Katsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy

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1 11/14/12 Katsushi Arisaka 1 Katsushi Arisaka University of California, Los Angeles Department of Physics and Astronomy arisaka@physics.ucla.edu

2 Seven Phases of Cosmic Evolution 11/14/12 Katsushi Arisaka 2 14 billion years ago Origin of Particles Origin of Structure Origin of Life Origin of Consciousness

3 11/14/12 Katsushi Arisaka 3 Expansion of Universe Size Size of Universe Time Horizon ct Beginning Today Time

4 11/14/12 Katsushi Arisaka 4 Temperature of Universe Temperature Temperature = 1/Size 3,000 o K 2.7 o K Beginning 300,000 years Today Size

5 Cosmology 11/14/12 Katsushi Arisaka, UCLA 5

6 The Fate of the Cosmos 6/24/2011 Katsushi Arisaka 6??

7 6/24/2011 Katsushi Arisaka 7 Geometry of the Universe Open Ω<1 Flat Ω=1 Closed Ω>1

8 6/24/2011 Katsushi Arisaka 8

9 6/24/2011 Katsushi Arisaka 9

10 Cosmic Microwave Background (Discovered in 1964) 6/24/2011 Katsushi Arisaka 10 T=300,000 years after the Big Bang Temperature =3,000 o K Sun/Earth z=1,100 Today: 3000 o K/1,100 =2.7 o K Transparent Opaque

11 Time = 300,000 years, Temp.= 3000 o K 3/8/2007 Katsushi Arisaka 11 Ø All the electrons were bound by Hydrogen and Helium Nuclei. Atoms formed. Ø The Universe became transparent. Photons were released. Radiation decoupled. Cosmic Microwave Background (CMB)

12 Two Fundamental Problem of Big Bang Cosmology 2/27/2007 Katsushi Arisaka 12 Ø Horizon Problem At early Universe, Size >> Horizon. Why is CMB so uniform in every direction? Ø Flatness Problem Ω-1 grows proportional to the size of the Universe. Why is Ω of today close to 1?

13 2/27/2007 Katsushi Arisaka 13 Expansion of Universe Size Horizon ct Within 1 o Beginning 300k Years Today Time

14 2/27/2007 Katsushi Arisaka 14 Horizon Problem The horizon problem: When observed in diametrically opposite directions from Earth, cosmic background radiation appears the same even though there hasn t been enough time since the Big Bang for them to be in thermal contact.

15 2/27/2007 Katsushi Arisaka 15 Flatness Problem Ω-1 Size of Universe The flatness problem: In order for the universe to have survived this long, its density in the early stages must have differed from the critical density by no more than 1 part in

16 2/27/2007 Katsushi Arisaka 16 Inflation in Early Universe Size Inflation Horizon ct Beginning Today Time

17 2/27/2007 Katsushi Arisaka 17 The Inflationary Universe Inflation, if correct, would solve both the horizon and the flatness problems. This diagram shows how the horizon problem is solved the points diametrically opposite from Earth were in fact in contact at one time.

18 2/27/2007 Katsushi Arisaka 18 The Inflationary Universe The flatness problem is solved as well after the inflation the need to be exceedingly close to the critical density is much more easily met:

19 WMAP 6/24/2011 Katsushi Arisaka 19

20 6/24/2011 Katsushi Arisaka 20 WMAP Power Spectrum Universe is Flat. Inflation

21 6/24/2011 Katsushi Arisaka 21 Geometry of the Universe Open Ω<1 Flat Ω=1 Closed Ω>1

22 Supernova as a Standard Candle 6/24/2011 Katsushi Arisaka 22

23 The Accelerating Universe (1998) 2/27/2007 Katsushi Arisaka 23 Ω Λ = 0.7

24 Density of Our Universe Ø Ω Total =Ω Λ +Ω Matter =1.0 Ω Λ Ø Universe is Flat. Inflation Ω M = 27% Ø 73% is Dark Energy. Accelerating Ω Matter and Ω Λ are two of Just Six Numbers Ω Matter 11/14/12 Katsushi Arisaka 24

25 Density Fluctuations 6/24/2011 Katsushi Arisaka 25

26 6/24/2011 Katsushi Arisaka 26 Cosmic Pyramid Baryonic Matter Metal 0.01% Star 0.5% Gas, Dust 5% Dark Matter 25% Dark Energy 70%

27 Dark Energy and Cosmology 11/14/12 Katsushi Arisaka 27 This graph now includes the accelerating universe. Given what we now know, the age of the universe works out to be 13.7 billion years.

