Transcript Neutrons Neutron b-Decay Vud, and the question of unitarity

Kosmologie II
WMAP of cosmic 3K microwaveradiation
Staus: 300000 years after BB
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Phase Transitions of the Universe
and observables from neutron experiments
The neutron as an object:
New Physics:
Standard Model:
Temperature


10+19
GeV
~ as a tool:
n nbar
EDM
Mdn
mWR, 


qn
aW
V
ud
Planck
M

GUTs - gA /gV
N
 pp
Inflation

n
A,P
Electroweak
Chiral transition
Nucleon freeze out -1
,,
,
Nuclear freeze out ,,
Atomic freeze out
Galactic freeze out
10-11 GeV
10-43s
10-35s
Dubbers: ESS presentation 2002
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10-12s
1s
105y
Time
109y today
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rot: 2.729 K
blau:2.721 K
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Nature, 17.6.05
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100 GeV, LEP-energy at CERN
 = 1/128
 = 1/137
MnPL
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GUT
MPL
quantum gravity
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The Neutron Lifetime and Big Bang Nucleo Synthesis

Problem 1s after Big Bang:
– What does a gas of n and p, when
the universe expands and the
temperature drops?

Inputs:
– neutron lifetime 
– Cross sections
– neutrino cross-sections   1/
– nuclear physics 0.1 – 1 MeV
(measured!)

Outputs: H, D, He, Li
– number of particle families N
– density  of (ordinary) matter in
universe
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