Electroweak Baryogenesis in Non-Standard Cosmology · Electroweak Baryogenesis in Non-Standard Cosmology Germano Nardini Universitat Bielefeld¨..... KOSMOLOGIETAG ’12..... Related

Electroweak Baryogenesis inNon-Standard Cosmology

Germano Nardini

Universitat Bielefeld

.............................KOSMOLOGIETAG ’12

.............................

Related to works in colloboration withM. Carena, A. Delgado, A. De Simone, M. Quiros,

A. Riotto, N. Sahu, C. Wagner

Germano Nardini EWBG in non-standard cosmology

Outline

Outline

1 EWBG Mechanism Review

2 Effective Theory of the LSS (MSSM)

3 EWBG in the MSSM (Standard Cosmology)

4 EWBG in the MSSM (Non-Standard Cosmology)


EWBG Mechanism Review

The Question: Why this asymmetry?

The Universe is populated by matter. BBN and CMB furnishindependently:

η ≡ nB − nB

nγ= (6.11± 0.19)× 10−10

Mechanisms attempting to produce η must contain theingredients [Sakharov,1967] (if CPT symmetry)

1 B violation

2 C and CP violation

3 Departure from thermal equilibrium

How did the Universe arrive to this asymmetry?

One possible mechanism: EWBG (alternatives: Drewes,Domcke,Wu,Herranen’s talks)



EWBG in the SM and MSSM

Kuzmin, Rubakov and Shapshnikov, Phys.Lett.B155:36,1985;.........

Some EWBG reviews:M. Quiros, hep-ph/9901312A. Riotto, hep-ph/9807454J. Cline, hep-ph/0609145

SM(even with mν = 0) and MSSM contain the Sakh. condts:1 B number is non-perturbative violated

at T 6= 0 (sphalerons) [’t Hooft,76]��

��

L

L

L

Q

Q

Qτ

e

µ

1

2

32 CKM matrix (SM) or Soft Breaking terms (MSSM)contain CP violating phases

3 EWPT (when of 1st order) proceeds by bubble nucleation.Expanding bubbles break the thermal equilibrium.




V (φ, T ) ≃ m(T )φ2 + F (T )φ3 + λ(T )φ4

φ



��

L

L

L

Q

Q

Qτ

e

µ

1

2






V (φ, T ) ≃ m(T )φ2 + F (T )φ3 + λ(T )φ4

φ

φ =0φ >0

φ >0

φ >0

φ >0

φ >0

φ >0

⇒ .



��

L

L

L

Q

Q

Qτ

e

µ

1

2






V (φ, T ) ≃ m(T )φ2 + F (T )φ3 + λ(T )φ4

φ

CP asymmetry

z

wall

φ 6= 0

φ = 0

qL>qL⇒ .

In (front of) the wall CP asymm. generates temporally qL > qL⇒ There are more sphalerons B↑ than those B↓⇒ Temporally B asymm. is present beyond the wall ⇒ The wallexpansion introduces B > 0 inside the bubble, where

it remains there forever IF sphalerons do not wash out it!!!




Sphalerons do not wash out η if ...

Dilution: “Bf ∼ Bi exp[−Γsp(Tn)/H]”

Γsp(Tn) = KTn e−

Esp(Tn)

Tn

⇓ (taking H in rad. era).

Esp(Tn) & 35 Tn

⇓〈φ(Tn)〉 & Tn

... the 1st order phase transition is STRONG




EWBG in the SM is ruled out:

The EWPT turns out not to be strong for mh > 75GeV[Kajantie et al.,97]

Small CP asymmetry

And in the MSSM ?New physics at the EW scale may modify the EWPT

New couplings violating CP


Effective Theory

LSS Framework [Carena et al.,96;Delepine et al.,96;Cline et al.,98]

The main features of the LSS spectrum are:

Fermions are at the EW scale (gluino may be a bit heavy)

The tR is lighter than the top quark

The other scalars MQ ≃ mA ≃ ... ≡ m ≫ few TeV

At ≪ m (enhancing the strength of the EWPT)

(A sort of light-stop scenario in SS)

⇓LOW ENERGY EFFECTIVE THEORY

(to avoid large logs)

[Carena,GN,Quiros,Wagner 08,09]


Effective Theory

LE Lagrangian [Carena,GN,Quiros,Wagner 08,09]

The effective Lagrangian is

Leff = m2H†H − λ

2

(H†H

)2 − ht [qLǫH∗tR] + Yt

[HuǫqLt

∗R

]

−√2G Θg tRg

aTatR +

√2J t∗RBtR − 1

6K|tR|2 |tR|2 −Q

∣∣tR∣∣2 |H|2

+H†√2

(guσ

aW a + g′uB)Hu +

HT ǫ√2

(−gdσ

aW a + g′dB)Hd + h.c.

