hartmut abele 1 wmap of cosmic 3k microwaveradiation staus: 300000 years after bb kosmologie ii
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Hartmut Abele 1
WMAP of cosmic 3K microwaveradiation
Staus: 300000 years after BB
Kosmologie II
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Phase Transitions of the Universe and observables from neutron experiments The neutron as an object: ~ as a tool: New Physics: Standard Model:
Temperature 10+19 GeV Planck
GUTs - - Inflation Electroweak Chiral transition Nucleon freeze out Nuclear freeze out Atomic freeze out Galactic freeze out
10-11 GeV 10-43s 10-35s 10-12s 1 s 105y 109y today
Time
EDMMdn
qn
n nbar
mWR,
Vud
gA / gV
n
-1
N
aW
M
A ,P
, , , , ,
pp
Dubbers: ESS presentation 2002
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blau:2.721 K
rot: 2.729 K
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Nature, 17.6.05Nature, 17.6.05
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GUTMPL
MnPL
quantum gravity
= 1/137
100 GeV, LEP-energy at CERN
= 1/128
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The Neutron Lifetime and Big Bang Nucleo SynthesisThe 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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