Testing Higgs Relaxation Leptogenesis: Why Isocurvature Is More Promising Than CP Violation

Transcription

1 Testing Higgs Relaxation Leptogenesis: Why Isocurvature Is More Promising Than CP Violation Lauren Pearce University of Illinois, Urbana-Champaign Based on: Alexander Kusenko, LP, Louis Yang, Phys.Rev.Lett. 114 (2015) no.6, Masahiro Kawasaki, LP, Louis Yang, Alexander Kusenko, Phys.Rev. D95 (2017) no.10, Lauren Pearce (UIUC) 1 / 23

2 Outline Outline Briefly review Higgs relaxation leptogenesis Lauren Pearce (UIUC) 2 / 23

3 Outline Outline Briefly review Higgs relaxation leptogenesis Focus on CP violation: Lauren Pearce (UIUC) 2 / 23

4 Outline Outline Briefly review Higgs relaxation leptogenesis Focus on CP violation: An effective O 6 operator obscures source of CP violation Lauren Pearce (UIUC) 2 / 23

5 Outline Outline Briefly review Higgs relaxation leptogenesis Focus on CP violation: An effective O 6 operator obscures source of CP violation Therefore CP constraints are not very restrictive Lauren Pearce (UIUC) 2 / 23

6 Outline Outline Briefly review Higgs relaxation leptogenesis Focus on CP violation: An effective O 6 operator obscures source of CP violation Therefore CP constraints are not very restrictive Test via cosmological isocurvature measurements? Lauren Pearce (UIUC) 2 / 23

7 Higgs Relaxation The Higgs Potential The LHC has found a Higgs boson with mass 125 GeV Lauren Pearce (UIUC) 3 / 23

8 Higgs Relaxation The Higgs Potential The LHC has found a Higgs boson with mass 125 GeV If we evolve the Standard Model RGE equation out to high scales, the Higgs potential becomes shallow, and even appears to have a second minimum Lauren Pearce (UIUC) 3 / 23

9 Higgs Relaxation The Higgs Potential The LHC has found a Higgs boson with mass 125 GeV If we evolve the Standard Model RGE equation out to high scales, the Higgs potential becomes shallow, and even appears to have a second minimum V (φ) φ Lauren Pearce (UIUC) 3 / 23

10 Higgs Relaxation Bunch & Davies (1978), Linde (1982) Hawking & Moss (1982) Inflation and the Higgs Potential During inflation, scalar fields with a shallow potential develop large VEVs: Lauren Pearce (UIUC) 4 / 23

11 Higgs Relaxation Bunch & Davies (1978), Linde (1982) Hawking & Moss (1982) Inflation and the Higgs Potential During inflation, scalar fields with a shallow potential develop large VEVs: VEV fluctuates to a large values (due to quantum fluctuations) V (φ) φ Lauren Pearce (UIUC) 4 / 23

12 Higgs Relaxation Bunch & Davies (1978), Linde (1982) Hawking & Moss (1982) Inflation and the Higgs Potential During inflation, scalar fields with a shallow potential develop large VEVs: VEV fluctuates to a large values (due to quantum fluctuations) Hubble friction from expansion of universe prevents from rolling back down φ + 3H φ + V φ = 0 V (φ) H φ Lauren Pearce (UIUC) 4 / 23

13 Higgs Relaxation Higgs Relaxation During reheating, the Hubble parameter decreases. V (φ) H φ Lauren Pearce (UIUC) 5 / 23

14 Higgs Relaxation Higgs Relaxation During reheating, the Hubble parameter decreases. When H(t) curvature of potential, Hubble friction no longer prevents the VEV from rolling down. V (φ) φ Lauren Pearce (UIUC) 5 / 23

15 Higgs Relaxation Higgs Relaxation During reheating, the Hubble parameter decreases. When H(t) curvature of potential, Hubble friction no longer prevents the VEV from rolling down. V (φ) φ Lauren Pearce (UIUC) 5 / 23

16 Higgs Relaxation Higgs Relaxation During reheating, the Hubble parameter decreases. When H(t) curvature of potential, Hubble friction no longer prevents the VEV from rolling down. V (φ) φ Lauren Pearce (UIUC) 5 / 23

17 Higgs Relaxation Higgs Relaxation During reheating, the Hubble parameter decreases. When H(t) curvature of potential, Hubble friction no longer prevents the VEV from rolling down. Naturally have an epoch with an evolving scalar VEV. V (φ) φ Lauren Pearce (UIUC) 5 / 23

18 Higgs Relaxation Leptogenesis Higgs relaxation leptogenesis Higgs relaxation + Spontaneous baryogenesis Lauren Pearce (UIUC) 6 / 23

19 Higgs Relaxation Leptogenesis Higgs relaxation leptogenesis Higgs relaxation + Spontaneous baryogenesis Where is CP violation hidden? Lauren Pearce (UIUC) 6 / 23

20 Higgs Relaxation Leptogenesis Higgs relaxation leptogenesis Higgs relaxation + Spontaneous baryogenesis Where is CP violation hidden? One of the differences between Higgs relaxation leptogenesis and spontaneous baryogenesis Lauren Pearce (UIUC) 6 / 23

21 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis Spontaneous baryogenesis models use an evolving VEV to produce a net particle asymmetry: Lauren Pearce (UIUC) 7 / 23

22 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis Spontaneous baryogenesis models use an evolving VEV to produce a net particle asymmetry: Consider the coupling: L (a/f )W W Lauren Pearce (UIUC) 7 / 23

23 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis Spontaneous baryogenesis models use an evolving VEV to produce a net particle asymmetry: Consider the coupling: L (a/f )W W a: Axion field, W : SU(2) gauge field, f : Axion coupling strength Lauren Pearce (UIUC) 7 / 23

