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Surveying Inflation and Reheating
Cosmological Landscape: Strings, Gravity and Inflation Seoul, September 2005
“K. listened intently. So the Castle had appointed him land surveyor …”
“The Castle” by F.Kafka
Lev Kofman, CITA
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Bottom-up approach to inflation:reconstruction of acceleration trajectories
Top-down approach to inflation:seeks to embed it in fundamental theory
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Early Universe Inflation
Scale factor
time
Realization of Inflation
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Phase portrait of inflation
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Particlegenesis
time
Inflation
no entropyno temperature
BANG
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Occupation number
Classical Quantum
Resonant Preheating in Chaotic Inflation
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Resonant Preheating in Chaotic Inflation
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Classical Quantum
Decay of inflatonand preheating after inflation
movieFelder, LK,05
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Classical Quantum
Decay of inflatonand preheating after inflation
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Tachyonic Preheating in Hybrid Inflation
l
movie
Felder, LK, Linde,01
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Tachyonic Preheating
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inflationHot FRW
Initial conditions from Inflation
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Modulated Fluctuations
Hà1
x~
î ÿ(x~)
î ÿ =Rd3k(akÿk(t)eik
~x~+h:c:)
t
Light field at inflation
Inflation radiation
LK03;Dvali et al,03
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Modulated fluctuations in Chaotic Inflation
Podolsky, Felder, LK,Pelosohep-ph/0507096
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Modulated fluctuations in Hybrid Inflation
inhomogeneous waterfall
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Bernardeau, Uzan, LK 03
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4 dimensional Inflation predicts
No classical inhomogeneities from the past
Scale free gaussian fluctuations of all light scalars
No vector perturbations
Scalar (almost scale free gaussian) metric perturbations
Tensor (scale free gaussian) metric perturbations
Creation of all SM particles in preheating/thermalization
Òtot =1
Cö÷úû = 0
î ÿk(t)eik~x~
Aö =0
Ð ! Ðk(t)eik~x~
hik ! hk(t)eik~x~eij
Treh
One inflation helps to ignite another inflation
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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-flationN-flation
Warped Brane inflation
inflation
Power-law inflation
Tachyon inflationRacetrack inflation
Assisted inflation
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Search for inflaton with branes in extra dimensions
4-dim picture
Dvali,Tye 98
Prototype of hybrid inflation
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Compactification of inner dimensions with branes
Old string theory
New phenomenology
Strongly warped 5d geometry
ds2 = A2(y)(à dt2+dx~2) +gabdyadyb
RS 99
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Stabilization of Inner dimensionsand moduli in string theory
dS4 â M
ds2 = A2(y)(à dt2+e2Htdx~2) +gabdyadyb
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Realization of String Theory Chaotic Inflation
Mobile brane
Chaotic inflation
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Realization of String Theory Inflation
on the ground of KKLT throat warped geometry
Mobile brane
modulated fluctuations
Conformal coupling problem
scalar field associated with angular position at
KKLMMT03
Warped brane inflation
Realization of warped brane inflation with conformal inflaton
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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
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Open strings
between branes are unstable
End point of inflation
BANG
SM particles
Closed strings
Unstable KK modes
Long-living KK modesrelated to inner isometries
LK, Yi 05
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KK story
KK particles are thermalized firstSM particles are thermalized much later
KK from M with isometriesare stable
No complete decya
KK particles freeze out
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KK
KK
KK
KK
SM
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4 dim Inflation in 10dim String Theory predicts
All what 4 dim inflation predicts
Scale free gaussian fluctuations of many light scalars
Creation of non-SM particles (KK modes) in reheating/thermalization
î ÿk(t)eik~x~
TK K
Short-wavelength gravitational radiation
Modulated cosmological fluctuations
String theory Cosmic strings
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string theoristCY
AdS3+1 FRW
Fluctuations in Cosmology with Compactification
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string theoristCY
AdS3+1 FRW
3+1 FRW
Fluctuations in Cosmology with Compactification
CYcosmologist
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string theorist
Practical cosmologist
CY
AdS
CY +fluctuations
3+1 FRW
3+1 FRW
3+1 FRW +fluctuations
Fluctuations in Cosmology with Compactification
CYcosmologist
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background
fluctuations
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Fluctuations in Cosmology with Compactification
ds2=A2(y)[(à dt2+e2Htdx~2) +gabdyadyb]
dS4 â M
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Gravitational instability of anysotropocgeometry
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Too strong fluxes lead to new instability
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Summary
Theory of cosmological fluctuations in models withextra dimensions
Generic properties of fluctuations in 3+1+d dim
Instabilities exclude regions of landscape
Potential observables: varying couplings/masses,Primordial fluctuations
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Scanning Inflation R.Bond, C.Contaldi,A.Frolov, L.KofmanT.SouradeepP.Vandrevange
Bottom-up
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Ensemble of Inflationary trajectories
Chebyshev decomposition
Space of models opens wide
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H(N) P(k)
ns;nt; r;dn=dlnk;As; :::
ï ;ñ:::
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Observational constraints on trajectories
Markov Chain Monte Carlo
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Degeneracy of the Potential Reconstruction
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“Best fit” model is awkward:
features in the potential
suppression of scalar mode at large scales
large tensor mode
Bottom-up:personal priors
Top-down approach:no priors
Non-vanishing probability
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Reconstruction of Inflationary Trajectory
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