A Brief Introduction to Asymmetric Dark Matter Mattias Blennow - PowerPoint PPT Presentation

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions A Brief Introduction to Asymmetric Dark Matter Mattias Blennow Mattias.Blennow@mpi-hd.mpg.de Max–Planck–Institut f¨ ur Kernphysik June 27, 2012 @ GGI, Florence, Italy Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions 1 Asymmetric Dark Matter Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions 1 Asymmetric Dark Matter 2 Type I: Sharing Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions 1 Asymmetric Dark Matter 2 Type I: Sharing 3 Type II: Cogenesis Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions 1 Asymmetric Dark Matter 2 Type I: Sharing 3 Type II: Cogenesis 4 Summary and conclusions Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions 1 Asymmetric Dark Matter 2 Type I: Sharing 3 Type II: Cogenesis 4 Summary and conclusions Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation Beyond the Standard Model Hints for physics beyond the Standard Model: Dark Matter Dark Energy Neutrino oscillations Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation Beyond the Standard Model Hints for physics beyond the Standard Model: Dark Matter Dark Energy Neutrino oscillations Open questions What is the nature of DM? How is DM created? Why is Ω DM ∼ Ω b ? Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation Comparing Baryonic and Dark Matter Baryons Dark Matter Mass: Mass: m N ≃ 1 GeV Abundance: Abundance: n b / n γ = (6 . 19 ± 0 . 15) · 10 − 10 Density: Density: Ω b ≃ 0 . 046 Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation Comparing Baryonic and Dark Matter Baryons Dark Matter Mass: Mass: m DM = ? m N ≃ 1 GeV Abundance: Abundance: n b / n γ = (6 . 19 ± 0 . 15) · 10 − 10 Density: Density: Ω b ≃ 0 . 046 Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation Comparing Baryonic and Dark Matter Baryons Dark Matter Mass: Mass: m DM = ? m N ≃ 1 GeV Abundance: Abundance: n b / n γ = (6 . 19 ± 0 . 15) · 10 − 10 n DM = ? Density: Density: Ω b ≃ 0 . 046 Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation Comparing Baryonic and Dark Matter Baryons Dark Matter Mass: Mass: m DM = ? m N ≃ 1 GeV Abundance: Abundance: n b / n γ = (6 . 19 ± 0 . 15) · 10 − 10 n DM = ? Density: Density: Ω DM ≃ 0 . 23 Ω b ≃ 0 . 046 Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation Comparing Baryonic and Dark Matter Baryons Dark Matter Mass: Mass: m DM = ? m N ≃ 1 GeV Abundance: Abundance: n b / n γ = (6 . 19 ± 0 . 15) · 10 − 10 n DM = ? Density: Density: Ω DM ≃ 0 . 23 Ω b ≃ 0 . 046 Ω DM ≃ 5 Ω b Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation WIMP Dark Matter Theorists have a (unhealthy) predisposition to expect new physics at the TeV scale Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation WIMP Dark Matter Theorists have a (unhealthy) predisposition to expect new physics at the TeV scale Assume dark matter at the TeV scale, m DM ≃ 0 . 1 − 1 TeV Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation WIMP Dark Matter Theorists have a (unhealthy) predisposition to expect new physics at the TeV scale Assume dark matter at the TeV scale, m DM ≃ 0 . 1 − 1 TeV Assume dark matter is produced thermally in the early Universe Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation WIMP Dark Matter Theorists have a (unhealthy) predisposition to expect new physics at the TeV scale Assume dark matter at the TeV scale, m DM ≃ 0 . 1 − 1 TeV Assume dark matter is produced thermally in the early Universe = ⇒ Cross section of weak strength Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation WIMP Dark Matter Theorists have a (unhealthy) predisposition to expect new physics at the TeV scale Assume dark matter at the TeV scale, m DM ≃ 0 . 1 − 1 TeV Assume dark matter is produced thermally in the early Universe = ⇒ Cross section of weak strength Weakly Interacting Massive Particles (WIMPs) Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation WIMP Dark Matter Theorists have a (unhealthy) predisposition to expect new physics at the TeV scale Assume dark matter at the TeV scale, m DM ≃ 0 . 1 − 1 TeV Assume dark matter is produced thermally in the early Universe = ⇒ Cross section of weak strength Weakly Interacting Massive Particles (WIMPs) Great! Or is it? Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation The WIMP miracle Baryons WIMP Dark Matter Mass: Mass: m DM ≃ 1 TeV m N ≃ 1 GeV Abundance: Abundance: n DM ≃ 10 − 3 n b n b / n γ = (6 . 19 ± 0 . 15) · 10 − 10 Density: Density: Ω DM ≃ 0 . 23 Ω b ≃ 0 . 046 Ω DM ≃ 5 Ω b The WIMP miracle! Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation The WIMP miracle Baryons WIMP Dark Matter Mass: Mass: m DM ≃ 1 TeV m N ≃ 1 GeV Abundance: Abundance: n DM ≃ 10 − 3 n b n b / n γ = (6 . 19 ± 0 . 15) · 10 − 10 Thermal freezout NOT thermal production! Density: Density: Ω DM ≃ 0 . 23 Ω b ≃ 0 . 046 Ω DM ≃ 5 Ω b The WIMP miracle! Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter

Outline Asymmetric Dark Matter Type I: Sharing Type II: Cogenesis Summary and conclusions Motivation Facing the WIMP miracle If you like WIMPS: If you do not like WIMPS: “Just assuming new physics at “I dont believe that just by TeV scale, we derived that DM coincidence you would get the interacts with a weak scale cross same DM and baryon section to the SM. This fits my abundances when they have so expectations of how and where different masses and production new physics should be found.” mechanisms. I want DM and baryons to be more similar.” Mattias Blennow Max–Planck–Institut f¨ ur Kernphysik A Brief Introduction to Asymmetric Dark Matter