COSMOLOGY 566: Cosmological and Astrophysical Constraints on Fundamental Physics in 4 dimensions

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COSMOLOGY 566 Cosmological and Astrophysical
Constraints on Fundamental Physics(in 4
dimensions)

• Lawrence M. Krauss
• CWRU
• Jan 14- April 21 2004

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Tentative Observables to be dicussed (8 sessions)

• Astrophysics Constraints, FRW Expansion and Age
  of the Universe
• Density of the Universe Dark Matter Dark
  Energy
• Nucleosynthesis Constraints
• Stellar Evolution
• Baryogenesis and Inflation
• Large Scale Structure and CMB
• Gravitational Waves
• ????

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TERM PLAN

• No make up classes
• Term assignments will be handed out Feb 4
  Students will work in groups 2 and prepare a
  paper and lecture on astrophysical implications
  of a particle scenario. I will choose as many
  different scenarios as there are groups.. Each
  one will have different astrophysical
  implications.
• CLASS SCHEDULE AND SYLLABUS.. See sheet
• April 14 -21, student presentations

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Tentative Syllabus
Jan 14 CLASS 0 Overview of the Course, and
general intro Jan 21 CLASS 1 The STANDARD
MODEL GEOMETRY AND EXPANSION Jan 28 NO
CLASS Feb. 4 CLASS 2 AGE CONSTRAINTS AND
DENSITY OF THE UNIVERSE Feb 11 CLASS 3 EQ. OF
STATE, MATTER DENSITY, DARK MATTER Feb. 18 (NOTE
CLASS 4 will meet 2-4 pm this day!) DARK MATTER
AND PARTICLE PHYSICS Feb. 25 CLASS 5 DARK
MATTER AND PARTICLE PHYSICS CONTINUED March 3 NO
CLASS March 10 SPRING BREAK NO CLASS March 17
CLASS 6 BIG BANG NUCLEOSYNTHESIS March 24 CLASS
7 STELLAR STRUCTURE AND CONSTRAINTS ON
FUNDAMENTAL PARAMETERS March 31 NO CLASS April
7 CLASS 8 ?????? April 14 PRESENTATIONS April
21 PRESENTATIONS
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1 Why Cosmology?
The Universe as (a) Accelerator (b)
target (c) laboratory
The Discovery Potential of Astrophysics is
immense, as new windows on the Universe are
opening up.
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(No Transcript)
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1 Why Cosmology?
The Observables

• Expansion Rate
• Distance (luminosity, size, age)-redshift
  relation
• Mass Density
• Stellar Luminosities and Distribution
• Large Scale Structure
• Light Element Abundance
• Baryon to Photon Ratio
• Cosmic Microwave Background
• X Ray, Gamma Ray and Gravitational Wave
  Backgrounds
• Dark Matter Density and Distribution
• Dark Energy Density and Distribution
• Neutrino Background

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1 Why Cosmology?
QCD, SUSY?
106 103 100 10-3
LHC
Ecm (GeV)
t
Fermilab
W,Z
CERN
QCD
SLAC, BNL
1975 1985 1995 2005 2015
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1 Why Cosmology?
COSMIC RAYS
BARYONS?
SN
QCD, SUSY?
106 103 100 10-3
DARK MATTER?
LHC
Ecm (GeV)
EW PT
t
BBN
Fermilab
W,Z
CERN
QCD
QCD PT
SLAC, BNL
1975 1985 1995 2005 2015
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1 Why Cosmology?
Luminosity (erg/sec)
eg. CERN 1999 lt I gtbeam 4mA 1016 e/sec
lt E gtbeam 100 GeV 10-1 erg -gt L 1015 erg/sec
108 W
Compare to Earth 1013 W 1020
erg/sec Sun 1033 erg/sec AGN-Quasar
1045 erg/sec Supernova 1053 erg/sec
Astrophysics Rules!!!
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1 Why Cosmology?
Astrophysics
CROSS SECTION
10-42 10-40 10-38 10-36 10-34
? (cm2)
Accelerators
1 10 102 103 104 105 106
(cm)
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1 Why Cosmology?
Target Volumes (MASS)
108 USD 105 Tons
1022
1 SUN 1027 Tons
Interaction Regions LHC/BNL (1 fm)3 at T
100 MeV
1057
Supernova (1019 fm)3 at T 100 MeV
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1 Why Cosmology?
Caveats

• An Observation is NOT an experiment!
• Systematics are EVERYTHING!
• Beware of Over-interpreting the data

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2 The standard model
The Standard Model of cosmology in the 1980s,
developed by a remarkable interplay of ideas from
particle theory, along with particle experiments,
and observations from astrophysics
IS DEAD..
It has been replaced by something far more
bizarre..