Patel, R-M, PRD 88 (2013) 035013
LHC Tests: Modified Higgs Properties 1 st order 2 nd order < > HL-LHC, FCC-ee /CPEC Mass (Ge. V) EWB favorable ILC 250 H Coupling Patel, R-M, PRD 88 (2013) 035013
Two-Step EW Baryogenesis Illustrative Model: < > New sector: “Real Triplet” Gauge singlet S H ! Set of “SM” fields: 2 HDM Quench sphalerons Small entropy dilution Two CPV Phases: d : d. S : Baryogenesis Triplet phase Singlet phase dark matter Inoue, Ovanesyan, R-M: 1508. 05404 74
Two-Step EW Baryogenesis & EDMs are Two Loop Two CPV Phases: d : d. S : Triplet phase Singlet phase Insensitive to d. S : electrically neutral ! “partially secluded” Inoue, Ovanesyan, R-M: 1508. 05404 75
Illustrative Model: Results Two cases: (A) d. S = 0 Triplet CPV (B) d =0 YB Singlet CPV Present de Future dn Future dp ? No EDM constraints Inoue, Ovanesyan, R-M: 1508. 05404 76
Flavored EW Baryogenesis t. L EWBG by m. R 77
Flavored EW Baryogenesis t. L EWBG by m. R Flavor basis (high T) Mass basis (T=0) Guo, Liu, R-M, Shu 1609. 09849 78
Flavored EW Baryogenesis t. L EWBG by m. R Flavor basis (high T) Mass basis (T=0) CPV h ! tt Guo, Liu, R-M, Shu 1609. 09849 79
Flavored EW Baryogenesis t. L EWBG by m. R Flavor basis (high T) Mass basis (T=0) CPV h ! tt EWBG viable Guo, Liu, R-M, Shu 1609. 09849 80
EW Phase Transition: New Scalars & CPV 1 st order 2 nd order Increasing mh New scalars 81
EW Phase Transition: New Scalars & CPV 1 st order 2 nd order “Strong” 1 st order EWPT Bubble nucleation Increasing mh New scalars Baryogenesis Gravity Waves Scalar DM LHC Searches EWSB 82
Symmetries & Cosmic History EW Symmetry Breaking: Higgs BSM Physics? Standard Model Universe How did we go from nothing to something ? 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . .
Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe How did we go from nothing to something ? 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . .
Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe ? 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . .
Symmetries & Cosmic History EW Symmetry Breaking: Higgs Baryogenesis: When? CPV? SUSY? Neutrinos? Standard Model Universe ? EW Baryogenesis: testable w/ EDMs + colliders Leptogenesis: look for ingred’s w/ s: DBD, osc 10 -35 s 10 -11 s 10 -5 s ~1 m 380 k yr QCD: q+g! n, p… QCD: n+p! nuclei Astro: stars, galaxies, . .
- Slides: 86