University of California Los Angeles Department of Physics and Astronomy arisakaphysicsuclaedu 111412 Katsushi Arisaka 1 111412 Katsushi Arisaka 2 Seven Phases of Cosmic Evolution 14 billion years ago ID: 759495
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Slide1
Katsushi Arisaka
Origin of the Universe
University of California, Los Angeles
Department of Physics and Astronomy
arisaka@physics.ucla.edu
11/14/12
Katsushi Arisaka
1
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Seven Phases of Cosmic Evolution
14 billion years ago
Origin of
Particles
Origin of
Structure
Origin of Life
Origin of
Consciousness
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Expansion of Universe
Time
Size
Size of Universe
Time
Horizon
cT
Today
Beginning
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Temperature of Universe
Size
Temperature
Today
Beginning
Temperature = 1/Size
2.7
o
K
3,000
o
K
300,000
years
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Cosmology
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The Fate of the Cosmos
?
?
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Geometry of the Universe
Open
<1
Flat
=1
Closed
>1
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Cosmic Microwave Background(Discovered in 1964)
Sun/Earth
T=300,000 years
after the Big Bang
Temperature
=3,000
o
K
Transparent
Opaque
z=1,100
Today:
3000
o
K/1,100
=2.7
o
K
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Time = 300,000 years , Temp.= 3000 oK
All the electrons were bound by Hydrogen and Helium Nuclei. Atoms formed.The Universe became transparent. Photons were released. Radiation decoupled. Cosmic Microwave Background (CMB)
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Two Fundamental Problem of Big Bang Cosmology
Horizon Problem
At early Universe, Size >> Horizon.
Why is CMB so uniform in every direction?
Flatness Problem
-1 grows
proportional
to the size of the Universe.
Why is of today close to 1?
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Expansion of Universe
Time
Size
Horizon
cT
Today
Beginning
300k Years
Within 1
o
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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.
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Flatness Problem
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 1015.
| -1 | Size of Universe
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Inflation in Early Universe
Time
Size
Horizon
cT
Today
Beginning
Inflation
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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.
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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:
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WMAP
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WMAP Power Spectrum
Universe is Flat.
Inflation
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Geometry of the Universe
Open
<1 Flat =1Closed >1
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Supernova as a Standard Candle
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The Accelerating Universe （1998）
= 0.7
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Density of Our Universe
Matter
Total=+Matter =1.0Universe is Flat. Inflation73% is Dark Energy. Accelerating
M= 27%
Matter and are two of “Just Six Numbers”
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Density Fluctuations
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Cosmic Pyramid
Dark
Matter
Dark Energy
Gas,
Dust
Star
Metal
0.01%
0.5%
0.5%
5%
25%
70%
Baryonic Matter
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Dark Energy and Cosmology
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.
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Particle Physics
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Elementary Particles (~1970)
10
-10 m
10-14 m
10-15 m
< 10
-18
m
Slide30Quark Model
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u
u
d
Proton
u
d
d
Neutron
+ 2/3 + 2/3
– 1/3
= 1
+ 2/3
– 1/3
– 1/3
= 0
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Fermions
1973Elementary particles : “Fermions” Particle Anti-ParticleQuarks u u d s d sLeptons e µ e µ e- µ- e+ µ+
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SLAC
(Stanford Linear Accelerator Center)
e+ + e-
1 mile long
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Fermi Lab near Chicago
6km Circumference
1+1=2 TeV
Proton + Anti-proton
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Discovery of more quarks
1974 – 1994More quarks and leptons were discovered.1974 Ting (BNL) & Richter (SLAC) J/ = cc1975 Perl (SLAC) -lepton1978 Lederman (FNAL) = bb1994 CDF/D0 Group (FNAL) t (top quark)All discovered at US National Labs (Many Nobels!)
