Recomendados
Recomendados
Mais conteúdo relacionado
Mais procurados
Mais procurados (20)
Semelhante a Caldwell seminar
Semelhante a Caldwell seminar (10)
Último
Último (20)
Caldwell seminar
- 7. cosmic whirls Right ascension [deg.] Declination[deg.] BICEP2: B signal 0.3μK −50050 −65 −60 −55 −50 −0.3 0 0.3 μK BICEP2 2014 BICEP2 / KECK x Planck 2015 Infla%onary gravita%onal waves? Not so fast! The search conGnues…
- 9. What Is Infla%on? A burst of expansion in which the early Universe grows exponenGally in Gme It puts the BANG in the BIG BANG InflaGon is the physics of a cosmic scalar field V φ Slow roll: @V/@ ⌧ 3H ˙ H ⌘ d ln a dt ' constant ! a / eHt The scale of the Universe grows exponenGally H ' 1014 GeV ! t ' 10 36 sec, ln a/ai ' 60 Solves the horizon problem! A clean slate for the observable Universe! ✏ ⌘ ˙H/H2 ⌧ 1 ¨ + 3H ˙ + V, = 0
- 10. Space-Gme distorGon hij as a quantum field Classical Pendulum: very boring. Quantum Pendulum: very exciGng! initial final Ei = 1 2 ~!i Ef = 1 4 ~!i !i = p g/Li !f = p g/Lf ni = 0 nf = !i/4!f initial final Ei = 1 2 ~!i Ef = 1 2 ~!f !i = p g/Li !f = p g/Lf ni = 0 nf = 0 Let the rope out quickly Let the rope out slowly For inflaGon, nf > 1027 ! Consider the QM of h as a pendulum whose length is controlled by the cosmic expansion ti, Li tf , Lf Quantum Mechanics of Space-Time
- 12. What Is Infla%on? A burst of expansion in which the early Universe grows exponenGally in Gme It puts the BANG in the BIG BANG InflaGon is the physics of a cosmic scalar field V δφ Quantum fluctuaGons: Explains the origin of large scale structure, as observed in the cosmic microwave background anisotropy paIerns and in the distribuGon of galaxies! h 2 ik = (H/2⇡) 2 Density spectrum: GW spectrum: φ hh2 i+,⇥,k = 2 (2/MP )2 h 2 ik h⇣2 ik = (H/ ˙)2 h 2 ik Review: Baumann 2012
- 13. What Is Infla%on? A burst of expansion in which the early Universe grows exponenGally in Gme It puts the BANG in the BIG BANG InflaGon is the physics of a cosmic scalar field V δφ Tilt: H slowly decays during inflaGon The PRIZE of cosmology: detect the long wavelength GWs, a unique feature of inflaGon φ RaGo: Amplitude of GW to density spectra V ' (r/0.01) ⇥ (1016 GeV)4 h⇣2 ik = 1 8⇡2✏ ✓ H 2⇡ ◆2 ! P⇣ / kns 1 r ⌘ hh2 i+⇥/h⇣2 i = 16✏
- 14. What Is Infla%on? A (Nearly) Scale Invariant Spectrum of Density PerturbaGons and GravitaGonal Waves “Let’s go to the board” cosmic %ny SIZE early late TIME H 1 Only inflaGon stretches density, GWs to lengths “outside” the Hubble radius (Nearly) Scale Invariant pick a radius: h i = 0 h 2 i = constant
- 17. What Is Infla%on? A burst of expansion in which the early Universe grows exponenGally in Gme It puts the BANG in the BIG BANG Slow roll for a scalar field: V = 1 2 m2 2 if then m MP ✏ = 1 2 M2 P (V 0 /V )2 ⌧ 1 Detectable GW spectrum implies large field excursion MP = O(1) p r/0.01
- 18. Novel GravitaGonal Behavior L = 1 2 M2 P R 1 4 ~Fµ⌫ · ~Fµ⌫ ~Fµ⌫ = @µ ~A⌫ @⌫ ~Aµ g ~Aµ ⇥ ~A⌫ SU(2) Aa i = (⌧) a i flavor space locked ~Aµ · ~e⌫ = a(⌧)yµ⌫ gµ⌫ = a2 (⌧)hµ⌫ Devulder, Maksimova, RC 2016, 2017 Bielefeld, RC 2015, 2016
- 20. Models of InflaGon Adshead & Wyman 2012; Maleknejad & Sheikh-Jabbari 2011; Dimastrogiovanni & Peloso 2013 Chromo-Natural InflaGon, Gauge-FlaGon L = 1 2 M2 P R 1 2 (@ )2 V ( ) 1 4 Fa µ⌫Fµ⌫ a + M Fa µ⌫ eFµ⌫ a L = 1 2 M2 P R 1 4 Fa µ⌫Fµ⌫ a + (Fa µ⌫ eFµ⌫ a )2 V = µ4 (1 cos /f) ! 1 2 m2 2
- 21. Models of InflaGon ns = 0.9667 ± 0.0040 (1 ) r < 0.07 (95% C.L.) Planck 2016 BKP 2016 CMB-S3
- 22. New: Toy Model of InflaGon Devulder & RC 2017 L = 1 2 M2 P R 1 2 (@ )2 V ( ) 1 4 Fa µ⌫Fµ⌫ a + M Fa µ⌫ eFµ⌫ a V = 1 n m4 ( /m)n
- 28. Leptogenesis NR NL = 1 24(16⇡2) R d4 x p gR eR Eguchi, Gilkey, Hanson (1980) leptons created, with asymmetry
- 29. Leptogenesis Sakharov CondiGons • ViolaGon of baryon number • CP violaGon • Out of equilibrium … saGsfied • Lepton number violated • Inflaton/gauge field are parity-odd • InflaGon is far out of equilibrium
- 30. Leptogenesis ⌘ ⌘ nB n ' 1 7 ⇥ 28 79 ⇥ hn`i s ⌘ ' 6.1(±0.04) ⇥ 10 10 Planck 2016 Convert to baryon asymmetry by SM electroweak processes CMB-S3 (3σ) An observable within reach!