1. Making and Probing Inflation Lev Kofman KITPC Beijing November 6 2007 Making Inflation in String Theory How small can be r Gravity Waves from Preheating

2. Concise History of the Early Universe

3. Early Universe Inflation Scale factor time Realization of Inflation

4. Inflation in the context of ever changing fundamental theory 1980 2000 1990 -inflationOld Inflation New Inflation Chaotic inflation Double Inflation Extended inflation DBI inflation Super-natural Inflation Hybrid inflation SUGRA inflation SUSY F-term inflation SUSY D-term inflation SUSY P-term inflation Brane inflation K-flation Roulette Warped Brane inflation inflation Power-law inflation Tachyon inflation Racetrack inflation Assisted inflation

5. Family phase portrait of inflation

6. string theorist CY AdS 3+1 FRW Inflation in String Theory: Cosmology with Compactification

7. string theorist CY AdS 3+1 FRW Inflation in String Theory: Cosmology with Compactification 3+1 FRW CY cosmologist

8. Modular Inflation. Modular Inflation. They use Kahler moduli/axion like the fields that are a present in the KKLT stabilization. Brane inflation. Brane inflation. The inflaton field corresponds to the distance between branes in Calabi-Yau space. Historically, this was the first class of string inflation models. Modular Inflation. Modular Inflation. They use Kahler moduli/axion like the fields that are a present in the KKLT stabilization. Brane inflation. Brane inflation. The inflaton field corresponds to the distance between branes in Calabi-Yau space. Historically, this was the first class of string inflation models. String Theory inflation models

9. Inflation with branes in String Theory 4-dim picture Prototype of hybrid inflation

10. Inflation with branes in String Theory 4-dim picture Prototype of hybrid inflation throat warped geometry Mobile brane KKLMMT

11. m  2 = 2H Conformal coupling problem Due to conformal coupling effective inflaton mass Expected to prevent inflation

12. m  2 = 2H Conformal coupling problem Due to conformal coupling effective inflaton mass Expected to prevent inflation Rapid-roll Inflation with conformal coupling

13. Scalar field non-minimally coupling with gravity

14. Rapid-roll inflation with conformal field De Sitter solution

16. Efoldings warping

17. Efoldings and mass hierarchy Energy scale

18. Efoldings and mass hierarchy solution

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

22. String theory landscape of the Kahler moduli/axion Inflation

23. Ensemble of Inflationary trajectories

24. Lessons: Multiple fields Inflation Ensemble of acceleration histories (trajectories) for the same underlying theory Prior probabilities of trajectories P(H(t)) Small amplitude of gravity waves r from inflation

25. Generation of gravitational waves from inflation

26. time Hubble radius end of inflation recombination

27. inflation Hot FRW Initial conditions from Inflation

28. Baumann&Mcallister hep-th/0610285 Lyth hep-ph/9606387 Efstathiou &Mack astro-ph/0503360

29. .Spider Balloon 2009.9 Planck Satellite 2008.6 CMBPol 2017 Measurement of GW from CMB anisotropy polarization 0.1 0.01 < 0.34 Current limit 0.001 Ultimate limit

30. superheavy gravitino A discovery or non-discovery of tensor modes would be a crucial test for string theory and particle phenomenology unobservable for inflationary perturbations KKLT Kallosh, Linde hepth/0704.0647 Amplitude of GW and gravitino mass

32. Particlegenesis time Inflation no entropy no temperature BANG

33. Occupation number Classical Quantum Resonant Preheating in Chaotic Inflation

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

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

37. Classical Quantum Decay of inflaton and preheating after inflation movie

38. Classical Quantum Decay of inflaton and preheating after inflation

40. Evolutionof energy density Evolution of gravitational potential l A. Frolov 07

41. Tachyonic Preheating in Hybrid Inflation l movie

42. Tachyonic Preheating

44. Generation of gravitational waves from random media

45. time Hubble radius end of inflation recombination

46. Stochastic background of gravitational waves emitted from preheating after inflation

48. Emission of stochastic GW by random media

49. Emission of stochastic GW by random scalar fields First order phase transitions Second order phase transitions Topological defects formation Thermal bath of scalars Tachyonic preheating Resonant preheating

51. No GW emission

52. GW generated for non-trivial dispersion relation

53. Random gaussian fields

54. Emission of GW from preheating

55. Numerical calculations of GW emission from Preheating

60. Analytic check

61. estimation Shortcut to the answer Felder, LK hep-ph/0606256

62. topological effects after hybrid inflation (unstable) formation of defects results in GW emission

65. Application to particular hybrid model

66. GW from high energy inflation are targeted by CMB B-mode polarization experiments The story of stochastic gravitational waves is CMB anisotropies of 21 century GW from low-energy inflation are targeted by GW astronomy