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Natural Inflation after WMAP

Natural Inflation after WMAP

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Natural Inflation after WMAP

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  1. Natural Inflation after WMAP Katherine Freese Michigan Center for Theoretical Physics University of Michigan

  2. TWO TYPES OF INFLATION MODELS • TUNNELING MODELS Old Inflation (Guth 1981 Chain Inflation (Freese and Spolyar 2005) tunnel through series of vacua: in string landscape, or with QCD axion ROLLING MODELS Predictions being tested with CMB

  3. I. TUNNELING MODELSOld Inflation(Guth 1981) Universe goes from false vacuum to true vacuum. Bubbles of true vacuum nucleate in a sea of false vacuum (first order phase transition).

  4. Swiss Cheese Problem of Old Inflation: no graceful exit PROBLEM: Bubbles never percolate and thermalize: REHEATING FAILS; we don’t live in a vacuum Bubbles of true vacuum nucleate in a sea of false vacuum.

  5. What is needed for tunneling inflation to work? • Probability of a point remaining in false vacuum phase: where is the nucleation rate of bubbles and H is the expansion rate of the universe • The number of e-foldings per tunneling event is • Graceful exit: Critical value of is required to get percolation and reheating. In terms of number of efolds, this is • Sufficient Inflation requires

  6. Graceful Exit Achieved

  7. Inflation Requires Two Basic Ingredients • 1. Sufficient e-foldings of inflation • 2. The universe must thermalize and reheat • Old inflation, wih a single tunneling event, failed to do both. • Here, MULTIPLE TUNNELING events, each responsible for a fraction of an e-fold (adds to enough). Graceful exit is obtained: phase transition completes at each tunneling event.

  8. Multiple tunnelingevents Chain Inflation Freese & Spolyar (2005) Freese, Liu, & Spolyar (2005) • Graceful exit:requires that the number of e-foldings per stage is N < 1/3 • Sufficient inflation:total number of e-foldings is Ntot > 60 Relevant to: • stringy landscape • QCD (or other) axion

  9. Basic Scenario: Inflation with the QCD axion or in the Stringy Landscape V (a) = V0[1− cos (Na /v)] − η cos(a/v +γ) Chain Inflate: Tunnel from higher to lower minimum in stages, with a fraction of an efold at each stage Freese, Liu, and Spolyar (2005)

  10. Chain Inflation: Basic Setup • The universe transitions from an initially high vacuum down towards zero, through a series of tunneling events. • The picture to consider: tilted cosine • Solves old inflation problem: Graceful Exit requires that the number of e-folds per stage < 1/3 • Sufficient Inflation requires a total number of e-folds > 60, hence there are many tunneling events

  11. Chain Inflation in String Landscape • Chain inflation is generic in the string landscape, as the universe tunnels through a series of metastable vacua, each with different fluxes. There appear to be at least 10^200 vacua. Vacua of different fluxes are disconnected in the multidimensional potential, with barriers in between them. Chain inflation is the result of tunneling between these vacua. N.b. Quantized drops in four-form field strength. Tunneling can be fast early on; can it stop without going through intermediate slow stage?

  12. Chain Inflation with QCD Axion • Low scale inflation at 200 MeV: axion can simultaneously solve strong CP problem and provide inflation • In addition to standard QCD axion, need (i) new heavy fermions to get many bumps in the theta field and (ii) tilt from soft breaking of underlying PQ symmetry

  13. Rolling Models of Inflation Linde (1982) Albrecht & Steinhardt (1982) • Equation of motion: • Flat region: • V almost constant • rvac dominatesenergy density • Decay of f: • Particle production • Reheating

  14. On: the role of observations “Faith is a fine invention When Gentlemen can see --- But Microscopes are prudent In an Emergency Emily Dickinson, 1860

  15. 50-60e-foldings Spectrum of Perturbations • Total number of inflation e-foldings Ntot 60 • Spectrum of observable scales is produced~ 50 – 60 e-foldings before the end of inflation • 50: later during inflation smaller scales (~1 Mpc) • 60: earlier during inflation larger scales (~3000 Mpc)

  16. Tensor (gravitational wave) modes • In addition to density fluctuations, inflation also predicts the generation of tensor fluctuations with amplitude • For comparison with observation, the tensor amplitude is conventionally expressed as: • (denominator: scalar modes)

  17. Gravity Modes are (at least) two orders of magnitude smaller than density fluctuations: hard to find!

  18. Four parameters from inflationary perturbations: I. Scalar perturbations: amplitude spectral index II. Tensor (gravitational wave) modes: amplitude spectral index Expressed as Inflationary consistency condition: Plot in r-n plane

  19. Different Types of Potentials in the r-n plane (KINNEY 2002)

  20. Examples of Models

  21. Effect of more data WMAP I WMAP I Ext WMAP II LCDM model Reducing the noise by 3 degeneracies broken

  22. Tensor-to-scalar ratio r vs. scalar spectral index n

  23. Specific models critically tested dns/dlnk=0 dns/dlnk=0 r r n n Models like V(f)~fp p=4 p=2 For 50 and 60 e-foldings p fix, Ne varies HZ (taken from L. Verde) p varies, Ne fix

  24. The full treatment:

  25. Natural Inflation after WMAP Chris Savage, K. Freese, W. Kinney, hep-ph/ 0609144 Theoretical motivation: no fine-tuning Recent interest in light of theoretical developments Unique predictions: Looks good compared to data

  26. Fine Tuning in Rolling Models • The potential must be very flat: (Adams, Freese, and Guth 1990) But particle physics typically gives this ratio = 1!

