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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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