24 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis Spontaneous baryogenesis models use an evolving VEV to produce a net particle asymmetry: Consider the coupling: L (a/f )W W a: Axion field, W : SU(2) gauge field, f : Axion coupling strength Using electroweak anomaly equation: (a/f ) µ j µ B+L Lauren Pearce (UIUC) 7 / 23

25 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis Spontaneous baryogenesis models use an evolving VEV to produce a net particle asymmetry: Consider the coupling: L (a/f )W W a: Axion field, W : SU(2) gauge field, f : Axion coupling strength Using electroweak anomaly equation: (a/f ) µ j µ B+L Integration by parts: ( µ a/f )j µ B+L Lauren Pearce (UIUC) 7 / 23

26 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis Spontaneous baryogenesis models use an evolving VEV to produce a net particle asymmetry: Consider the coupling: L (a/f )W W a: Axion field, W : SU(2) gauge field, f : Axion coupling strength Using electroweak anomaly equation: (a/f ) µ j µ B+L Integration by parts: ( µ a/f )j µ B+L When a has a time-dependent VEV a : L ( t a /f )n B+L Lauren Pearce (UIUC) 7 / 23

27 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis L ( t a /f )n B+L Lauren Pearce (UIUC) 8 / 23

28 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis L ( t a /f )n B+L If scatterings in plasma are rapid on the VEV evolution timescale: Lauren Pearce (UIUC) 8 / 23

29 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis L ( t a /f )n B+L If scatterings in plasma are rapid on the VEV evolution timescale: Treat VEV as a classical background when constructing Hamiltonian Lauren Pearce (UIUC) 8 / 23

30 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis L ( t a /f )n B+L If scatterings in plasma are rapid on the VEV evolution timescale: Treat VEV as a classical background when constructing Hamiltonian Effective chemical potential µ t a /f for B + L charge Lauren Pearce (UIUC) 8 / 23

31 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis L ( t a /f )n B+L If scatterings in plasma are rapid on the VEV evolution timescale: Treat VEV as a classical background when constructing Hamiltonian Effective chemical potential µ t a /f for B + L charge Lauren Pearce (UIUC) 8 / 23

32 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis L ( t a /f )n B+L If scatterings in plasma are rapid on the VEV evolution timescale: Treat VEV as a classical background when constructing Hamiltonian Effective chemical potential µ t a /f for B + L charge l, q Leads to l, q Lauren Pearce (UIUC) 8 / 23

33 Spontaneous Baryogenesis Dine et. al., Phys.Lett. B257 (1991) Cohen, Kaplan, Nelson Phys.Lett. B263 (1991) Spontaneous Baryogenesis L ( t a /f )n B+L If scatterings in plasma are rapid on the VEV evolution timescale: Treat VEV as a classical background when constructing Hamiltonian Effective chemical potential µ t a /f for B + L charge Scatterings with B- or L-number violation lead to asymmetry Lauren Pearce (UIUC) 8 / 23

34 Spontaneous Baryogenesis Dolgov & Freese Phys.Rev. D51 (1995) hep-ph/ Spontaneous Baryogenesis L ( t a /f )n B+L If scatterings in plasma are rapid on the VEV evolution timescale: Treat VEV as a classical background when constructing Hamiltonian Effective chemical potential µ t a /f for B + L charge Scatterings with B- or L-number violation lead to asymmetry If not, analyze asymmetric particle production using Bogoliubov analysis Lauren Pearce (UIUC) 8 / 23

35 Higgs Relaxation Leptogenesis Higgs Relaxation Leptogenesis Consider instead the operator: L ϕ2 Λ 2 W W, n ϕ : Higgs field Lauren Pearce (UIUC) 9 / 23

36 Higgs Relaxation Leptogenesis Higgs Relaxation Leptogenesis Consider instead the operator: L ϕ2 Λ 2 W W, n ϕ : Higgs field Following same steps as above gives: L µϕ 2 Λ 2 j µ B+L n Lauren Pearce (UIUC) 9 / 23

37 Higgs Relaxation Leptogenesis Higgs Relaxation Leptogenesis Consider instead the operator: L ϕ2 Λ 2 W W, n ϕ : Higgs field Following same steps as above gives: Higgs VEV φ = ϕ 2 gives: L µϕ 2 Λ 2 j µ B+L n L tφ 2 Λ 2 n B+L n Lauren Pearce (UIUC) 9 / 23

38 Higgs Relaxation Leptogenesis Higgs Relaxation Leptogenesis Consider instead the operator: L ϕ2 Λ 2 W W, n ϕ : Higgs field Following same steps as above gives: Higgs VEV φ = ϕ 2 gives: L µϕ 2 Λ 2 j µ B+L n L tφ 2 Λ 2 n B+L n If have B- or L-violating processes, produces a matter/antimatter asymmetry Lauren Pearce (UIUC) 9 / 23

39 Higgs Relaxation Leptogenesis Advantages The Higgs field exists & naturally acquires a large VEV during inflation Lauren Pearce (UIUC) 10 / 23

40 Higgs Relaxation Leptogenesis Advantages The Higgs field exists & naturally acquires a large VEV during inflation t φ 2 decreases during relaxation in every Hubble patch Lauren Pearce (UIUC) 10 / 23

41 Higgs Relaxation Leptogenesis Advantages The Higgs field exists & naturally acquires a large VEV during inflation t φ 2 decreases during relaxation in every Hubble patch Therefore same sign asymmetry in each Hubble patch Lauren Pearce (UIUC) 10 / 23

42 Higgs Relaxation Leptogenesis Advantages The Higgs field exists & naturally acquires a large VEV during inflation t φ 2 decreases during relaxation in every Hubble patch Therefore same sign asymmetry in each Hubble patch (Unlike t a ) Lauren Pearce (UIUC) 10 / 23

43 CP Violation & Higgs Relaxation Leptogenesis CPT & CP Note that ( t φ 2 /Λ n )n B+L breaks CPT Lauren Pearce (UIUC) 11 / 23

