T-Violation & Baryogenesis M.J. Ramsey-Musolf U Mass Amherst http://www.physics.umass.edu/acfi/ ACFI TRV Workshop December 2018 1
Themes for This Talk • So far, connecting tests of TR invariance in neutron physics with the baryon asymmetry has focused on the neutron EDM • In this context, the neutron EDM provides an important probe that complements information from paramagnetic systems and diamagnetic atoms • Non-observations of EDMs place severe – but not fatal – constraints on baryogenesis scenarios at the TeV scale & below • There is room for more thought about connections with other neutron TR tests 2
Goals for This Talk • Provide a general context for interpreting EDM experiments • Illustrate the interplay of EDM searches with TeV scale & below baryogenesis scenarios • Invite discussion 3
Outline I. EDM’s: The SM & BSM context II. The Cosmic Matter-Antimatter Asymmetry III. Electroweak Baryogenesis: Examples IV. Post-sphaleron Baryogenesis V. Outlook 4
I. EDMs: The SM & BSM Context 5
EDMs & SM Physics d n SM ~ (10 -16 e cm) x θ QCD + d n CKM 6
EDMs & SM Physics d n SM ~ (10 -16 e cm) x θ QCD + d n CKM d n CKM = (1 – 6) x 10 -32 e cm C. Seng arXiv: 1411.1476 7
EDMs & SM Physics d n SM ~ (10 -16 e cm) x θ QCD + d n CKM d n CKM = (1 – 6) x 10 -32 e cm* C. Seng arXiv: 1411.1476 * 3.3 x 10 -33 e cm < d p < 3.3 x 10 -32 e cm 8
EDMs & BSM Physics d ~ (10 -16 e cm) x ( υ / Λ ) 2 x sin φ x y f F 9
EDMs & BSM Physics d ~ (10 -16 e cm) x ( υ / Λ ) 2 x sin φ x y f F CPV Phase: large enough for baryogenesis ? 10
EDMs & BSM Physics d ~ (10 -16 e cm) x ( υ / Λ ) 2 x sin φ x y f F BSM mass scale: TeV ? Much higher ? 11
EDMs & BSM Physics d ~ (10 -16 e cm) x ( υ / Λ ) 2 x sin φ x y f F BSM dynamics: perturbative? Strongly coupled? Dependence on other parameters ? 12
EDMs & BSM Physics d ~ (10 -16 e cm) x ( υ / Λ ) 2 x sin φ x y f F Need information from at least three “frontiers” 13
EDMs & BSM Physics d ~ (10 -16 e cm) x ( υ / Λ ) 2 x sin φ x y f F Need information from at least three “frontiers” • Baryon asymmetry Cosmic Frontier • High energy collisions Energy Frontier • EDMs Intensity Frontier 14
EDMs: New CPV? System Limit (e cm) * SM CKM CPV BSM CPV • SM “ background ” well 199 Hg 7.4 x 10 -30 10 -33 10 -29 below new CPV expectations ThO 1.1 x 10 -29 ** 10 -38 10 -28 • New expts: 10 2 to 10 3 more sensitive n 3.3 x 10 -26 10 -31 10 -26 • CPV needed for BAU? * 95% CL ** e - equivalent 15
EDMs: New CPV? System Limit (e cm) * SM CKM CPV BSM CPV • SM “ background ” well 199 Hg 7.4 x 10 -30 10 -33 10 -29 below new CPV expectations ThO 1.1 x 10 -29 ** 10 -38 10 -28 • New expts: 10 2 to 10 3 more sensitive n 3.3 x 10 -26 10 -31 10 -26 • CPV needed for BAU? * 95% CL ** e - equivalent Mass Scale Sensitivity sin φ CP ~ 1 ! M > 5000 GeV ϕ ψ γ M < 500 GeV ! sin φ CP < 10 -2 ϕ e 16
