Spontaneous B L Breaking as the Origin of the Hot Early Universe - - PowerPoint PPT Presentation

▶
spontaneous b l breaking as the origin of the hot early
SMART_READER_LITE
LIVE PREVIEW

Spontaneous B L Breaking as the Origin of the Hot Early Universe - - PowerPoint PPT Presentation

Nov 20, 2023 573 likes •800 views

Spontaneous B L Breaking as the Origin of the Hot Early Universe Valerie Domcke DESY, Hamburg, Germany in collaboration with W. Buchm uller, K. Schmitz, K. Kamada arxiv[hep-ph]: 1202.6679, 1203.0285, 1305.3392 Spontaneous B L

slide-1
SLIDE 1

Spontaneous B−L Breaking as the Origin of the Hot Early Universe

Valerie Domcke DESY, Hamburg, Germany in collaboration with

  • W. Buchm¨

uller, K. Schmitz, K. Kamada arxiv[hep-ph]: 1202.6679, 1203.0285, 1305.3392

slide-2
SLIDE 2

Spontaneous B−L Breaking as the Origin of the Hot Early Universe

Valerie Domcke DESY, Hamburg, Germany in collaboration with

  • W. Buchm¨

uller, K. Schmitz, K. Kamada arxiv[hep-ph]: 1202.6679, 1203.0285, 1305.3392

slide-3
SLIDE 3

Spontaneous B−L Breaking as the Origin of the Hot Early Universe

Valerie Domcke DESY, Hamburg, Germany in collaboration with

  • W. Buchm¨

uller, K. Schmitz, K. Kamada arxiv[hep-ph]: 1202.6679, 1203.0285, 1305.3392

slide-4
SLIDE 4

Vanilla Cosmology?

Motivation

10 27 10 24 10 21 1018 1015 1012 109 106 103 100 103 106

energy [eV] time

LHC formation

  • f

light elements cosmic microwave background today

3 min 105 y 1010 y < 1 s

?

Valerie Domcke — DESY — 19.07.2013 — Page 2

slide-5
SLIDE 5

Motivation

Motivation

inflation entropy production matter - antimatter asymmetry dark matter

Valerie Domcke — DESY — 19.07.2013 — Page 3

slide-6
SLIDE 6

Motivation

Motivation

inflation entropy production matter - antimatter asymmetry dark matter spontaneous breaking

  • f U(1)B−L

Valerie Domcke — DESY — 19.07.2013 — Page 3

slide-7
SLIDE 7

Inflation

Motivation [Planck ’13] inflaton field scalar potential

exponential expansion driven by slowly rolling scalar field ‘stretched’ quantum fluctuations → inhomogeneities

  • f the cosmic microwave

background more a paradigm than a model

Valerie Domcke — DESY — 19.07.2013 — Page 4

slide-8
SLIDE 8

Entropy Production

Motivation

Expanding, cooling universe: Hot thermal plasma as initial state Reheating: generation of the thermal bath through decay of heavy particles perturbative process Preheating: rapid, nonperturbative process tachyonic preheating: triggered by tachyonic instability, exponential growth of low momentum modes

[Felder et al. ’01] Higgs field scalar potential

large abundance of non-relativistic Higgs bosons, small abundances of particles coupled to it

[Garcia-Bellido et al. ’02] Valerie Domcke — DESY — 19.07.2013 — Page 5

slide-9
SLIDE 9

Matter and Dark Matter

Motivation

Matter-Antimatter asymmetry small, but very significant B−L asymmetry: nB − n ¯

B

nγ = (6.19 ± 0.15) · 10−10

[Komatsu et al ’10]

leptogenesis: generate matter asymmetry dynamically in lepton sector, typically via decay of heavy Majorana neutrino transfer to baryon sector via SM processes (✘✘ ✘ B+L Sphalerons) Dark matter ... see earlier talks here: gravitino or neutralino dark matter

Valerie Domcke — DESY — 19.07.2013 — Page 6

slide-10
SLIDE 10

Adding U(1)B−L to the SM gauge group

Motivation

... see also Shaaban Khalil’s talk top-down approach: U(1)B−L as part of GUT group bottom-up approach: ’accidental’ global symmetry of the SM → gauge symmetry possible after introduction of right-handed neutrinos for anomaly cancellation spontaneously broken at GUT scale

Higgs field H i g g s fi e l d s c a l a r p

  • t

e n t i a l Valerie Domcke — DESY — 19.07.2013 — Page 7

slide-11
SLIDE 11

Outline

Motivation Towards a Consistent Cosmological Picture: Spontaneous B−L Breaking qualitative picture: linking inflation, leptogenesis and dark matter quantitative description: the reheating process in terms of Boltzmann equations Phenomenology Conclusion

Valerie Domcke — DESY — 19.07.2013 — Page 8

slide-12
SLIDE 12

A Phase Transition in the Early Universe

Spontaneous B−L Breaking Higgs field H i g g s fi e l d Higgs field H i g g s fi e l d

W = √ λ 2 Φ (v2

B−L − 2 S1S2) + 1

√ 2hn

i nc inc iS1 + hν ijnc i5∗ jHu + WMSSM

Before hybrid inflation

[Dvali et al. ’94]

Phase transition tachyonic preheating cosmic strings After reheating leptogenesis dark matter

Valerie Domcke — DESY — 19.07.2013 — Page 9

slide-13
SLIDE 13

A Phase Transition in the Early Universe

Spontaneous B−L Breaking H i g g s fi e l d inflaton field Higgs field H i g g s fi e l d Higgs field H i g g s fi e l d