44 CP Violation & Higgs Relaxation Leptogenesis CPT & CP Note that ( t φ 2 /Λ n )n B+L breaks CPT (as does ( t a /f )n B+L ) Lauren Pearce (UIUC) 11 / 23

45 CP Violation & Higgs Relaxation Leptogenesis CPT & CP Note that ( t φ 2 /Λ n )n B+L breaks CPT (as does ( t a /f )n B+L ) However, this is dynamical CPT breaking, due to the evolving VEV Lauren Pearce (UIUC) 11 / 23

46 CP Violation & Higgs Relaxation Leptogenesis CPT & CP Note that ( t φ 2 /Λ n )n B+L breaks CPT (as does ( t a /f )n B+L ) However, this is dynamical CPT breaking, due to the evolving VEV Both aw W /f and ϕ 2 W W /Λ 2 n conserve CPT: C P T Psuedoscalar (a) Scalar (ϕ) Gauge fields (F F ) Lauren Pearce (UIUC) 11 / 23

47 CP Violation & Higgs Relaxation Leptogenesis CPT & CP Note that ( t φ 2 /Λ n )n B+L breaks CPT (as does ( t a /f )n B+L ) However, this is dynamical CPT breaking, due to the evolving VEV Both aw W /f and ϕ 2 W W /Λ 2 n conserve CPT: C P T Psuedoscalar (a) Scalar (ϕ) Gauge fields (F F ) However, the effective operator ϕ 2 W W /Λ 2 n does break CP... Lauren Pearce (UIUC) 11 / 23

48 CP Violation & Higgs Relaxation Leptogenesis CPT & CP Note that ( t φ 2 /Λ n )n B+L breaks CPT (as does ( t a /f )n B+L ) However, this is dynamical CPT breaking, due to the evolving VEV Both aw W /f and ϕ 2 W W /Λ 2 n conserve CPT: C P T Psuedoscalar (a) Scalar (ϕ) Gauge fields (F F ) However, the effective operator ϕ 2 W W /Λ 2 n does break CP... Λ n involves both the scale of new physics and the CP violation in this new sector Lauren Pearce (UIUC) 11 / 23

49 CP Violation & Higgs Relaxation Leptogenesis Building the ϕ 2 W W /Λ 2 n Operator I generally don t discuss model building much: Lauren Pearce (UIUC) 12 / 23

50 CP Violation & Higgs Relaxation Leptogenesis Building the ϕ 2 W W /Λ 2 n Operator I generally don t discuss model building much: All of our constraints & parameter space results depend only on Λn Lauren Pearce (UIUC) 12 / 23

51 CP Violation & Higgs Relaxation Leptogenesis Building the ϕ 2 W W /Λ 2 n Operator I generally don t discuss model building much: All of our constraints & parameter space results depend only on Λn But since this is a workshop on CP violation, I will discuss model building... Lauren Pearce (UIUC) 12 / 23

52 CP Violation & Model Building M. E. Shaposhnikov (1987) M. E. Shaposhnikov (1988) Standard Model As Shaposhnikov pointed out, this operator exists in the Standard Model: Lauren Pearce (UIUC) 13 / 23

53 CP Violation & Model Building M. E. Shaposhnikov (1987) M. E. Shaposhnikov (1988) Standard Model As Shaposhnikov pointed out, this operator exists in the Standard Model: (Works in basis in which diagonalizes SU(2) eigenstates, so Higgs couplings are not diagonal) Lauren Pearce (UIUC) 13 / 23

54 CP Violation & Model Building M. E. Shaposhnikov (1987) M. E. Shaposhnikov (1988) Standard Model As Shaposhnikov pointed out, this operator exists in the Standard Model: (Works in basis in which diagonalizes SU(2) eigenstates, so Higgs couplings are not diagonal) To pick up the CP-violating CKM phase, need to use all three generations of quarks: Lauren Pearce (UIUC) 13 / 23

55 CP Violation & Model Building M. E. Shaposhnikov (1987) M. E. Shaposhnikov (1988) Standard Model As Shaposhnikov pointed out, this operator exists in the Standard Model: (Works in basis in which diagonalizes SU(2) eigenstates, so Higgs couplings are not diagonal) To pick up the CP-violating CKM phase, need to use all three generations of quarks: L R L Lauren Pearce (UIUC) 13 / 23

56 CP Violation & Model Building M. E. Shaposhnikov (1987) M. E. Shaposhnikov (1988) Standard Model As Shaposhnikov pointed out, this operator exists in the Standard Model: (Works in basis in which diagonalizes SU(2) eigenstates, so Higgs couplings are not diagonal) To pick up the CP-violating CKM phase, need to use all three generations of quarks: L R L But this operator is extremely tiny: Lauren Pearce (UIUC) 13 / 23

57 CP Violation & Model Building M. E. Shaposhnikov (1987) M. E. Shaposhnikov (1988) Standard Model As Shaposhnikov pointed out, this operator exists in the Standard Model: (Works in basis in which diagonalizes SU(2) eigenstates, so Higgs couplings are not diagonal) To pick up the CP-violating CKM phase, need to use all three generations of quarks: L R L But this operator is extremely tiny: Small CP-violating phase Lauren Pearce (UIUC) 13 / 23

58 CP Violation & Model Building M. E. Shaposhnikov (1987) M. E. Shaposhnikov (1988) Standard Model As Shaposhnikov pointed out, this operator exists in the Standard Model: (Works in basis in which diagonalizes SU(2) eigenstates, so Higgs couplings are not diagonal) To pick up the CP-violating CKM phase, need to use all three generations of quarks: L R L But this operator is extremely tiny: Small CP-violating phase Small quark Yukawa couplings Lauren Pearce (UIUC) 13 / 23

