inflation and branes
DESCRIPTION
Inflation and Branes. Top-down approach to inflation : seeks to embed it in fundamental theory. Bottom-up approach to inflation: reconstruction of acceleration trajectories. Lev Kofman, CITA Nearly Normal Galaxies August 8, 2005, Santa Cruz. Early Universe Inflation. - PowerPoint PPT PresentationTRANSCRIPT
Inflation and Branes
Bottom-up approach to inflation: reconstruction of acceleration trajectories
Top-down approach to inflation:seeks to embed it in fundamental theory
Lev Kofman, CITA
Nearly Normal Galaxies August 8, 2005, Santa Cruz
Early Universe Inflation
Scale factor
time
Realization of Inflation
Particlegenesis
time
Inflation
no entropyno temperature
BANG
Classical Quantum
Decay of inflatonand preheating after inflation
movieFelder, LK, Linde, 01,05
Classical Quantum
Decay of inflatonand preheating after inflation
inflationHot FRW
Initial conditions from Inflation
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
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
Search for inflaton with branes in extra dimensions
4-dim picture
Dvali,Tye 98
Compactification of inner dimensions with branes
Old string theory
New phenomenology
Strongly warped 5d geometry
ds2 = A2(y)(à dt2+dx~2) +gabdyadyb
Randal, Sundrum 99
New ideas about 4d gravity
New interactions with SM particles
New ideas about mass hierarchy
New ideas about cosmological constant
New ideas about Inflation
Stabilization of Inner dimensionsand moduli in string theory
dS4 â M
ds2 = A2(y)(à dt2+e2Htdx~2) +gabdyadyb
Realization of String Theory Inflation
on the ground of KKLT throat warped geometry
Hybrid inflationwith inflaton fluctuationsMobile brane
Mobile brane
modulated fluctuations
Conformal coupling problem
Chaotic inflation
scalar field associated with angular position at
KKLMMT03
Mukohyama, LK 05
Kallosh etal 02
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
string theoristCY
AdS3+1 FRW
Fluctuations in Cosmology with Compactification
string theoristCY
AdS3+1 FRW
3+1 FRW
Fluctuations in Cosmology with Compactification
CYcosmologist
string theorist
Practical cosmologist
CY
AdS
CY +fluctuations
3+1 FRW
3+1 FRW
3+1 FRW +fluctuations
Fluctuations in Cosmology with Compactification
CYcosmologist
Modulated Fluctuations
Hà1
x~
t
Light field at inflation
Inflation radiation
LK03, Dvali etal03
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
Scanning Inflation R.Bond, C.Contaldi,A.Frolov, L.KofmanT.SouradeepP.Vandrevange
Bottom-up
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
Ensemble of Inflationary trajectories
Chebyshev decomposition
Space of models opens wide
H(N) P(k)
ns;nt; r;dn=dlnk;As; :::
ï ;ñ:::
Observational constraints on trajectories
Markov Chain Monte Carlo
Degeneracy of the Potential Reconstruction
Reconstruction of Inflationary Trajectory
Cosmic Numerology: CMBall + LSS, stable & consistent pre-WMAP1 & post-WMAP1 (BCP03), Jun03 data (BCLP04), CMBall+CBIpol04, CMBall+Boom03+LSS
Jul’21 05, CMBall Jul05
LSS=2dF, SDSS (weak lensing, cluster abundances); also HST, SN1a
As = 22 +- 3 x 10-10
ns = .95 +- .02 (.97 +- .02 with tensor) (+- .004 PL1)
At / As < 0.36 95% CL (+- .02 PL2.5+Spider)
dns /dln k = -.07 +- .04 to -.05 +- .03 (+- .005 P1)
-.002 +- .01 (+Lya McDonald etal 04)
(Aiso / As < 0.3 large scale, < 3 small scale niso = 1.1+-.6)
The Parameters of Cosmic Structur Formation