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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.
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Inflation and Branes Top-downapproach 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 UniverseInflation Scale factor time Realization of Inflation
Particlegenesis time Inflation no entropy no temperature BANG
Decay of inflaton and preheating after inflation Classical Quantum movie Felder, LK, Linde, 01,05
Decay of inflaton and preheating after inflation Classical Quantum
Initial conditions from Inflation inflation Hot FRW
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
Inflation in the context of ever changing fundamental theory 1980 -inflation Old Inflation New Inflation Chaotic inflation SUGRA inflation Power-law inflation Double Inflation Extended inflation 1990 Hybrid inflation Assisted inflation SUSY F-term inflation SUSY D-term inflation Brane inflation Super-natural Inflation 2000 SUSY P-term inflation K-flation N-flation DBI inflation inflation Warped Brane inflation Tachyon inflation Racetrack 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 Randal, Sundrum 99
New ideas about mass hierarchy New ideas about Inflation New ideas about cosmological constant New ideas about 4d gravity New interactions with SM particles
Stabilization of Inner dimensions and moduli in string theory
Realization of String Theory Inflation on the ground of KKLT throat warped geometry KKLMMT03 Hybrid inflation with inflaton fluctuations Mobile brane Conformal coupling problem modulated fluctuations scalar field associated with angular position at Kallosh etal 02 Mukohyama, LK 05 Mobile brane Chaotic inflation
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
Fluctuations in Cosmology with Compactification string theorist CY AdS 3+1 FRW
Fluctuations in Cosmology with Compactification string theorist CY cosmologist CY 3+1 FRW AdS 3+1 FRW
Fluctuations in Cosmology with Compactification string theorist CY cosmologist CY 3+1 FRW AdS 3+1 FRW CY +fluctuations Practical cosmologist 3+1FRW +fluctuations
ModulatedFluctuations Inflationradiation Light field at inflation LK03, Dvali etal03
4 dim Inflation in 10dim String Theory predicts All what 4 dim inflation predicts Creation of non-SM particles (KK modes) in reheating/thermalization Short-wavelength gravitational radiation Scale free gaussian fluctuations of many light scalars Modulated cosmological fluctuations String theory Cosmic strings
Scanning Inflation R.Bond, C.Contaldi, A.Frolov, L.Kofman T.Souradeep P.Vandrevange Bottom-up
Inflation in the context of ever changing fundamental theory 1980 -inflation Old Inflation New Inflation Chaotic inflation SUGRA inflation Power-law inflation Double Inflation Extended inflation 1990 Hybrid inflation Assisted inflation SUSY F-term inflation SUSY D-term inflation Brane inflation Super-natural Inflation 2000 SUSY P-term inflation K-flation N-flation DBI inflation inflation Warped Brane inflation Tachyon inflation Racetrack inflation
Ensemble of Inflationary trajectories Chebyshev decomposition Space of models opens wide
Observational constraints on trajectories Markov Chain MonteCarlo
The Parameters of Cosmic Structur Formation 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)