Inflation : why and how ?. Gert Jan Hoeve, December 2012. Problems with the Hot Big Bang. Flatness | Ω -1|<10 16 at nucleosythesis Unwanted relics Horizon problem Homogeneity over parts of space that are presumably not causally correlated . Baryogenesis
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Gert Jan Hoeve, December 2012
d2a/dt2 >> 0
-(dH/dt)/H2 >> 1
Between Planck time (10-43) andGUT decoupling (10-35)
Alan Guth, 1981
Picture: one minute astronomer
Inflationends at t0 = 10-35 s, we are at t1 = 1017 s
In radiationdominateduniverse |Ω-1|proportional to time
|Ωnow-1| ≤ 10-2 |ΩGUT-1|≤ 10-54
Duringinflation H=constant, so|Ω-1|proportional to 1/a2
Total expansion > ~ 1027
Scalar field V(φ) causesspontaneoussymmetrybreaking
First or second order phasetransition?
B. Clauwens , R. Jeanerot, D-term inflationafterspontaneoussymmetrybreaking
Cosmologicalinflation is a viable hypothesis, but in desperate need of a more solid foundation (and experimental confirmation) from the realm of particle physics.