28 Particle Physics 11/14/12 Katsushi Arisaka, UCLA 28

29 Elementary Particles (~1970) m m m < m 6/23/2011 Katsushi Arisaka 29

30 11/14/12 Katsushi Arisaka 30 Quark Model Proton Neutron u u u d d d + 2/3 + 2/3 1/3 = 1 + 2/3 1/3 1/3 = 0

31 6/23/2011 Katsushi Arisaka 31 Fermions Ø 1973 Elementary particles : Fermions Particle Anti-Particle Quarks u u d s d s Leptons ν e ν µ ν e ν µ e - µ - e + µ +

32 SLAC (Stanford Linear Accelerator Center) 1 mile long e + + e - 6/23/2011 Katsushi Arisaka 32

33 Fermi Lab near Chicago 6km Circumference 1+1=2 TeV Proton + Anti-proton 6/23/2011 Katsushi Arisaka 33

34 6/23/2011 Katsushi Arisaka 34 Discovery of more quarks Ø More quarks and leptons were discovered Ting (BNL) & Richter (SLAC) J/Ψ = cc 1975 Perl (SLAC) τ-lepton 1978 Lederman (FNAL) ϒ = bb 1994 CDF/D0 Group (FNAL) t (top quark) All discovered at US National Labs (Many Nobels!)

35 6/23/2011 Katsushi Arisaka 35 Elementary Particles Charge +2/3-1/3 0-1 Fermion Boson Charge ±1 + Anti-particles

36 3/6/2007 Katsushi Arisaka 36 Elementary Particles Today s Universe Charge +2/3-1/3 0-1 Fermion Boson Charge ±1

37 Now Time = 14B yrs, Temp.= 2.7 o K ( ev) 6/23/2011 Katsushi Arisaka 37 Ø Fermions: Ratio (in numbers) Lepton: ν e e - ~1 ~ Baryon: p ~ n ~ Ø Bosons: Photon: γ 1 No anti-particles # Photon : # Baryon = 1 : ~ # p = # e -

38 11/14/12 Katsushi Arisaka 38 Expansion of Universe Size Size of Universe Time Horizon ct Beginning Today Time

39 11/14/12 Katsushi Arisaka 39 Temperature of Universe Temperature Temperature = 1/Size 3,000 o K 2.7 o K Beginning 300,000 years Today Size

40 Relation between Temperature and Time 6/23/2011 Katsushi Arisaka 40 Temperature 130 GeV 130 MeV 1.3 MeV 130 kev T: Temperature t : time T = t(sec) = t(sec) o K MeV Time (sec)

41 6/23/2011 Katsushi Arisaka 41 Thermal Equilibrium If thermal energy is greater than twice the mass of particles, E > 2 mc2 Photon Particle + Anti-particle Example: m e = MeV if E > MeV γ e - + e + γ e - e+ e - γ e + e + γ γ e - e - e +

42 Time = 1 sec, Temp.= o K (1.3 MeV) 6/23/2011 Katsushi Arisaka 42 Ø Fermions: Ratio Lepton: ν e 1 e - 1 ν e 1 e + 1 Baryon: p ~ n ~ Ø Bosons: Photon: γ 1 ν e p e + ν e e - γ γ γ n ν e ν e - e e + γ Horizon ~ 3x10 8 m

43 6/23/2011 Katsushi Arisaka 43 Time = 10-4 sec, Temp.= o K (~100 MeV) Ø Thermal Equilibrium of Protons and Neutrons n p + e - + ν e n + e + p + ν e n + ν e p + e - Ø Lepton Dominant Era Ø Fermions: Ratio Lepton: ν e 1 e - 1 ν e 1 e + 1 Baryon: p ~ n ~ Ø Bosons: Photon: γ 1 ν e p e + ν e e - γ γ γ n ν e ν e - e e + γ Horizon ~ 30 km

