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
Jan 13, 2016
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
Concise History of the Early Universe
Early Universe Inflation
Scale factor
time
Realization of Inflation
Inflation in the context of ever changing fundamental theory
1980
2000
1990
-inflation Old Inflation
New Inflation Chaotic inflation
Double InflationExtended 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-flationRoulette
Warped Brane inflation
inflation
Power-law inflation
Tachyon inflationRacetrack inflation
Assisted inflation
Family phase portrait of inflation
string theoristCY
AdS3+1 FRW
Inflation in String Theory: Cosmology with Compactification
string theoristCY
AdS3+1 FRW
Inflation in String Theory: Cosmology with Compactification
3+1 FRW
CYcosmologist
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
Inflation with branes in String Theory
4-dim picture
Prototype of hybrid inflation
Inflation with branes in String Theory
4-dim picture
Prototype of hybrid inflation
throat warped geometry
Mobile brane
KKLMMT
m2 = 2H
Conformal coupling problem
Due to conformal coupling effective inflaton mass
Expected to prevent inflation
m2 = 2H
Conformal coupling problem
Due to conformal coupling effective inflaton mass
Expected to prevent inflation
Rapid-roll Inflation with conformal coupling
Scalar field non-minimally coupling with gravity
Rapid-roll inflation with conformal field
De Sitter solution
Efoldings
warping
Efoldings and mass hierarchy
Energy scale
Efoldings and mass hierarchy
solution
Kahler moduli Inflation (Conlon&Quevedo hep-th/050912)Roulette Inflation-Kahler moduli/axion
(Bond, LK, Prokushkin&Vandrevange hep-th/0612197)
String theory landscape of the Kahler moduli/axion Inflation
Ensemble of Inflationary trajectories
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
Generation of gravitational waves from inflation
time
Hubble radius
end of inflation
recombination
inflationHot FRW
Initial conditions from Inflation
Baumann&Mcallister hep-th/0610285
Lyth hep-ph/9606387
Efstathiou &Mack astro-ph/0503360
.SpiderBalloon2009.9
PlanckSatellite2008.6
CMBPol 2017
Measurement of GW from CMB anisotropy polarization
0.1
0.01
< 0.34 Current limit
0.001 Ultimate limit
superheavy gravitino
A discovery or non-discovery of tensor modes A discovery or non-discovery of tensor modes would be a crucial test for string theory and particle would be a crucial test for string theory and particle
phenomenologyphenomenology
unobservable
for inflationary perturbations
KKLTKKLT
Kallosh, Linde hepth/0704.0647
Amplitude of GW and gravitino mass
Particlegenesis
time
Inflation
no entropyno temperature
BANG
Occupation number
Classical Quantum
Resonant Preheating in Chaotic Inflation
Resonant Preheating in Chaotic Inflation
preheatingexp excitation
Kolmogorovturbulence of bosons
thermalizationNon-linear
“bubbly” stage
Classical Quantum
Decay of inflatonand preheating after inflation
movie
Felder, LKhep-ph/0606256
Classical Quantum
Decay of inflatonand preheating after inflation
movie
Classical Quantum
Decay of inflatonand preheating after inflation
Evolutionof energy density
Evolution of gravitational potentiall
A. Frolov 07
Tachyonic Preheating in Hybrid Inflation
l
movie
Tachyonic Preheating
Generation of gravitational waves from random media
time
Hubble radius
end of inflation
recombination
Stochastic background of gravitational waves emitted from preheating after inflation
Emission of stochastic GW by random media
Emission of stochastic GW by random scalar fields
First order phase transitionsSecond order phase transitionsTopological defects formation
Thermal bath of scalarsTachyonic preheatingResonant preheating
No GW emission
GW generated for non-trivial dispersion relation
Random gaussian fields
Emission of GW from preheating
Numerical calculations of GW emission from Preheating
Numerical calculations of GW emission from Preheating
Analytic check
estimation
Shortcut to the answer Felder, LKhep-ph/0606256
topological effects after hybrid inflation (unstable)formation of defects results in GW emission
Application to particular hybrid model
GW from high energy inflation are targeted by CMB B-mode polarization experiments
The story of stochastic gravitational waves isCMB anisotropies of 21 century
GW from low-energy inflation are targeted by GW astronomy