59 CP Violation & Model Building L R L Model Building But there s a more serious problem as well: Lauren Pearce (UIUC) 14 / 23

60 CP Violation & Model Building L R L Model Building But there s a more serious problem as well: Quark masses Higgs VEV φ Lauren Pearce (UIUC) 14 / 23

61 CP Violation & Model Building L R L Model Building But there s a more serious problem as well: Quark masses Higgs VEV φ So Λ n φ Lauren Pearce (UIUC) 14 / 23

62 CP Violation & Model Building L R L Model Building But there s a more serious problem as well: Quark masses Higgs VEV φ So Λ n φ So the coefficient of the j µ B+L term is: ( ) ( ) φ 2 φ 2 µ Λ 2 µ n φ 2 = 0 Lauren Pearce (UIUC) 14 / 23

63 CP Violation & Model Building L R L Model Building A similar operator can be constructed using leptons: Lauren Pearce (UIUC) 14 / 23

64 CP Violation & Model Building L R L Model Building A similar operator can be constructed using leptons: (Even smaller Yukawas) Lauren Pearce (UIUC) 14 / 23

65 CP Violation & Model Building L R L Model Building A similar operator can be constructed using leptons: (Even smaller Yukawas) But scale Λ n M RH if RH neutrinos have a Majorana mass Lauren Pearce (UIUC) 14 / 23

66 CP Violation & Model Building L R L Model Building A similar operator can be constructed using leptons: (Even smaller Yukawas) But scale Λ n M RH if RH neutrinos have a Majorana mass Easiest solution: Copy the lepton sector, with larger Yukawa couplings and smaller Majorana masses Lauren Pearce (UIUC) 14 / 23

67 CP Violation & Model Building L R L Model Building A similar operator can be constructed using leptons: (Even smaller Yukawas) But scale Λ n M RH if RH neutrinos have a Majorana mass Easiest solution: Copy the lepton sector, with larger Yukawa couplings and smaller Majorana masses (Make sure Yukawa couplings are large enough that you don t disturb Higgs decays) Lauren Pearce (UIUC) 14 / 23

68 CP Violation & Model Building Basic Conditions Need to involve states that: Lauren Pearce (UIUC) 15 / 23

69 CP Violation & Model Building Basic Conditions Need to involve states that: Couple to the Higgs Lauren Pearce (UIUC) 15 / 23

70 CP Violation & Model Building Basic Conditions Need to involve states that: Couple to the Higgs Couple to the SU(2) gauge bosons Lauren Pearce (UIUC) 15 / 23

71 CP Violation & Model Building Basic Conditions Need to involve states that: Couple to the Higgs Couple to the SU(2) gauge bosons Do not (all) get their masses from the Higgs mechanism Lauren Pearce (UIUC) 15 / 23

72 CP Violation & Model Building Basic Conditions Need to involve states that: Couple to the Higgs Couple to the SU(2) gauge bosons Do not (all) get their masses from the Higgs mechanism Allow for additional CP violation Lauren Pearce (UIUC) 15 / 23

73 CP Violation & Model Building Basic Conditions Need to involve states that: Couple to the Higgs Couple to the SU(2) gauge bosons Do not (all) get their masses from the Higgs mechanism Allow for additional CP violation Several other options as well Lauren Pearce (UIUC) 15 / 23

74 CP Violation & Model Building Basic Conditions Need to involve states that: Couple to the Higgs Couple to the SU(2) gauge bosons Do not (all) get their masses from the Higgs mechanism Allow for additional CP violation Several other options as well Main Point We don t particularly care about the source of CP violation in the UV-complete theory, once the effective operator is constructed and the effective scale Λ n is known Lauren Pearce (UIUC) 15 / 23

75 Having Said That... In the Standard Model, the relevant parameter space is in the regime in which the use of effective field theory is questionable: Lauren Pearce (UIUC) 16 / 23

76 Having Said That... In the Standard Model, the relevant parameter space is in the regime in which the use of effective field theory is questionable: log(λn [GeV]) Λn < TMax Λn < ϕ Inflaton scale: Λ I = GeV x-axis: Inflaton decay scale Γ I, controls reheating creation of plasma in which /L interactions occur (Used RH neutrino for /L violation, masses set high enough to suppress thermal leptogenesis) log(γi [GeV]) Lauren Pearce (UIUC) 16 / 23

77 Having Said That... In the Standard Model, the relevant parameter space is in the regime in which the use of effective field theory is questionable: log(λn [GeV]) Λn < ϕ Λn < TMax Models with extended Higgs sector: Can protect flat direction Regime in which EFT is valid H. Gertov et. al., Phys.Rev. D93 (2016) no.11, log(γi [GeV]) Lauren Pearce (UIUC) 16 / 23

78 Having Said That... In the Standard Model, the relevant parameter space is in the regime in which the use of effective field theory is questionable: Relevant scales: Λ n 10 8 to GeV log(λn [GeV]) Λn < ϕ0 Λn < TMax log(γi [GeV]) Lauren Pearce (UIUC) 16 / 23

79 Having Said That... In the Standard Model, the relevant parameter space is in the regime in which the use of effective field theory is questionable: log(λn [GeV]) Λn < ϕ Λn < TMax Relevant scales: Λ n 10 8 to GeV (Not likely to be probed any time soon) log(γi [GeV]) Lauren Pearce (UIUC) 16 / 23

80 Having Said That... In the Standard Model, the relevant parameter space is in the regime in which the use of effective field theory is questionable: log(λn [GeV]) Λn < ϕ Λn < TMax Relevant scales: Λ n 10 8 to GeV (Not likely to be probed any time soon) Other observational consequences? log(γi [GeV]) Lauren Pearce (UIUC) 16 / 23

81 Isocurvature Perturbations VEV Variation The Fokker-Planck equation gives us the Higgs VEV averaged over many Hubble volumes Lauren Pearce (UIUC) 17 / 23