W = √ λ 2 Φ (v2

B−L − 2 S1S2) + 1

√ 2hn

i nc inc iS1 + hν ijnc i5∗ jHu + WMSSM

Before hybrid inflation

[Dvali et al. ’94]

Phase transition tachyonic preheating cosmic strings After reheating leptogenesis dark matter

Valerie Domcke — DESY — 19.07.2013 — Page 9

slide-14
SLIDE 14

A Phase Transition in the Early Universe

Spontaneous B−L Breaking H i g g s fi e l d inflaton field Higgs field H i g g s fi e l d Higgs field H i g g s fi e l d

W = √ λ 2 Φ (v2

B−L − 2 S1S2) + 1

√ 2hn

i nc inc iS1 + hν ijnc i5∗ jHu + WMSSM

Before hybrid inflation

[Dvali et al. ’94]

Phase transition tachyonic preheating cosmic strings After reheating leptogenesis dark matter

Valerie Domcke — DESY — 19.07.2013 — Page 9

slide-15
SLIDE 15

A Phase Transition in the Early Universe

Spontaneous B−L Breaking H i g g s fi e l d inflaton field Higgs field H i g g s fi e l d Higgs field H i g g s fi e l d

W = √ λ 2 Φ (v2

B−L − 2 S1S2) + 1

√ 2hn

i nc inc iS1 + hν ijnc i5∗ jHu + WMSSM

Before hybrid inflation

[Dvali et al. ’94]

Phase transition tachyonic preheating cosmic strings After reheating leptogenesis dark matter

Valerie Domcke — DESY — 19.07.2013 — Page 9

slide-16
SLIDE 16

A Phase Transition in the Early Universe

Spontaneous B−L Breaking H i g g s fi e l d inflaton field Higgs field H i g g s fi e l d Higgs field H i g g s fi e l d

W = √ λ 2 Φ (v2

B−L − 2 S1S2) + 1

√ 2hn

i nc inc iS1 + hν ijnc i5∗ jHu + WMSSM

Before hybrid inflation

[Dvali et al. ’94]

Phase transition tachyonic preheating cosmic strings After reheating leptogenesis dark matter

Valerie Domcke — DESY — 19.07.2013 — Page 9

slide-17
SLIDE 17

A Phase Transition in the Early Universe

Spontaneous B−L Breaking H i g g s fi e l d inflaton field Higgs field H i g g s fi e l d Higgs field H i g g s fi e l d

W = √ λ 2 Φ (v2

B−L − 2 S1S2) + 1

√ 2hn

i nc inc iS1 + hν ijnc i5∗ jHu + WMSSM

SSB of B−L links inflation, (p)reheating, leptogenesis and DM

Valerie Domcke — DESY — 19.07.2013 — Page 9

slide-18
SLIDE 18

A Useful Tool: Boltzmann Equations

Spontaneous B−L Breaking

evolution of the phase space density fX(t, p): ˆ LfX(t, p) = ∂ ∂t − ˙ a a p ∂ ∂p

  • fX(t, p) =
  • CX

collision operator: CX(Xab.. ↔ ij..) = 1 2gXEX

  • dΠ(X|a, b, ..; i, j, ..)(2π)4δ(4)(Pout − Pin)

× [fifj..|M(ij.. → Xab..)|2 − fXfafb..|M(Xab.. → ij..)|2] Friedmann equation: 3M 2

P

˙

a a

2 = ρtot Calculating the time evolution of phase space densities

Valerie Domcke — DESY — 19.07.2013 — Page 10

slide-19
SLIDE 19

A Useful Tool: Boltzmann Equations

Spontaneous B−L Breaking

evolution of the phase space density fX(t, p): ˆ LfX(t, p) = ∂ ∂t − ˙ a a p ∂ ∂p

  • fX(t, p) =
  • CX

collision operator: CX(Xab.. ↔ ij..) = 1 2gXEX

  • dΠ(X|a, b, ..; i, j, ..)(2π)4δ(4)(Pout − Pin)

× [fifj..|M(ij.. → Xab..)|2 − fXfafb..|M(Xab.. → ij..)|2] Friedmann equation: 3M 2

P

˙

a a

2 = ρtot Calculating the time evolution of phase space densities

Valerie Domcke — DESY — 19.07.2013 — Page 10

slide-20
SLIDE 20

A Useful Tool: Boltzmann Equations

Spontaneous B−L Breaking

evolution of the phase space density fX(t, p): ˆ LfX(t, p) = ∂ ∂t − ˙ a a p ∂ ∂p

  • fX(t, p) =
  • CX

collision operator: CX(Xab.. ↔ ij..) = 1 2gXEX

  • dΠ(X|a, b, ..; i, j, ..)(2π)4δ(4)(Pout − Pin)

× [fifj..|M(ij.. → Xab..)|2 − fXfafb..|M(Xab.. → ij..)|2] Friedmann equation: 3M 2

P

˙

a a

2 = ρtot Calculating the time evolution of phase space densities

Valerie Domcke — DESY — 19.07.2013 — Page 10

slide-21
SLIDE 21

A Useful Tool: Boltzmann Equations

Spontaneous B−L Breaking

evolution of the phase space density fX(t, p): ˆ LfX(t, p) = ∂ ∂t − ˙ a a p ∂ ∂p

  • fX(t, p) =
  • CX

collision operator: CX(Xab.. ↔ ij..) = 1 2gXEX

  • dΠ(X|a, b, ..; i, j, ..)(2π)4δ(4)(Pout − Pin)

× [fifj..|M(ij.. → Xab..)|2 − fXfafb..|M(Xab.. → ij..)|2] Friedmann equation: 3M 2

P

˙

a a

2 = ρtot Calculating the time evolution of phase space densities

Valerie Domcke — DESY — 19.07.2013 — Page 10