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Preheating after Inflation

Preheating after Inflation. Preheating with QFT Cosmological fluctuatons from Preheating Reheating with String Theory. Lev Kofman KITPC November 14, 2007. Early Universe Inflation. Scale factor. time. Realization of Inflation. Particlegenesis. time.

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Preheating after Inflation

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  1. Preheating after Inflation Preheating with QFT Cosmological fluctuatons from Preheating Reheating with String Theory Lev Kofman KITPC November 14, 2007

  2. Early UniverseInflation Scale factor time Realization of Inflation

  3. Particlegenesis time Inflation no entropy no temperature BANG

  4. Output of Preheating

  5. Schwinger formula for particle creation classical Scalar ED Quantum

  6. Resonant Preheating in Chaotic Inflation Classical Quantum Occupation number

  7. Method od successive scatterings

  8. Resonant Preheating in Chaotic Inflation

  9. Decay of inflaton and preheating after inflation Classical Quantum movie Felder, LK, 06

  10. Decay of inflaton and preheating after inflation Classical Quantum Felder, LK hep-ph/0606256 movie

  11. Decay of inflaton and preheating after inflation Classical Quantum

  12. Kolmogorov turbulence of bosons preheating exp excitation Non-linear “bubbly” stage thermalization

  13. A. Frolov 07 Evolutionof energy density Evolution of gravitational potentiall

  14. Three-linear interaction In expanding universe complete inflaton decay requires 3-legs interactions Broad Parametric Resonance Tachyonic Resonance

  15. Above the barrier Below the barrier

  16. Three- vs four-legs Four-legs dominates at preheating SUSY Three-legs dominates after preheating

  17. Preheating of fermions

  18. Tachyonic Preheating in Hybrid Inflation l movie

  19. Tachyonic Preheating

  20. Hubble radius end of inflation recombination time

  21. Initial conditions from Inflation inflation Hot FRW

  22. Light field at inflation

  23. ModulatedFluctuations Inflationradiation Light field at inflation develops fluctuations

  24. Modulated fluctuations in Hybrid Inflation inhomogeneouswaterfall Bernardeau, LK, Uzan 03

  25. modulated fluctuations scalar field associated with angular position at throat warped geometry Mobile brane

  26. Kahler moduli Inflation (Conlon&Quevedo hep-th/050912) Roulette Inflation-Kahler moduli/axion (Bond, LK, Prokushkin&Vandrevange hep-th/0612197)

  27. Reheating after String Theory Inflation Barnaby, Burgess, Cline, hep-th/0412095 LK, Yi, hep-th/0507257 Frey, Mazumdar, Myers, hep-th/0508139 Chialva, Shiu, Underwood, hep-th/0508229 Chen, Tye, hep-th/05120000; 0602136 Dufaux, LK, Peloso 07

  28. Realization of String Theory Hybrid Inflation Warped brane inflation throat warped geometry Mobile brane 4-dim picture Prototype of hybrid inflation

  29. LK, Yi 05 End point of inflation Closed strings Unstable KK modes BANG SM particles Long-living KK modes related to inner isometries Open strings between branes are unstable

  30. KK story KK particles are thermalized first SM particles are thermalized much later KK from M with isometries are stable No complete decay KK particles freeze out

  31. Fluctuations in Cosmology with Compactification string theorist CY cosmologist CY 3+1 FRW AdS 3+1 FRW Practical cosmologist CY +fluctuations KK atom 3+1FRW +KK gas

  32. metric wave equation for KK mode Throat geometry “big” CY

  33. KK modes interactions kk kk kk H kk H

  34. KK KK SM KK KK

  35. resolution? Attachment of KS throat to a compact CY Induces symmetry breaking perturbations. Tip of KS throat is a particular case of Sasaki-Einstein manifolds. There are asymmetric SE manifolds, but no examples of asymmetric throats

  36. Impact of isometry breaking perturbation on KK modes decay Dufaux, LK, Peloso 07

  37. Decay of KK modes into SM particles

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