EDMs: New CPV? System Limit (e cm) * SM CKM CPV BSM CPV • SM “ background ” well 199 Hg 7.4 x 10 -30 10 -33 10 -29 below new CPV expectations ThO 1.1 x 10 -29 ** 10 -38 10 -28 • New expts: 10 2 to 10 3 more sensitive n 3.3 x 10 -26 10 -31 10 -26 • CPV needed for BAU? * 95% CL ** e - equivalent neutron proton & nuclei atoms ~ 100 x better sensitivity Not shown: muon 17
EDMs: New CPV? System Limit (e cm) * SM CKM CPV BSM CPV • SM “ background ” well 199 Hg 7.4 x 10 -30 10 -33 10 -29 below new CPV expectations ThO 1.1 x 10 -29 ** 10 -38 10 -28 • New expts: 10 2 to 10 3 more sensitive n 3.3 x 10 -26 10 -31 10 -26 • CPV needed for BAU? * 95% CL ** e - equivalent Mass Scale Sensitivity G B W < r o sin φ CP ~ 1 ! M > 5000 GeV f e g ϕ n e l l a h ψ C γ M < 500 GeV ! sin φ CP < 10 -2 ϕ e 18
EDMs: New CPV? System Limit (e cm) * SM CKM CPV BSM CPV • SM “ background ” well 199 Hg 7.4 x 10 -30 10 -33 10 -29 below new CPV expectations ThO 1.1 x 10 -29 ** 10 -38 10 -28 • New expts: 10 2 to 10 3 more sensitive n 3.3 x 10 -26 10 -31 10 -26 • CPV needed for BAU? * 95% CL ** e - equivalent Mass Scale Sensitivity G B W < r o • EDMs arise at > 1 loop f e g ϕ n e l l a h ψ C γ • CPV is flavor non-diagonal ϕ • CPV is “partially secluded” e • CPV is vector-like 19
EDMs: New CPV? System Limit (e cm) * SM CKM CPV BSM CPV • SM “ background ” well 199 Hg 7.4 x 10 -30 10 -33 10 -29 below new CPV expectations ThO 1.1 x 10 -29 ** 10 -38 10 -28 • New expts: 10 2 to 10 3 more sensitive n 3.3 x 10 -26 10 -31 10 -26 • CPV needed for BAU? * 95% CL ** e - equivalent Mass Scale Sensitivity This talk G B W < r o • EDMs arise at > 1 loop f e g ϕ n e l l a h ψ C γ • CPV is flavor non-diagonal ϕ • CPV is “partially secluded” e • CPV is vector-like 20
CPV for <WBG EDM Theoretical creativity EDM EWBG 21
II. The Matter-Antimatter Asymmetry 22
Cosmic Baryon Asymmetry Y B = n B = (8 . 82 ± 0 . 23) ⇥ 10 � 11 s One number ! BSM Physics 23
Cosmic Baryon Asymmetry Y B = n B = (8 . 82 ± 0 . 23) ⇥ 10 � 11 s One number ! IIII IIII IIII … Explanations BARYOGENESIS THEORIES Theory 24
Cosmic Baryon Asymmetry Y B = n B = (8 . 82 ± 0 . 23) ⇥ 10 � 11 s One number ! IIII IIII IIII … Explanations Experiment can help: BARYOGENESIS THEORIES • Discover ingredients • Falsify candidates Theory 25
Baryogenesis Scenarios 10 12 Standard thermal lepto Energy Scale (GeV) 10 9 Affleck Dine Electroweak, resonant lepto, 10 2 WIMPY baryo, ARS lepto… 10 -1 Post-sphaleron, cold… 26
Baryogenesis Scenarios 10 12 Standard thermal lepto Energy Scale (GeV) 10 9 Affleck Dine Electroweak, resonant lepto, 10 2 WIMPY baryo, ARS lepto… 10 -1 Post-sphaleron, cold… Era of EWSB: t univ ~ 10 ps 27
Electroweak Baryogenesis Was Y B generated in conjunction with electroweak symmetry-breaking? 28
III. Electroweak Baryogenesis • SUSY • Non-SUSY 29
