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The Universe
• Characteristics– Expanding (Hubble’s Law)– Finite age – Cool now, hotter long ago– Composition
• 70% H, 28% He, 2% the rest – Why?
– Most matter is dark (unseen)– Most content is dark energy > gravity
• Accelerates the Universe’s expansion
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Universe Content
• Matter – Composed of elementary particles– QED – quantum electrodynamic theory– Quarks, leptons, lions, tigers, and bears, oh my!– These particles interact via force carriers
• 3 out of 4 forces covered – gravity not
• How did this stuff form?• How does it behave under extreme conditions?
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Quarks u – up
+2/3
c – charm
Mass > s
t – top
Heaviest
– photon E-M
d – down
-1/3
s – strange
Mass > d,u
b – bottom
Mass>c
g – gluon Strong Nuclear
Leptons
e – electron neutrino
– mu neutrino
– tau neutrino
Z – z boson Weak Nuclear
e – electron
-1
– muon
Mass>e
– tau
Mass>W – w boson
Proton = uudNeutron = udd
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Universe’s Energy
Total Energy = Energy of motion + Energy of gravity
Combined with other laws to get the Friedmann Equation -
H = Hubble’s “constant” H, , R are
= density of the Universe time dependent
k = curvature measure
R = scale of the Universe
22
3
8
R
kGH
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k > 0
• Positive curvature, hyperbolic shape• Kinetic Energy rules• Open Universe• Eventually….
– 1012 – 1014 years - Star formation ends– 1020 years – Galaxy mergers end– 1030 years – Galaxy death (massive black hole)
• 1030 – 1035 years – proton decay• 10100 years – black hole evaporation
– Eventually “heat death”
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k < 0
• Negative curvature, spherical shape• Gravity rules• Closed Universe• Eventually…
– Galaxy redshifts become blueshifts– Universe’s temperature increases– Cluster collisions– Black hole growth, matter evaporation– Total collapse
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k = 0
• No curvature, Flat
• Perfect balance between gravity, energy
• Marginally Open
• Eventually– Like the k>0 case, but slower
Which is it?
Define critical densityG
H
G
H ocritical
8
3
8
3 22
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Other options?
Einstein’s Idea– Static Universe– No motion requires anti-
gravity effect – Change the formulae
The Field Equations = Cosmological Constant
An “anti-gravity” term
That can’t really exist, can it?
33
4
33
8
2
2
2222
RGR
dt
Rd
Rk
GR
dt
dRv
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1997
West Coast – Supernova Cosmology Project
East Coast – High-z Supernova Team
Type I SN – best for great distances– Testing expansion rate of the Universe– How much is gravity slowing the expansion?– How fast was the expansion in the past?– Current expansion rate? (Hubble constant)
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Low redshifts
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Where is the SN?
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Higher redshifts
Best result is caseWhere 0!
Also find k=0
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> 0 Universe
> 0 Accelerating Universek =0 implies a Flat UniverseDensity of the Universe = Critical Density?• What is the “density”
– Matter• Dark and regular
– Energy (remember E=mc2)• Energy of light, radiation• Energy of motion - gravity• Energy of motion – anti-gravity!
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• Continual acceleration?– No, varies with z (distance)– Initial deceleration for z>1– Acceleration took over later, z<1
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Confusing terms
• k=curvature (0 = Flat, <0 Closed, >0 Open)• Define Flat, <1 Open, >1 Closed)• =cosmological constant
– Also written as
• M = matter density (regular and dark)– Also written as M
General rule - = + M
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Universal Light - CMBR
• Cosmic Microwave Background Radiation – Everywhere– Black body temperature = 2.725 K– First detected in 1963 by Penzias, Wilson
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WMAP Results
Launched 2001
First results – 2003– Flat (k=0, =1)– Age = 13.7 billion years– Hubble Constant = 72 km/s/Mpc– Most of the Universe = Dark Energy
– M =.27
– =.73
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Same results - Supernova projectsCMBR projectsGalaxy Cluster projects
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Options for the Universe?
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Big Rip
should increase with expansion
Lead to a tearing apart of all matter?
When?~22 Billion years from now
• Galaxy cluster dissolve (1 Gyr before end)• Galaxies dissolve (60 Myr before end)• Solar systems dissolve (3 months before end)• Planets dissolve (1/2 hour before end)• Atoms dissolve (10-19 seconds before end)