82 Isocurvature Perturbations VEV Variation The Fokker-Planck equation gives us the Higgs VEV averaged over many Hubble volumes Lauren Pearce (UIUC) 17 / 23

83 Isocurvature Perturbations VEV Variation The Fokker-Planck equation gives us the Higgs VEV averaged over many Hubble volumes The VEVs in individual Hubble volumes will vary φ 0 φ 0 φ 0 Lauren Pearce (UIUC) 17 / 23

84 Isocurvature Perturbations VEV Variation The Fokker-Planck equation gives us the Higgs VEV averaged over many Hubble volumes The VEVs in individual Hubble volumes will vary φ 0 φ 0 φ 0 Therefore, the final partial-antiparticle asymmetry also varies Lauren Pearce (UIUC) 17 / 23

85 Isocurvature Perturbations VEV Variation The Fokker-Planck equation gives us the Higgs VEV averaged over many Hubble volumes The VEVs in individual Hubble volumes will vary Therefore, the final partial-antiparticle asymmetry also varies Lauren Pearce (UIUC) 17 / 23

86 Isocurvature Perturbations Isocurvature Perturbations Because the Higgs VEV does not dominate the energy density of the universe, these are isocurvature perturbations Lauren Pearce (UIUC) 18 / 23

87 Isocurvature Perturbations S. Weinberg Phys.Rev. D70 (2004) astro-ph/ Isocurvature Perturbations Because the Higgs VEV does not dominate the energy density of the universe, these are isocurvature perturbations Weinberg has a famous theorem that isocurvature perturbations must decay when as the universe thermalizes... Lauren Pearce (UIUC) 18 / 23

88 Isocurvature Perturbations S. Weinberg Phys.Rev. D70 (2004) astro-ph/ Isocurvature Perturbations Because the Higgs VEV does not dominate the energy density of the universe, these are isocurvature perturbations Weinberg has a famous theorem that isocurvature perturbations must decay when as the universe thermalizes become adiabatic if the universe after inflation enters an era of local thermal equilibrium, with no non-zero conserved quantities Lauren Pearce (UIUC) 18 / 23

89 Isocurvature Perturbations Isocurvature Perturbations Because the Higgs VEV does not dominate the energy density of the universe, these are isocurvature perturbations Weinberg has a famous theorem that isocurvature perturbations must decay when as the universe thermalizes become adiabatic if the universe after inflation enters an era of local thermal equilibrium, with no non-zero conserved quantities In our scenario: isocurvature perturbations survive because they are carried along with nonzero lepton/baryon number Lauren Pearce (UIUC) 18 / 23

90 Isocurvature Perturbations Isocurvature Perturbations Because the Higgs VEV does not dominate the energy density of the universe, these are isocurvature perturbations Weinberg has a famous theorem that isocurvature perturbations must decay when as the universe thermalizes become adiabatic if the universe after inflation enters an era of local thermal equilibrium, with no non-zero conserved quantities In our scenario: isocurvature perturbations survive because they are carried along with nonzero lepton/baryon number Why Isocurvature? Few theories produce isocurvature perturbations Lauren Pearce (UIUC) 18 / 23

91 Isocurvature Perturbations Isocurvature Perturbations Because the Higgs VEV does not dominate the energy density of the universe, these are isocurvature perturbations Weinberg has a famous theorem that isocurvature perturbations must decay when as the universe thermalizes become adiabatic if the universe after inflation enters an era of local thermal equilibrium, with no non-zero conserved quantities In our scenario: isocurvature perturbations survive because they are carried along with nonzero lepton/baryon number Why Isocurvature? Few theories produce isocurvature perturbations Stringently constrained by CMB & Lyman α data Lauren Pearce (UIUC) 18 / 23

92 Isocurvature In fact, too strong... In fact, isocurvature constraints already rule out the naive version I ve introduced here (details below)! Lauren Pearce (UIUC) 19 / 23

93 Isocurvature In fact, too strong... In fact, isocurvature constraints already rule out the naive version I ve introduced here (details below)! Decrease amplitude of perturbations suppresses asymmetry Lauren Pearce (UIUC) 19 / 23

94 Isocurvature In fact, too strong... In fact, isocurvature constraints already rule out the naive version I ve introduced here (details below)! Decrease amplitude of perturbations suppresses asymmetry Cannot eliminate isocurvature perturbations! Lauren Pearce (UIUC) 19 / 23

95 Isocurvature In fact, too strong... In fact, isocurvature constraints already rule out the naive version I ve introduced here (details below)! Decrease amplitude of perturbations suppresses asymmetry Cannot eliminate isocurvature perturbations! But can shift to smaller scales via a Higgs-inflaton coupling: V (φ) Couplings I n φ m lead to I n φ m terms in the potential φ Lauren Pearce (UIUC) 19 / 23

96 Isocurvature In fact, too strong... In fact, isocurvature constraints already rule out the naive version I ve introduced here (details below)! Decrease amplitude of perturbations suppresses asymmetry Cannot eliminate isocurvature perturbations! But can shift to smaller scales via a Higgs-inflaton coupling: V (φ) Couplings I n φ m lead to I n φ m terms in the potential Can destroy flatness φ Lauren Pearce (UIUC) 19 / 23

97 Isocurvature In fact, too strong... In fact, isocurvature constraints already rule out the naive version I ve introduced here (details below)! Decrease amplitude of perturbations suppresses asymmetry Cannot eliminate isocurvature perturbations! But can shift to smaller scales via a Higgs-inflaton coupling: V (φ) Couplings I n φ m lead to I n φ m terms in the potential Can destroy flatness These terms 0 at the end of inflation φ Lauren Pearce (UIUC) 19 / 23