−M3

2Θg g

aga − M2

2WAWA − M1

2BB − µHT

u ǫHd −M2U t∗RtR

EEW (M3) m

tL, bL, Hh, . . .SUSYEFF.


EWBG in the MSSM (Standard Cosmology)

Higgs-Stop window 〈φ(Tn)〉/Tn > 1 (µ = 100,M3 = 500)

Condt. 1: tanβ . 15 by EDM and BAUCondt. 2: stab. or metastab. (Tn

SP→CB < T fSP→EWB)

Based on effect. parameters. g3, ht 2-loops T 6= 0 at g3, ht approx

For EDM: Chang et al.,99For BAU: Carena et al.,03; Konstandin et al.,06; D. J. H. Chung et.al.,09

m = 500 TeV m = 8000 TeV

1 1

2 2



Higgs-Stop window 〈φ(Tn)〉/Tn > 1 (µ = 100,M3 = 500)

Condt. 1: tanβ . 15 by EDM and BAUCondt. 2: stab. or metastab. (Tn

SP→CB < T fSP→EWB)

EWBG bounds (LEP bound):

mh . 127 GeV mtR. 120 GeV

m & 7 TeV

m = 500 TeV m = 8000 TeV

1 1

2 2



Produced B-asymmetry

Different approaches: Carena et al.,03; Konstandin et al.,06;D. J. H. Chung et.al.,09. We apply the intermediate one

2 4 6 8 10 12 14 16 18 20 22 24 26 28 300

2

4

6

8

10

µ = 100 GeV sin φ = 1µ = 250 GeV sin φ = 1µ = 100 GeV sin φ = 0.6µ = 250 GeV sin φ = 0.6

η/ηBBN

tanβ

Calculation strongly depends on details (M1,M2, µ):

⇓Good choice: tanβ ≤ 15 Very conservative: tanβ ≤ 5


EWBG in the MSSM (Non-Standard Cosmology)

Relaxing Assumption (NON-SC)

-14 -12 -10 -8 -6 -4 -2 0-14 -12 -10 -8 -6 0

replacements

〈φ(Tn)〉Tn

>1

〈φ(Tn)〉Tn

<1

log10 Γ

log10GeVT

T = O(100 GeV) radiation domination



Relaxing Assumption [Joyce et al.’98]

-14 -12 -10 -8 -6 -4 -2 0-14 -12 -10 -8 -6 0

replacements

〈φ(Tn)〉Tn

>1

〈φ(Tn)〉Tn

<1

log10 Γ

log10GeVT

.

No entropy injection(gain strength,loose η)

[GN, Sahu 11]

Fig. from ’Particle Dark Matter: Observations, Models and Searches’, edited by G. Bertone



Relaxing Assumption [Joyce et al.’98]

-14 -12 -10 -8 -6 -4 -2 0-14 -12 -10 -8 -6 0

〈φ(Tn)〉Tn

>1

〈φ(Tn)〉Tn

<1

log10 Γ

log10GeVT

Sphal. in equil. in unbroken phase

Hew/Hsc < 1011

Sphal. out-of-equil. in broken phase

〈φ(T )〉T

∣∣∣T=Tn

> D + 135 log

HscHew

, D = 1



Relaxed window [Carena,GN,Quiros,Wagner in progress]

Hew/Hsc = 1, 103, 106

112 114 116 118 120 122

95

100

105

110

115

120

125

m = 8TeV

mh [GeV]

mt

[GeV

]

112 114 116 118 120 122 124 126 128 130 132

95

100

105

110

115

120

125

m = 106 TeV

mh [GeV]

mt

[GeV

]New upper bounds: mh . 135GeV and mt . 125GeV

New parameter region of the effective couplings: different fingerprintof LSS at LHC for SC/NSC?



Minimal m for (mh,mtR) = (114.7, 95)GeV

100

101

102

103

104

105

106

107

108

109

4000

5000

6000

7000

Hew/Hsc

m[G

eV]

larger Hew/Hsc, less hierarchy problem !



