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Inflation after WMAP Kin-Wang Ng ( 吳建宏 ) Academia Sinica, Taiwan

Inflation after WMAP Kin-Wang Ng ( 吳建宏 ) Academia Sinica, Taiwan. 2nd International Workshop on Dark Matter, Dark Energy, and Matter-Antimatter Asymmetry Hsinchu, Nov 5 – 6 , 2010. Collaborators: Yeo-Yie Charng, Hing-Tong Cho, Da-Shin Lee, Wolung Lee,

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Inflation after WMAP Kin-Wang Ng ( 吳建宏 ) Academia Sinica, Taiwan

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  1. Inflation after WMAPKin-Wang Ng (吳建宏)Academia Sinica, Taiwan 2nd International Workshop on Dark Matter, Dark Energy, and Matter-Antimatter Asymmetry Hsinchu, Nov 5 – 6 , 2010 Collaborators: Yeo-Yie Charng, Hing-Tong Cho, Da-Shin Lee, Wolung Lee, I-Chin Wang, Chun-Hsien Wu

  2. Outline • Cosmic background backgroud anisotropy and WMAP observation • Primordial density perturbation scale-invariant, running spectral index, Gaussianity • Large-scale CMB anomalies • Implications to inflation

  3. 7-year WMAP 2010

  4. PR(k)= (δρ/ρ)2

  5. Running spectral index

  6. Inflation and Primordial Density Fluctuations

  7. H

  8. PR(k)= (δρ/ρ)2 |dn/dlnk| << |n-1|

  9. Curvature potential Slow-roll inflation Radiation transfer function ▽2Φ=δρ/ρ WMAP3 Data on Non-Gaussianity

  10. Large-scale CMB anomalies

  11. Low quadrupole WMAP1 WMAP3

  12. northern hemisphere southern hemisphere full sky Eriksen et al 04 Park 04 South-North Power Asymmetry Eriksen et al 04 North pole (80o,57o)

  13. WMAP3 CMB sky map

  14. “Axis of Evil” Land & Magueijo 05 l=2, quadrupole l=3, octopole

  15. Slow-roll kinematics Quantum fluctuations A Challenge to Standard Slow-roll inflation!? • Chaotic inflation – classical fluctuations driven by a white noise (Starobinsky) or by a colored noise (Liguori, Matarrese et al.) coming from high-k inflaton • Driven by a colored noise from interacting quantum environment (Wu et al) • Trapped inflation (Green et al) • Slow-roll conditions violated after horizon crossing (Leach et al) • General slow-roll condition (Steward) |n-1|~|dn/dlnk| • Multi-field (Vernizzi, Tent, Rigopoulos, Yokoyama et al) • etc

  16. Our Inflaton-Scalar Interacting Model (Wu et al 07) Single-field inflation〈σ〉= 0

  17. Dissipation Noise imaginary part real part Colored, dependent on history Trace out sigma field to obtain : Feynman & Vernon 1963 Influence Functional Method semi-classical

  18. Start of inflation

  19. Dominant passive fluctuations and low CMB quadrupole assuming no active de Sitter quantum fluctuations

  20. Relative large three-point functions ns Dissipation? Running spectral index and Non-gaussianity • We propose a new dynamical source for density perturbation: Colored Quantum Noise - give alow CMB quadrupole • Can be applied to trapped inflation (Green et al. 09) • Working on running spectral index and non-Gaussianity, both are natural with colored noise

  21. Following is an effort to go from homogenous to directional effects

  22. A black hole in inflation Cho, Ng, Wang 09 M - black hole mass H - Hubble parameter Schwarzschild-de Sitter Static ------> Planar

  23. Inflaton fluctuations Expansion parameter where the source term

  24. Solutions Zero order First order

  25. Power spectrum de Sitter quantum fluctuations End of inflation  → 0

  26. Inflation early universe present universe Possible effects to CMB anisotropy e.g. black holes formed via thermal fluctuations Scardigli et al. Carroll, Tseng, & Wise 08 preferred point, line, or plane

  27. Speculations • Is it possible not to fine tune inflation duration to 60 efolds? • Then there must be something taking place during slow-roll inflation • Formation rate must not be far below the expansion rate of inflation • e.g. Collapse of density peaks of quantum fluctuations during inflation or…

  28. String Landscape • 10500 de Sitter vacua • Metastable, bubble nucleation via tunneling • Barriers of string scale, slow tunneling rate • The spacetime is a hierachy of de Sitter vacuum bubbles • Most part in eternal inflation • Some regions tunnel down to flat potential for slow-roll infaltion • We sit in a vacuum with a small cosmological constant today

  29. slow-roll inflation in a de Sitter vauum Λ2 Will these bubbles Λ1collapse into black holes? Efficient and rapid tunneling Tye, Shiu,… Λ2 Λ1

  30. surface tension Motion of the bubble wall bubble radius

  31. Work is in progress towardsan explanation of large-scale CMB anomalies with black holes, domain filaments, and bubble walls

  32. Conclusion • Hints from WMAP data on beyond standard slow-roll inflation !? • A fine tuning – physics just at 60 e-foldings • Maybe there is a window to see the first few e-foldings of inflation !? • Many models give a suppressed CMB low multipoles and/or directional effects • Perhaps we are all fooled by probability – it is indeed a Gaussian quantum process • Nongaussianity is an important check

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