98 Isocurvature In fact, too strong... In fact, isocurvature constraints already rule out the naive version I ve introduced here (details below)! Decrease amplitude of perturbations suppresses asymmetry Cannot eliminate isocurvature perturbations! But can shift to smaller scales via a Higgs-inflaton coupling: V (φ) φ Couplings I n φ m lead to I n φ m terms in the potential Can destroy flatness These terms 0 at the end of inflation VEV grows only at end of inflation Lauren Pearce (UIUC) 19 / 23

99 Isocurvature In fact, too strong... In fact, isocurvature constraints already rule out the naive version I ve introduced here (details below)! Decrease amplitude of perturbations suppresses asymmetry Cannot eliminate isocurvature perturbations! But can shift to smaller scales via a Higgs-inflaton coupling: V (φ) φ Couplings I n φ m lead to I n φ m terms in the potential Can destroy flatness These terms 0 at the end of inflation VEV grows only at end of inflation Isocurvature only on small scales Lauren Pearce (UIUC) 19 / 23

100 Isocurvature Isocurvature & Small Structures Parameterize by N last, number of e-folds VEV grows through 10 6 T RH = GeV ks [Mpc -1 ] Λ I = GeV Λ I = GeV Λ I = GeV Lyman-α Forest constraint k s : Largest scale of isocurvature perturbations 10-4 CMB constraint N last of e-folds Lauren Pearce (UIUC) 20 / 23

101 Isocurvature Isocurvature & Small Structures Parameterize by N last, number of e-folds VEV grows through 10 6 T RH = GeV ks [Mpc -1 ] Λ I = GeV Λ I = GeV Λ I = GeV Lyman-α Forest constraint k s : Largest scale of isocurvature perturbations 10-4 CMB constraint N last of e-folds Decreases predictive power, obviously Lauren Pearce (UIUC) 20 / 23

102 Isocurvature Isocurvature & Small Structures Parameterize by N last, number of e-folds VEV grows through 10 6 T RH = GeV ks [Mpc -1 ] Λ I = GeV Λ I = GeV Λ I = GeV Lyman-α Forest constraint k s : Largest scale of isocurvature perturbations 10-4 CMB constraint N last of e-folds Decreases predictive power, obviously But perhaps has interesting consequences... Lauren Pearce (UIUC) 20 / 23

103 Isocurvature Isocurvature & Small Structures Power spectrum enhanced at small scales: 4 log(p(k) [h -3 Mpc 3 ]) Silk dampling Lyman-α Forest log(k [h/mpc]) Ad. z = 0 Ad. z = 10 Ad. z = 20 Iso. z = 0 Iso. z = 10 Iso. z = 20 Lauren Pearce (UIUC) 20 / 23

104 Isocurvature Isocurvature & Small Structures Power spectrum enhanced at small scales: 4 log(p(k) [h -3 Mpc 3 ]) Silk dampling Lyman-α Forest log(k [h/mpc]) Ad. z = 0 Ad. z = 10 Ad. z = 20 Iso. z = 0 Iso. z = 10 Iso. z = 20 Leads to small structures collapsing early Lauren Pearce (UIUC) 20 / 23

105 Isocurvature Kashlinsky et. al. Astrophys.J. 804 (2015) no.2, 99 arxiv: Cosmic Infrared Background Spitzer and Akari space telescopes have observed (source-subtracted) anisotropies in the cosmic infrared background (5 arcminutes, 2 5 µm, 0.09 nw m 2 sr 1 ). Lauren Pearce (UIUC) 21 / 23

106 Isocurvature Kashlinsky et. al. Astrophys.J. 804 (2015) no.2, 99 arxiv: Cosmic Infrared Background Spitzer and Akari space telescopes have observed (source-subtracted) anisotropies in the cosmic infrared background (5 arcminutes, 2 5 µm, 0.09 nw m 2 sr 1 ). From the anisotropy, can infer a large isotropic CIB flux Lauren Pearce (UIUC) 21 / 23

107 Isocurvature Kashlinsky et. al. Astrophys.J. 804 (2015) no.2, 99 arxiv: Cosmic Infrared Background Spitzer and Akari space telescopes have observed (source-subtracted) anisotropies in the cosmic infrared background (5 arcminutes, 2 5 µm, 0.09 nw m 2 sr 1 ). From the anisotropy, can infer a large isotropic CIB flux Can explain with early stars (z = 10) if mass fraction of baryons in star-forming collapsed halos, f halo, 0.2 Lauren Pearce (UIUC) 21 / 23

108 Isocurvature Kashlinsky et. al. Astrophys.J. 804 (2015) no.2, 99 arxiv: Cosmic Infrared Background Spitzer and Akari space telescopes have observed (source-subtracted) anisotropies in the cosmic infrared background (5 arcminutes, 2 5 µm, 0.09 nw m 2 sr 1 ). From the anisotropy, can infer a large isotropic CIB flux Can explain with early stars (z = 10) if mass fraction of baryons in star-forming collapsed halos, f halo, 0.2 But this is too large a value to accomodate in the usual cosmological picture Lauren Pearce (UIUC) 21 / 23

109 Isocurvature Early Stars However, we can nicely collapse the requisite small halos early without disturbing dwarf galaxy halos: 1 fhalo z Iso. with k s = 30 Mpc -1 Iso. with k s = 65 Mpc -1 Iso. with k s = 100 Mpc -1 Ad. Lauren Pearce (UIUC) 22 / 23

110 Isocurvature Early Stars However, we can nicely collapse the requisite small halos early without disturbing dwarf galaxy halos: 1 fhalo z Iso. with k s = 30 Mpc -1 Iso. with k s = 65 Mpc -1 Iso. with k s = 100 Mpc -1 Ad. Solid: Mass fraction of baryons in collapsed halos 10 6 M (star forming) Lauren Pearce (UIUC) 22 / 23