Conclusions

Hew = Hsc ⇒ mh . 127 ,GeV, mt . 120GeV

Hew 6= Hsc ⇒ mh . 135 GeV, mt . 125 GeV

GW [D.Chung et al.’10]

Growth of DM (if freeze-out) → no neutralino DM[M.Kamionkowski et al.’90]

Magnetic field evolution ? [T.Stevens et al.’11]

At LHC signatures different from SC? [Menon et al.’09, Cohen etal.’12, Curtin et al.’12, Carena,GN,Quiros,Wagner ’12*]

Applied on MSSM, but general!



Why EWBG interesting? Pheno connections with

In cosmology (at the electroweak epoch):

Primordial magnetic field

Gravitational waves

Pre-BBN cosmology

...

In particle physics (new physics at the EW scale):

Signatures at colliders

Precision physics (EDMs, ...)

...



bkp



Stop-neutralino

]2 Stop Mass [GeV/c

60 80 100 120 140 160 180

]2

Neu

tral

ino

Mas

s [G

eV/c

40

60

80

100

120

]2 Stop Mass [GeV/c

60 80 100 120 140 160 180

]2

Neu

tral

ino

Mas

s [G

eV/c

40

60

80

100

120

Observed Limit (95% CL)

)σ1±Expected Limit (

]2 Stop Mass [GeV/c

60 80 100 120 140 160 180

]2

Neu

tral

ino

Mas

s [G

eV/c

40

60

80

100

120

c

+ m

1o

χ∼

= m

t~m

1o

χ∼

+ m

b

+ m

W

= m

t~

m

o = 56θLEP o = 0θLEP

-1CDF 295 pb

-1DØ 995 pb

CDF Run II Preliminary -1

L dt=2.6 fb∫



Matter-Decay Domination

te τ

ΡX

ΡR

S

ΡX

ΡR

19 20 21 22 23-2

0

2

4

6

Log10@t/GeV−1

D

Log 1

0@Ρ

�ΡX

HΤL

D

3 �

4S�

S i

Hew

Hsc

.Hew

Hsc

∣∣∣∣t≡

√teτ

.

√ρXρR

∣∣∣∣t

≃ ρ+Rρ−R

∣∣∣∣1/4

t=τ

= ∆1/6 =

(ηmax

ηexp

)1/6

NO ENHANCEMENT!



bkp



Gauge Coupling Unification

EWBG suggests m ≫TeV. Large modif. from the usualparameter region of the MSSM, which unifies.

EWBG compatible with unification?

(4π)2 ddtgi = g3i bi+

+g3i

(4π)2

[∑3j=1Bijg

2j − dui h

2t − dGi G

2 − dJi J2 − · · ·

]g21 = (5/3)g′2

bLSS =(143

30,− 7

6,− 41

6+ 2Θg

)

bSUSY =(33

5,−2,−3

)

mZ

m

MGUT



Gauge Coupling Unification

EWBG suggests m ≫TeV. Large modif. from the usualparameter region of the MSSM, which unifies.

EWBG compatible with unification? YES

103

104

105

106

107

1080.11

0.112

0.114

0.116

0.118

0.12

0.122

0.124

0.126

0.128

0.13

α3(M

Z)

m [GeV]

1-σ prediction:

M3 = 500GeV:m = 103.3±0.6 TeV

M3 = 150GeV:m = 101.6±0.6 TeV



Metastability

Is the transition EWB→CB possible ? NO

150 100 50 0 50 100 150 200

-2e+06 -2e+06

0 0

2e+06 2e+06

4e+06 4e+06

V[G

eV4]

←t | h→300 200 100 0 100 200 300

-2e+08

-1.5e+08

-1e+08

-5e+07

0

V[G

eV4]

←t | h→

SEWB→CB ≫ 135

IT DOESN’T DECAY !60 70 80 90 100 110 120

T0

1000

2000

3000

4000

5000

6000

S 3 / T

Tnh



Carena, Quiros, Riotto, Vilja, Wagner Nucl.PhysB 503Germano Nardini EWBG in non-standard cosmology


mA = 2000GeV

mA = 300GeV

D. Curtin, P. Jaiswal, P. Meade, arXiv:1203.2932Germano Nardini EWBG in non-standard cosmology

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Electroweak Baryogenesis in Non-Standard Cosmology · Electroweak Baryogenesis in Non-Standard Cosmology Germano Nardini Universitat Bielefeld¨..... KOSMOLOGIETAG ’12..... Related