EWBG: Ingredients • Strong first order EWPT: LHC ! Excluded for the MSSM ! Possible w/ extensions (e.g., NMSSM) • CPV: SUSY: Sources same as in MSSM + possible additional; non-SUSY 30
Strong 1 st Order EWPT MSSM Light Stop Scenario Beyond the MSSM: singlets, 2-step…. Definitive probe of the possibilities ! LHC + next generation colliders 31
EDMs & EWBG: MSSM + Singlets ~ γ , g f ~ f V f Heavy sfermions: LHC Sub-TeV EW-inos: LHC & EWB - consistent & suppress viable but non-universal phases 1-loop EDMs 32
EDMs & EWBG: MSSM + Singlets ~ γ , g f ~ f V f Heavy sfermions: LHC Sub-TeV EW-inos: LHC & EWB - consistent & suppress viable but non-universal phases 1-loop EDMs Compatible with d e = 10 -28 e cm observed BAU sin( µ M 1 b * ) sin( µ M 1 b * ) d n = 10 -27 e cm ACME: ThO d e = 10 -29 e cm d n = 10 -28 e cm Next gen d n Li, Profumo, RM ‘ 09- ’ 10 33
EDMs & EWBG: MSSM + Singlets ~ γ , g f ~ f V f Heavy sfermions: LHC Sub-TeV EW-inos: LHC & EWB - consistent & suppress viable but non-universal phases 1-loop EDMs Compatible with d e = 10 -28 e cm observed BAU sin( µ M 1 b * ) sin( µ M 1 b * ) d n = 10 -27 e cm ACME: ThO d e = 10 -29 e cm d n = 10 -28 e cm Next gen d n Compressed spectrum Li, Profumo, RM ‘ 09- ’ 10 34
CPV for <WBG EDM Theoretical creativity EDM EWBG 35
EW Multiplets: Two-Step EWPT 1st order 2nd order F F < φ 0 > One step Two step j φ φ Increasing m h New scalars • Step 1: EWSB along φ • Step 2: EWSB along H 36 Patel, R-M: arXiv 1212.5652 ; Blinov et al: 1505.05195
Two-Step EW Baryogenesis H j St’d Model Scalar Sector BSM Scalar Sector: at least one φ SU(2) L non-singlet plus possibly < φ 0 > gauge singlets: “partially 1 secluded sector CPV” 2 j Conventional one step EWSB Two step EWSB BSM CPV in φ H interactions: baryogenesis during step 1 Inoue, Ovanesyan, R-M: 1508.05404; 37 Patel & R-M: 1212.5652; Blinov, Kozaczuk, Morrissey: 1504.05195
Two-Step EW Baryogenesis Illustrative Model: New sector: “Real Triplet” Σ < φ 0 > Gauge singlet S H ! Set of “SM” fields: 2 HDM (SUSY: “TNMSSM”, Coriano…) Small entropy Quench dilution sphalerons Two CPV Phases: Triplet phase δ Σ : Baryogenesis δ S : Singlet phase Σ dark matter 38 Inoue, Ovanesyan, R-M: 1508.05404
Two-Step EW Baryogenesis & EDMs EDMs are Two Loop Two CPV Phases: Triplet phase δ Σ : δ S : Singlet phase Insensitive to δ S : electrically neutral ! “partially secluded” 39 Inoue, Ovanesyan, R-M: 1508.05404
Two-Step EW Baryogenesis Two cases: (A) δ S = 0 (B) δ Σ =0 Y B Present d e Present d e Future d n Future d p ? No EDM constraints Inoue, Ovanesyan, R-M: 1508.05404 40
Flavored EW Baryogenesis τ L EWBG by µ R φ ( x ) Flavor basis (high T) e j L Lepton ( Y E 1 ) ij Φ 1 + ( Y E Yukawa = − E i ⇥ ⇤ 2 ) ij Φ 2 R + h.c., L Mass basis (T=0) m f v κ τ (cos φ τ ¯ ττ + sin φ τ ¯ τ i γ 5 τ ) h. Guo, Li, Liu, R-M, Shu 1609.09849 Chiang, Fuyuto, Senaha 1607.07316 41
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