44 Time = 10-5 sec, Temp.= o K (300 MeV) 6/23/2011 Katsushi Arisaka 44 Ø Quark Hadron Phase Transition u-quarks and d-quarks are bound together to form protons and neutrons. d d u u d d d u u u u d Quark-gluon Plasma n p u d d u u d p u d d u u d n No anti-quarks Horizon ~ 3 km

45 Time = 10-6 sec, Temp.= o K (~1 GeV) 6/23/2011 Katsushi Arisaka 45 Ø Thermal Equilibrium of Photons, Leptons and Quarks Photon Lepton + Anti-lepton γ e - + e + γ µ - + µ + γ ν + ν Photon Quark+ Anti-quark γ u + u γ d + d γ s + s s µ - γ ν e γ d d e + u u ν µ γ γ ν e ν e - µ µ + s #photon ~ #lepton ~ #quark Horizon ~ 300 m

46 Mass of Particles 11/14/12 Katsushi Arisaka, UCLA 46

47 6/23/2011 Katsushi Arisaka 47 Elementary Particles Universe at t = 1 µsec Charge +2/3-1/3 0-1 Fermion Boson Charge ±1 + Anti-particles

48 6/23/2011 Katsushi Arisaka 48 Unification of Forces Electro-Weak Unification?? 100 GeV GeV GeV

49 Time = sec, Temp.= o K (~100 GeV) 6/23/2011 Katsushi Arisaka 49 Ø Electro-weak Unification Electro-Magnetic force = Weak force The highest energy we can study by the accelerators ν e s τ + d e + u u b ν µ b µ - W + d Z o W + γ c τ - ν e ν e - µ µ + c s Horizon ~ 3 cm

50 6/23/2011 Katsushi Arisaka 50 Elementary Particles Universe at = 0.1 nsec Fermion Boson Charge +2/3-1/3 0-1 Charge ±1 + Anti-particles

51 6/23/2011 Katsushi Arisaka 51 Unification of Forces Grand Unification 100 GeV GeV GeV

52 Time = sec, Temp.= o K (~10 16 GeV) 6/23/2011 Katsushi Arisaka 52 Ø Grand Unification Strong-Force = Electro-Magnetic force = Weak force Quark = Leptons Everything (except gravity) is unified. Inflation might happen? Size ~ 30 cm Horizon ~ cm

53 6/23/2011 Katsushi Arisaka 53 Inflation in Early Universe Size Inflation Horizon ct Beginning Today Time

54 6/23/2011 Katsushi Arisaka 54 Unification of Forces Plank Epoch 100 GeV GeV GeV

55 Time = sec, Temp.= o K (~10 19 GeV) 6/23/2011 Katsushi Arisaka 55 Ø Planck Epoch Gravitational Effect (Curvature of the space) Quantum Mechanical effect We can not define space-time any more at earlier stage. < Plank Scale> Size ~10-33 cm

56 11/14/12 Katsushi Arisaka 56 Hubble Deep Field Physicists View of Early Universe Fiat lux Let there be light

57 11/14/12 Katsushi Arisaka 57 Hubble Deep Field Physicists View of Early Universe Lorentz Invariance Local Gauge Invariance

58 Structure of DNA 11/14/12 Katsushi Arisaka, UCLA 58

59 11/14/12 Katsushi Arisaka,UCLA 59 Symmetry Breaking Time 0 1B years Simple Symmetry Break Down Complex s b µ - W + ν γ e τ Z d + c o d τ - u e+ ν u b µ W + c ν e - e ν µ + s

60 6/23/2011 Katsushi Arisaka 60

61 11/14/12 Katsushi Arisaka 61 The Beginning Ø Everything was the same Perfect symmetry. All the particles are the same as photons. All four forces are the same. Ø The Universe was 10 dimension. 3 Space Flattened 1 Time 3 Strong Force 6 2 Weak Compacitified 1 Electro-Magnetic

62 Early Universe & Unsolved Problems Time (sec) Temp. ( o K) sec Energy (GeV) Planck GUT Plank Epoch Grand Unification The Beginning Inflation sec 1 year year PeV 1TeV 1GeV 1MeV 1KeV 1eV 10-3 ev EW Now Electro-Weak Unification Matter-Radiation Decoupling Dark Matter Dark Energy 11/14/12 Katsushi Arisaka 62

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