Cosmology and theorigin of structureRocky I: The universe observed Rocky II:The growth of cosmological structureRocky III:Inflation and the origin of perturbationsRocky IV:Dark matter and dark energy

origin of small initial perturbations

Motivation for acausal perturbations Inflation in the cosmic symphony The alarming phenomenon of particle creation Inflation phenomenologyRocky III: Inflation

Acoustic peaks At recombination, baryon-photon fluid undergoes acoustic oscillations Compressions and rarefactions change Peaks in correspond to extrema of compressions and rarefactionsHu

Angular power spectrumisocurvature perts (no A)adiabatic A (acausal)

Input from the early universe1. Spectrum of perturbations (power spectrum)CMB correlations on scales greater thanHubble radius (RH~ct) INFLATION

2. Matter contentbaryons, dark matter (cold, warm, hot),vacuum energy,

non-inflationarycosmologynon-inflationarycosmology

inflationarycosmologyinflationarycosmology

Vacuum pressurehad to pull pistonnegative pressure

log alog RH ; log l

Cosmic Symphony (Harmonice Mundi)expansion tempo

pizzicato string dominated10-43 sec.? ???

CBR fluctuations, presto inflation 10-35 sec.? gravitational waves, seeds of structure allegro radiation dominatedearlier than abundance of the 10,000 yrs. light elements

andante matter dominated later than distant quasars 10,000 yrs. and galaxies

largo inflation day beforeacceleration of yesterday the universemovement epoch relic

Inflation, as a whole, canbe divided into three partsBeginning

Middle

Enddensity perturbations, gravitational waves,(particle production in the expanding universe)eternal inflation, wave function of the universe,did the universe have a beginning ????defrosting, heating, preheating, reheating, baryogenesis, phase transitions, dark matter,(particle production in the expanding universe)

Classical equations of motionPotential energy: energy of infinite-wavelength modeParticle content: condensate of infinite-wavelength particles

An early particle cosmologistIn mid-1930s, Schrodinger turned to cosmo issues, influenced by Eddington & Lemaitre1938-1939: Graz Vatican Gent, Belgium Dublin..

proper vibrations [positive and negative frequency modes] cannot be rigorously separated in the expanding universe. this is a phenomenon of outstanding importance. With particles it would mean production or annihilation of matter, merely by expansion, Alarmed by these prospects, I have examined the matter in more detail. There will be a mutual adulteration of positive and negative frequency terms in the course of time, giving rise to the alarming phenomenonIntroduction:Conclusion:The proper vibrations of the expanding universe

An even earlier Graz cosmologist1600-1630: Graz Prague Linz Sagan RatisbonWhen the storms rage around us, and the state is threatened by shipwreck, we can do nothing more noble than to lower the anchor of our peaceful studies in the ground of eternity. - J. Kepler

inflaton

log alog RH ; log lquantum fluctuationsalarming phenomenon

patterns of quantum fluctuations

Variational Formalism for Quantization:Scalar perturbations in terms of a field uMinkowski space(conformal time)mass changes with time

Variational formalism for quantization:Minkowski space(conformal time)changes in timeEinstein gravityInflaton fieldTensor perturbations in terms of

Quantum generation of perturbations: Initially only homogeneous mode. As evolve, mass is complicated function of time. Create nonzero momentum mode. Alarming phenomenon! Wave equation for u

(When a hammer is your only tool, everything has theappearance of a nail.)

Who is the inflaton?inflaton

Top downBottom up

Models of inflationold, new, pre-owned,chaotic, quixotic, ergodic,ekpyrotic, autoerotic,faith-based, free-based, brane, braneless, brainless,supersymmetric, supercilious,natural, supernatural, au natural,hybrid, low-bred, white bread,one-field, two-field, left-field,eternal, internal, infernal,self-reproducing, self-promoting, dilaton, dilettante, .

Model ClassificationType I: single-field, slow-roll models (or models that can be expressed as such)

Type II: anything else (branes, pre-big-bang, etc.)Type Ia: large-field modelsType Ib: small-field modelsType Ic: hybrid models

small-field (Ib)hybrid (Ic)

Quantum generation of perturbations: Characterize perturbations in terms of: Perturbations model-dependent function of H and how H changes during inflation.

Quantum generation of perturbations: Observer-friendly parameters:

Consistency relation:

Inflaton potential : Input inflation potential :

0 0.5 1.0n0.8 0.85 0.9 0.95 1.0 1.05 1.1rhybridlarge fieldsmall fieldDodelson, Kinney, Kolb astro-ph/9702156

Kinney, Melchiorri, Riottoastro-ph/0007375

Harrison-Zeldovichn = 1.00000r = 0.00000

Fixed point of ignorance.

Polarization pattern E modes B modes (gravitational waves)Stebbins, Kosowsky, Kamionkowski Seljak & Zaldarriaga

astro-ph/9806259Kinney

ReconstructionBond, Abney, Copeland, Grivell, Kolb, Liddle, Lindsey, Turner, Sourdeep

Reconstructiontensor spectral index in terms of scalar & tensor (consistency relation)knowledge of the scale of V requires tensor

Power-law spectrum

Power-law spectrum

Type I models* predicta (nearly) exact power-lawspectrum of gaussiansuper-Hubble-radiusscalar (density) andtensor (gravitational-wave) perturbationsrelated by a consistency relationin their growing modein a spatially flat universe.*at least the simplest ones

Inflation conclusionsThe alarming phenomenon of particle creation in the early universe can be studied by looking at the sky!

If you can look into the seeds of timeAnd say which grain will grow and which will not,Speak then to me, who neither beg nor fearYour favours nor your hate.-MACBETH (Banquo)

Rocky III: Inflation Motivation for acausal perturbations Inflation in the cosmic symphony The alarming phenomenon of particle creation Inflation phenomenology

Cosmology and theorigin of structureRocky I: The universe observed Rocky II:The growth of cosmological structureRocky III:Inflation and the origin of perturbationsRocky IV:Dark matter and dark energy