111 Isocurvature Early Stars However, we can nicely collapse the requisite small halos early without disturbing dwarf galaxy halos: 1 fhalo z Iso. with k s = 30 Mpc -1 Iso. with k s = 65 Mpc -1 Iso. with k s = 100 Mpc -1 Ad. Solid: Mass fraction of baryons in collapsed halos 10 6 M (star forming) Dashed: Mass fraction of baryons in collapsed halos 10 8 M (dwarf galaxy) Lauren Pearce (UIUC) 22 / 23

112 Isocurvature Early Stars However, we can nicely collapse the requisite small halos early without disturbing dwarf galaxy halos: 1 fhalo z Iso. with k s = 30 Mpc -1 Iso. with k s = 65 Mpc -1 Iso. with k s = 100 Mpc -1 Ad. By choosing N last, we can explain infrared excess in most of parameter space where also generate a large enough baryon asymmetry Lauren Pearce (UIUC) 22 / 23

113 Conclusions In Higgs Relaxation Leptogenesis Lauren Pearce (UIUC) 23 / 23

114 Conclusions In Higgs Relaxation Leptogenesis CP violation is required in the construction of the O 6 operator used in Higgs relaxation leptogenesis Lauren Pearce (UIUC) 23 / 23

115 Conclusions In Higgs Relaxation Leptogenesis CP violation is required in the construction of the O 6 operator used in Higgs relaxation leptogenesis However the relevant parameter, Λ n, depends both on the CP violation parameter and the scale of new physics Lauren Pearce (UIUC) 23 / 23

116 Conclusions In Higgs Relaxation Leptogenesis CP violation is required in the construction of the O 6 operator used in Higgs relaxation leptogenesis However the relevant parameter, Λ n, depends both on the CP violation parameter and the scale of new physics Isocurvature perturbations are necessarily produced... Lauren Pearce (UIUC) 23 / 23

117 Conclusions In Higgs Relaxation Leptogenesis CP violation is required in the construction of the O 6 operator used in Higgs relaxation leptogenesis However the relevant parameter, Λ n, depends both on the CP violation parameter and the scale of new physics Isocurvature perturbations are necessarily produced......which constrains the models (but can be used to explain the cosmic infrared excess) Lauren Pearce (UIUC) 23 / 23

118 Conclusions In Higgs Relaxation Leptogenesis CP violation is required in the construction of the O 6 operator used in Higgs relaxation leptogenesis However the relevant parameter, Λ n, depends both on the CP violation parameter and the scale of new physics Isocurvature perturbations are necessarily produced......which constrains the models (but can be used to explain the cosmic infrared excess) Thank you! Questions? Lauren Pearce (UIUC) 23 / 23

119 Back-Up Slides Back-Up Slides More model building Details of asymmetry calculation Lauren Pearce (UIUC) 1 / 6

120 Model Building Unusual Proposal We don t actually know why left-handed fermions couple to SU(2) and right-handed ones don t... Lauren Pearce (UIUC) 2 / 6

121 Model Building Unusual Proposal We don t actually know why left-handed fermions couple to SU(2) and right-handed ones don t... Introduce the following fields (Y W = Q T 3 ): Lauren Pearce (UIUC) 2 / 6

122 Model Building Unusual Proposal We don t actually know why left-handed fermions couple to SU(2) and right-handed ones don t... Introduce the following fields (Y W = Q T 3 ): ψdi (both left and right): SU(2) doublet, hypercharge 1/2 Lauren Pearce (UIUC) 2 / 6

123 Model Building Unusual Proposal We don t actually know why left-handed fermions couple to SU(2) and right-handed ones don t... Introduce the following fields (Y W = Q T 3 ): ψdi (both left and right): SU(2) doublet, hypercharge 1/2 Can construct mass term M ij ( ψ DLi ψ DRj + ψ DRj ψ DLi ) + h.c. Lauren Pearce (UIUC) 2 / 6

124 Model Building Unusual Proposal We don t actually know why left-handed fermions couple to SU(2) and right-handed ones don t... Introduce the following fields (Y W = Q T 3 ): ψdi (both left and right): SU(2) doublet, hypercharge 1/2 Can construct mass term M ij ( ψ DLi ψ DRj + ψ DRj ψ DLi ) + h.c. ψs (both left and right): SU(2) singlet, hypercharge 1 Lauren Pearce (UIUC) 2 / 6

125 Model Building Unusual Proposal We don t actually know why left-handed fermions couple to SU(2) and right-handed ones don t... Introduce the following fields (Y W = Q T 3 ): ψdi (both left and right): SU(2) doublet, hypercharge 1/2 Can construct mass term M ij ( ψ DLi ψ DRj + ψ DRj ψ DLi ) + h.c. ψs (both left and right): SU(2) singlet, hypercharge 1 Can construct mass term m( ψ SL ψ SR + ψ SR ψ SL ) Lauren Pearce (UIUC) 2 / 6

126 Model Building Unusual Proposal We don t actually know why left-handed fermions couple to SU(2) and right-handed ones don t... Introduce the following fields (Y W = Q T 3 ): ψdi (both left and right): SU(2) doublet, hypercharge 1/2 Can construct mass term M ij ( ψ DLi ψ DRj + ψ DRj ψ DLi ) + h.c. ψs (both left and right): SU(2) singlet, hypercharge 1 Can construct mass term m( ψ SL ψ SR + ψ SR ψ SL ) Can couple to SM Higgs ϕ: SU(2) doublet, hypercharge 1/2 via: Lauren Pearce (UIUC) 2 / 6

127 Model Building Unusual Proposal We don t actually know why left-handed fermions couple to SU(2) and right-handed ones don t... Introduce the following fields (Y W = Q T 3 ): ψdi (both left and right): SU(2) doublet, hypercharge 1/2 Can construct mass term M ij ( ψ DLi ψ DRj + ψ DRj ψ DLi ) + h.c. ψs (both left and right): SU(2) singlet, hypercharge 1 Can construct mass term m( ψ SL ψ SR + ψ SR ψ SL ) Can couple to SM Higgs ϕ: SU(2) doublet, hypercharge 1/2 via: y i e iδ i Φ( ψ DLi ψ SR + ψ DRi ψ SL ) + h.c. Lauren Pearce (UIUC) 2 / 6

