Dark Matter in Particle Physics
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1 High Energy Theory Group, Northwestern University July, 2006
2 Outline Framework - General Relativity and Particle Physics Observed Universe and Inference Dark Energy, (DM) DM DM Direct Detection DM at Colliders
3 The Framework General Relativity Particle Physics Einstein s General Theory of Relativity (GR) In GR 4 dim space-time is dynamical Mass/Energy curves space-time: Curvature Energy-density (ρ) Define Ω = ρ ρ c ρ c is critical energy-density (a constant) All forms of matter/energy contributes to ρ - Particle Physics
4 General Relativity Particle Physics The Standard Model of Particle Physics Since E = m c 2, same unit for mass and energy: ev (set c = 1) 1GeV = 109 ev institution-logo
5 General Relativity Particle Physics The Standard Model of Particle Physics Since E = m c 2, same unit for mass and energy: ev (set c = 1) Building blocks: 1GeV = 109 ev Composites: [particleadventure.org] institution-logo
6 General Relativity Particle Physics The Standard Model of Particle Physics Since E = m c 2, same unit for mass and energy: ev (set c = 1) Building blocks: 1GeV = 109 ev Composites: [particleadventure.org] Big-Bang Neucleosynthesis (BBN) explains element (D, He, Li,...) abundances in the universe institution-logo
7 The Observed Universe The universe is expanding [Hubble] General Relativity Particle Physics [Riess, Press and Kirshner (1996)]
8 The Observed Universe The universe is expanding [Hubble] General Relativity Particle Physics [Riess, Press and Kirshner (1996)] Galaxy Rotation curve, Gravitational lensing
9 The Observed Universe The universe is expanding [Hubble] General Relativity Particle Physics [Riess, Press and Kirshner (1996)] Galaxy Rotation curve, Gravitational lensing Cosmic Microwave Background (CMB) WMAP [NASA/WMAP Science Team]
10 The Observed Universe The universe is expanding [Hubble] General Relativity Particle Physics [Riess, Press and Kirshner (1996)] Galaxy Rotation curve, Gravitational lensing Cosmic Microwave Background (CMB) WMAP [NASA/WMAP Science Team] Galaxy Clusters, Chandra, Ly α, 2dF, SDSS
![Team] Galaxy Clusters, Chandra, Ly α,](/docs-images/89/98493273/images/11-4.jpg "2dF, SDSS Supernova Cosmology Project")
11 The Observed Universe The universe is expanding [Hubble] General Relativity Particle Physics [Riess, Press and Kirshner (1996)] Galaxy Rotation curve, Gravitational lensing Cosmic Microwave Background (CMB) WMAP [NASA/WMAP Science Team] Galaxy Clusters, Chandra, Ly α, 2dF, SDSS Supernova Cosmology Project institution-logo
12 Inference General Relativity Particle Physics The universe [wikipedia] Flat on large scales Expansion is Accelerating 95% is unknown dark matter + dark energy - What is it??
13 Inference General Relativity Particle Physics The universe [wikipedia] Flat on large scales Expansion is Accelerating 95% is unknown dark matter + dark energy - What is it?? The DARK SIDE rules!!! institution-logo
14 General Relativity Particle Physics institution-logo [Mike Turner, Neutrino 2006]
15 General Relativity Particle Physics institution-logo
16 candidates Astrophysical objects - Disfavored MAssive Compact Halo Object (MACHO) Black holes
17 candidates Astrophysical objects - Disfavored MAssive Compact Halo Object (MACHO) Black holes Particle Axions Neutrinos Weakly Interacting Massive Particle (WIMP) Super-WIMP,E-WIMP,WIMPzilla LSP, LKP, LTP
18 Axions Strong interactions - Quantum Chromo Dynamics (QCD) Charge-Parity (CP) symmetry conserved - Why??? Possible explanation - Axion [Peccei-Quinn] Ω m = ( 10 5 ev m a ) 7/6 m a = 6 ev ( 106 GeV f a )
19 Axions Strong interactions - Quantum Chromo Dynamics (QCD) Charge-Parity (CP) symmetry conserved - Why??? Possible explanation - Axion [Peccei-Quinn] Ω m = ( 10 5 ev m a ) 7/6 m a = 6 ev ( 106 GeV f a ) CERN Axion Solar Telescope (CAST)