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Elementary Particles
Charge
+2/3-1/30-1
Fermion Boson
Charge0001
+ Anti-particles
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Elementary Particles
Charge
+2/3-1/30-1
Fermion Boson
Charge0001
Today
’s Universe
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Fermions: Ratio (in numbers)Lepton: e ~1 e- ~410-10Baryon: p ~410-10 n ~110-10Bosons:Photon: 1No anti-particles# Photon : # Baryon = 1 : ~410-10# p = # e-
Now
Time = 14B yrs, Temp.= 2.7
o
K (3
10
-4
eV)
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Expansion of Universe
Time
Size
Size of Universe
Time
Horizon
cT
Today
Beginning
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Temperature of Universe
Size
Temperature
Today
Beginning
Temperature = 1/Size
2.7
o
K
3,000
o
K
300,000
years
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Relation between Temperature and Time
T: Temperature t : time
Time (sec)
Temperature
130 GeV
130 MeV
1.3 MeV
130 keV
10
-10
10
-4
1
100
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Thermal Equilibrium
If thermal energy is greater than twice the mass of particles, E > 2 mc2 Photon Particle + Anti-particle Example: me = 0.511 MeV if E > 1.022 MeV e- + e+
e
-
e+
e-
e+
e-
e+
e-
e+
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Fermions: RatioLepton: e 1 e- 1 e 1 e+ 1Baryon: p ~410-10 n ~110-10Bosons:Photon: 1
Time = 1 sec, Temp.= 10
10
o
K (1.3 MeV)
e
-
n
e+
e
p
e+
e-
e
e
e
Horizon
~ 3x10
8
m
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Time = 10-4 sec, Temp.= 1012 oK (~100 MeV)
Thermal Equilibrium of Protons and Neutronsn p + e- + en + e+ p + en + e p + e-Lepton Dominant Era Fermions: RatioLepton: e 1 e- 1 e 1 e+ 1Baryon: p ~210-10 n ~210-10Bosons:Photon: 1
e
-
n
e
+
e
p
e
+
e-
e
e
e
Horizon
~ 30 km
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Time = 10-5 sec, Temp.= 31012 oK (300 MeV)
Quark Hadron Phase Transitionu-quarks and d-quarks are bound together to form protons and neutrons.No anti-quarks
u
d
u
u
u
u
u
d
d
d
d
d
u
d
d
u
d
d
u
u
d
u
u
d
p
n
p
n
Quark-gluon Plasma
Horizon
~ 3 km
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Time = 10-6 sec, Temp.= 1013 oK (~1 GeV)
Thermal Equilibrium of Photons, Leptons and Quarks Photon Lepton + Anti-lepton e- + e+ µ- + µ+ + Photon Quark+ Anti-quark u + u d + d s + s#photon ~ #lepton ~ #quark
µ
-
d
µ+
e
u
e+
e-
µ
e
µ
s
u
s
d
Horizon
~ 300 m
Slide46Mass of Particles
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Elementary Particles
Charge
+2/3-1/30-1
Fermion Boson
Charge0001
+ Anti-particles
Universe at t = 1 µsec
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Unification of Forces
10
32
??
1029
Electro-Weak Unification
100 GeV
10
16 GeV
10
19
GeV
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Time = 10-10 sec, Temp.= 1015 oK (~100 GeV)
Electro-weak Unification Electro-Magnetic force = Weak forceThe highest energy we can study by the accelerators
Z
o
µ-
d
µ+
e
u
e+
e-
W+
µ
e
µ
W+
s
u
s
d
Horizon
~ 3 cm
-
+
c
b
b
c
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Elementary Particles
Charge
+2/3-1/30-1
Fermion Boson
Charge0001
+ Anti-particles
Universe at = 0.1 nsec
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Unification of Forces
1032
1029
Grand Unification
100 GeV
10
16
GeV
10
19
GeV
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Time = 10-34 sec, Temp.= 1029 oK (~1016 GeV)
Grand Unification Strong-Force = Electro-Magnetic force = Weak forceQuark = LeptonsEverything (except gravity) is unified.Inflation might happen?
Horizon
~ 310
-24 cm
Size ~ 30 cm
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Inflation in Early Universe
Time
Size
Horizon
cT
Today
Beginning
Inflation
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Unification of Forces
10
32
Plank Epoch
1029
100 GeV
1016 GeV
10
19
GeV
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Time = 10-44 sec, Temp.= 1032 oK (~1019 GeV)
Planck Epoch Gravitational Effect (Curvature of the space)Quantum Mechanical effectWe can not define space-time any more at earlier stage. < Plank Scale>
Size
~10
-33 cm
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Hubble Deep Field
Physicists’ View of Early Universe
Fiat lux
Let there be light
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Hubble Deep Field
Physicists’ View of Early Universe
Lorentz Invariance
Local Gauge Invariance
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Structure of DNA
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Symmetry Breaking
Symmetry
Break Down
Simple
Complex
Time
2
3
4
5
6
7
8
9
10
11
12
13
14
1B years
0
Z
o
µ
-
d
µ
+
e
u
e
+
e
-
W
+
µ
e
µ
W
+
s
u
s
d
-
+
c
b
b
c
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The Beginning
Everything was the same Perfect symmetry.All the particles are the same as photons.All four forces are the same.The Universe was 10 dimension. 3 Space Flattened 1 Time 3 Strong Force 6 2 Weak Compacitified 1 Electro-Magnetic
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Early Universe & Unsolved Problems
10
-45
sec
10
-40
10
-35
10
-30
10
-25
10
-20
10
-15
10
-10
10
-5
10
5
sec
1
1
year
10
3
10
6
10
9
year
Time (sec)
Temp.
(oK)
10
18
10
15
10
12
10
9
1
PeV
1
TeV
1
GeV
1
MeV
1
KeV
1
eV
10
30
10
25
10
20
10
15
10
10
10
5
1
Energy (G
eV
)
10
-3
eV
Planck
EW
Now
GUT
Grand Unification
Plank Epoch
Electro-Weak Unification
Inflation
Dark Matter
Dark Energy
The Beginning
Matter-Radiation Decoupling