128 Chemical Potential Higgs VEV Evolution To find the chemical potential as a function of time we need to know the evolution of the Higgs VEV in time. Lauren Pearce (UIUC) 3 / 6

129 Chemical Potential Higgs VEV Evolution To find the chemical potential as a function of time we need to know the evolution of the Higgs VEV in time. Equation of motion: φ + 3H(t) φ + V φ (φ, T (t)) = 0 Lauren Pearce (UIUC) 3 / 6

130 Chemical Potential Higgs VEV Evolution To find the chemical potential as a function of time we need to know the evolution of the Higgs VEV in time. Equation of motion: φ + 3H(t) φ + V φ (φ, T (t)) = 0 Include running couplings, one-loop correction, and finite temperature corrections in potential. Lauren Pearce (UIUC) 3 / 6

131 Chemical Potential Higgs VEV Evolution To find the chemical potential as a function of time we need to know the evolution of the Higgs VEV in time. Equation of motion: φ + 3H(t) φ + V φ (φ, T (t)) = 0 Include running couplings, one-loop correction, and finite temperature corrections in potential. Also include condensate decay; not an important effect. Lauren Pearce (UIUC) 3 / 6

132 Lepton Number Violation Lepton Number Violation µ eff 0 implies the energy of the system is minimized at n L 0. Lauren Pearce (UIUC) 4 / 6

133 Lepton Number Violation Lepton Number Violation µ eff 0 implies the energy of the system is minimized at n L 0. However, we still need a lepton-number-violating process to allow the system to relax to its minimum energy. Lauren Pearce (UIUC) 4 / 6

134 Lepton Number Violation Lepton Number Violation µ eff 0 implies the energy of the system is minimized at n L 0. However, we still need a lepton-number-violating process to allow the system to relax to its minimum energy. Use right-handed neutrinos to generate lepton-number-violating processes... h 0 h 0 h 0 h 0 NR N c R NR N c R νl ν c l νl ν c l νl h 0 ν c L h 0 NR N c R NR N c R νl h 0 ν c l h 0 Lauren Pearce (UIUC) 4 / 6

135 Lepton Number Violation Lepton Number Violation µ eff 0 implies the energy of the system is minimized at n L 0. However, we still need a lepton-number-violating process to allow the system to relax to its minimum energy. Use right-handed neutrinos to generate lepton-number-violating processes......but ensure T M R to suppress thermal leptogenesis! h 0 h 0 h 0 h 0 NR N c R NR N c R νl ν c l νl ν c l νl h 0 ν c L h 0 NR N c R NR N c R νl h 0 ν c l h 0 Lauren Pearce (UIUC) 4 / 6

136 Washout Washout µ eff t φ 2 changes sign as VEV oscilates. Lauren Pearce (UIUC) 5 / 6

137 Washout Washout µ eff t φ 2 changes sign as VEV oscilates. Drives production with opposite sign. Lauren Pearce (UIUC) 5 / 6

138 Washout Washout µ eff t φ 2 changes sign as VEV oscilates. Drives production with opposite sign. Options to suppress this washout: Lauren Pearce (UIUC) 5 / 6

139 Washout Washout µ eff t φ 2 changes sign as VEV oscilates. Drives production with opposite sign. Options to suppress this washout: Choose parameters such that the Higgs oscillation is significantly damped. Lauren Pearce (UIUC) 5 / 6

140 Washout Washout µ eff t φ 2 changes sign as VEV oscilates. Drives production with opposite sign. Options to suppress this washout: Choose parameters such that the Higgs oscillation is significantly damped. Choose parameters such that the asymmetry generation freezes out during the first swing (if it is even in equilibrium). Lauren Pearce (UIUC) 5 / 6

141 Washout Washout µ eff t φ 2 changes sign as VEV oscilates. Drives production with opposite sign. Options to suppress this washout: Choose parameters such that the Higgs oscillation is significantly damped. Choose parameters such that the asymmetry generation freezes out during the first swing (if it is even in equilibrium). T M R suppresses lepton-number-violating cross section. Lauren Pearce (UIUC) 5 / 6

142 Washout Washout µ eff t φ 2 changes sign as VEV oscilates. Drives production with opposite sign. Options to suppress this washout: Choose parameters such that the Higgs oscillation is significantly damped. Choose parameters such that the asymmetry generation freezes out during the first swing (if it is even in equilibrium). T M R suppresses lepton-number-violating cross section. Regime where thermal leptogenesis is inefficient automatically is regime where washout is suppressed! Lauren Pearce (UIUC) 5 / 6

143 Washout Small Cross Section Effects The small cross section is counteracted by large chemical potential µ eff (because the Higgs VEV relaxes (relatively) quickly compared to Hubble parameter). Lauren Pearce (UIUC) 6 / 6

144 Washout Small Cross Section Effects The small cross section is counteracted by large chemical potential µ eff (because the Higgs VEV relaxes (relatively) quickly compared to Hubble parameter). The system won t reach the equilibrium asymmetry, but approaches it. Lauren Pearce (UIUC) 6 / 6

145 Washout Small Cross Section Effects The small cross section is counteracted by large chemical potential µ eff (because the Higgs VEV relaxes (relatively) quickly compared to Hubble parameter). The system won t reach the equilibrium asymmetry, but approaches it. Production of asymmetry described by Boltzmann-style equation: d dt n L + 3Hn L 2 = π 2 T 3 σ R (n L 2π ) 2 µ eff T 2. Lauren Pearce (UIUC) 6 / 6