![?? Possible explanation - Axion [Peccei-Quinn] Ω m = ( 10 5 ev m a](/docs-images/89/98493273/images/20-1.jpg ") 7/6 m a = 6 ev ( 106 GeV f a ) CERN Axion Solar Telescope (CAST)")
20 Axions Strong interactions - Quantum Chromo Dynamics (QCD) Charge-Parity (CP) symmetry conserved - Why??? Possible explanation - Axion [Peccei-Quinn] Ω m = ( 10 5 ev m a ) 7/6 m a = 6 ev ( 106 GeV f a ) CERN Axion Solar Telescope (CAST) Axion Expt. (ADMX) institution-logo
21 Neutrinos Neutrinos interact weakly Billions (from Sun) passing through you w/o interacting
22 Neutrinos Neutrinos interact weakly Billions (from Sun) passing through you w/o interacting Hot dark matter - freestreaming destroys structure Cannot be all of dark-matter Ω = 0.02 mν 1 ev [Dodelson]
23 Neutrinos Neutrinos interact weakly Billions (from Sun) passing through you w/o interacting Hot dark matter - freestreaming destroys structure Cannot be all of dark-matter Ω = 0.02 mν 1 ev [Dodelson] Right-handed Neutrino (Sterile Neutrino) can be DM Warm Solves many puzzles : LSND, Small scale structure, etc. institution-logo
24 Weakly Interacting Massive Particle (WIMP) WIMP Cold dark matter - New particle M 100 GeV Weak-interaction like coupling
25 Weakly Interacting Massive Particle (WIMP) WIMP Cold dark matter - New particle M 100 GeV Weak-interaction like coupling Most studied extension of the SM - Supersymmetry Extension of space-time symmetry to Superspace Boson Fermion symmetry. Every known particle has a Superpartner Lightest Supersymmetric Particle (LSP) can be stable LSP can be WIMP dark-matter. Eg. Neutralino
26 Other candidates SuperWIMP - Gravitino (partner of graviton) E-WIMP - Right-handed sneutrino (partner of neutrino) WIMPzilla - Extremely massive particle LKP - Lightest Kaluza-Klein Particle - Extra space dimensions LTP - Lightest T-odd Particle - Little-higgs theory with Z 2
27 Other candidates SuperWIMP - Gravitino (partner of graviton) E-WIMP - Right-handed sneutrino (partner of neutrino) WIMPzilla - Extremely massive particle LKP - Lightest Kaluza-Klein Particle - Extra space dimensions LTP - Lightest T-odd Particle - Little-higgs theory with Z 2 Your candidate here
28 DM direct detection Cryogenic Search (CDMS), Soudan Mine, USA Ge detector
29 DM direct detection Cryogenic Search (CDMS), Soudan Mine, USA DAMA, Gran Sasso, Italy. Detection claimed!! Ge detector NaI scintillators institution-logo
30 DM at Colliders I Fermilab: Tevatron, CDF, D0 institution-logo
31 DM at Colliders I Fermilab: Tevatron, CDF, D0 CERN: Large Hadron Collider (LHC), ATLAS, CMS institution-logo
32 DM at Colliders I Fermilab: Tevatron, CDF, D0 CERN: Large Hadron Collider (LHC), ATLAS, CMS institution-logo The Future: Linear Collider:
33 DM at Colliders II Example: Supersymmetry tr, br, g (YN) l + Hu (YN) l + Hu Hd X tr (Yt) ÑR br (Yb) ÑR bl tl LSP leads to missing momentum
34 Final Thoughts What is Dark Energy and??? Many, Mass range 10 5 ev GeV Vigorous search underway - Direct and Collider Exciting times! We might discover DM particle soon Dark Energy - Only for the brave!
35 Backup Slides Backup Slides
36 Ω m WMAP result (2003) Ω mh 2 = ; h2 0.5
37 Thermal History of the Universe Big Bang Inflation BBN Today Hubble rate: H ȧ a ; H = 1.66 g T 2 H2 = 8πG 3 ρ M Pl (Rad Dom)
38 Boltzmann Equation Big Bang Inflation BBN Today d ( ) dt n ν 0 = 3Hn ν0 σv SI n 2 ν 0 n 2 ν ( ) 0 eq σv CI n ν0 n φ n ν0 eqn φ eq + CΓ Thermal equilibrium if σv SI n ν0 > 3H ; σv CI n φ > 3H Freeze-out Ω 0 n 0M ρ c [Kolb & Turner, Early Universe] ( ) GeV 2 σv institution-logo
39 Mixed ν 0 ~ N 1 ~ N 1 (ig s 2 1P R ) W ~ 3 c W ~ 3 (ig s 2 1P R ) ν ν Ω 0 h 2 = 10 4 s 4 1 ( [g 2 ) ( 100 GeV + g 2 M W 100 GeV M B )] 2 1 s results in observed relic density
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