  27. Inflationary Model Constraints Success of inflationary models with rolling fields constraints on V(f) • Enough inflation Scale factor a must grow enough • Amplitude of density fluctuations not too large

  28. + + +    lg Fine Tuning due to Radiative Corrections • Perturbation theory: 1-loop, 2-loop, 3-loop, etc. • To keep must balance tree level term against corrections to each order in perturbation theory. Ugly!

  29. Inflation needs small ratio of mass scales • Two attitudes: 1) We know there is a heirarchy problem, wait until it’s explained 2) Two ways to get small masses in particles physics: (i) supersymmetry (ii) Goldstone bosons (shift symmetries)

  30. Natural Inflation: Shift Symmetries • Shift (axionic) symmetries protect flatness of inflaton potential (inflaton is Goldstone boson) • Additional explicit breaking allows field to roll. • This mechanism, known as natural inflation, was first proposed in Freese, Frieman, and Olinto 1990;Adams, Bond, Freese, Frieman and Olinto 1993

  31. Shift Symmetries  “Natural Inflation” Freese, Frieman & Olinto (1990) • We know of a particle with a small ratio of scales: the axion • IDEA: use a potential similar to that for axions in inflation natural inflation (no fine-tuning) • Here, we do not use the QCD axion.We use a heavier particle with similar behavior.

  32. e.g., mimic the physics of the axion (Weinberg; Wilczek)

  33. Natural Inflation(Freese, Frieman, and Olinto 1990; Adams, Bond, Freese, Frieman and Olinto 1993) • Two different mass scales: • Width f is the scale of SSB of some global symmetry • Height is the scale at which some gauge group becomes strong

  34. Two Mass Scales Provide required heirarchy • For QCD axion, • For inflation, need Enough inflation requires width = f ≈ mpl, Amplitude of density fluctuations requires height =

  35. x Sufficient Inflation • f initially randomly distributed between 0 and pfat different places in the universe. • T < : f rolls down the hill. The pieces of the universe with f far enough uphill will inflate enough. T > L T < L

  36. x Sufficient Inflation • f rolls down the hill.The pieces of the universe with f far enough uphill will inflate enough. T < L

  37. Sufficient Inflation • A posteriori probability:Those pieces of the universe that do inflate end up very large. Slice the universe after inflation and see what was probability of sufficient inflation. • Numerically evolved scalar field For f 0.06MPl ,P = O(1)

  38. Density Fluctuations Largest at 60 efolds before end of inflation  L ~ 1015 GeV – 1016 GeV (height of potential)  mf = L2/f ~ 1011 GeV – 1013 GeV • Density fluctuation spectrum is non-scale invariant with extra power on large length scales WMAP  f > 0.7 MPL

  39. Implementations of natural inflation’s shift symmetry • Natural chaotic inflation in SUGRA using shift symmetry in Kahler potential(Gaillard, Murayama, Olive 1995; Kawasaki, Yamaguchi, Yanagida 2000) • In context of extra dimensions: Wilson line with(Arkani-Hamed et al 2003)but Banks et al (2003) showed it fails in string theory. • “Little” field models(Kaplan and Weiner 2004) • In brane Inflation ideas(Firouzjahi and Tye 2004) • Gaugino condensation in SU(N) SU(M): Adams, Bond, Freese, Frieman, Olinto 1993; Blanco-Pillado, Linde et al 2004(Racetrack inflation)

  40. Legitimacy of large axion scale? Natural Inflation needs Is such a high value compatible with an effective field theory description? Do quantum gravity effects break the global axion symmetry? Kinney and Mahantappa 1995: symmetries suppress the mass term and is OK. Arkani-Hamed et al (2003):axion direction from Wilson line of U(1) field along compactified extra dimension provides However, Banks et al (2003) showed it does not work in string theory.

  41. A large effective axion scale(Kim, Nilles, Peloso 2004) • Two or more axions with low PQ scale can provide large • Two axions • Mass eigenstates are linear combinations of • Effective axion scale can be large,

  42. A large number of fields • Assisted Inflation (Liddle and Mazumdar 1998) • N-flation (Dimopoulos, Kachru, McGreevy, Wacker 2005): Shamit’s talk this morning • Creation of cosmological magnetic fields (Anber and Sorbo 2006)

  43. Density Fluctuations and Tensor Modes can determine which model is right Density Fluctuations and Tensor Modes • Density Fluctuations: WMAP data: Slight indication of running of spectral index • Tensor Modes gravitational wave modes, detectable in upcoming experiments

  44. Density Fluctuations in Natural Inflation • Power Spectrum: • WMAP data: implies (Freese and Kinney 2004)

  45. Tensor Modes in Natural Inflation(original model)(Freese and Kinney 2004) Two predictions, testable in next decade: 1) Tensor modes, while smaller than in other models, must be found. 2) There is very little running of n in natural inflation. n.b. not much running of n Sensitivity of PLANCK: error bars +/- 0.05 on r and 0.01 on n. Next generation expts (3 times more sensitive) must see it.

  46. Natural Inflation agrees wellwith WMAP!

  47. f > 0.7 MPl allowed r-n plane: Natural inflation after WMAP 3

  48. small f : (exponentially suppressed) large f : Spectral Index Running

  49. The full treatment:

  50. Potential • 60 e-foldings before the end of inflation ~ present day horizon