Cosmic Inflation Phy 262 2013 Andreas Albrecht - PowerPoint PPT Presentation

slide1 n.
Download
Skip this Video
Loading SlideShow in 5 Seconds..
Cosmic Inflation Phy 262 2013 Andreas Albrecht PowerPoint Presentation
Download Presentation
Cosmic Inflation Phy 262 2013 Andreas Albrecht

play fullscreen
1 / 264
Cosmic Inflation Phy 262 2013 Andreas Albrecht
143 Views
Download Presentation
alaire
Download Presentation

Cosmic Inflation Phy 262 2013 Andreas Albrecht

- - - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - - -
Presentation Transcript

  1. Cosmic Inflation Phy 262 2013 Andreas Albrecht A. Albrecht @ Stanford Jan 7 2013

  2. Cosmic Inflation: • Great phenomenology, but • Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. A. Albrecht @ Stanford Jan 7 2013

  3. Cosmic Inflation: • Great phenomenology, but • Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. This Talk A. Albrecht @ Stanford Jan 7 2013

  4. Cosmic Inflation: • Great phenomenology, but • Original goal of explaining why the cosmos is *likely* to take the form we observe has proven very difficult to realize. • OR: Just be happy we have equations to solve? A. Albrecht @ Stanford Jan 7 2013

  5. OUTLINE Big Bang & inflation basics Eternal inflation de Sitter Equilibrium cosmology Cosmic curvature from de Sitter Equilibrium cosmology A. Albrecht @ Stanford Jan 7 2013

  6. OUTLINE Big Bang & inflation basics Eternal inflation de Sitter Equilibrium cosmology Cosmic curvature from de Sitter Equilibrium cosmology A. Albrecht @ Stanford Jan 7 2013

  7. Friedmann Eqn. A. Albrecht @ Stanford Jan 7 2013

  8. Friedmann Eqn. A. Albrecht @ Stanford Jan 7 2013

  9. Friedmann Eqn. Hubble parameter (“constant”, because today it takes ~10Billion years to change appreciable) A. Albrecht @ Stanford Jan 7 2013

  10. Friedmann Eqn. Hubble parameter (“constant”, because today it takes ~10Billion years to change appreciable) “Scale factor” A. Albrecht @ Stanford Jan 7 2013

  11. Friedmann Eqn. Curvature “Scale factor” A. Albrecht @ Stanford Jan 7 2013

  12. Friedmann Eqn. Curvature Relativistic Matter “Scale factor” A. Albrecht @ Stanford Jan 7 2013

  13. Friedmann Eqn. Curvature Non-relativistic Matter Relativistic Matter “Scale factor” A. Albrecht @ Stanford Jan 7 2013

  14. Friedmann Eqn. Dark Energy Curvature Non-relativistic Matter Relativistic Matter “Scale factor” A. Albrecht @ Stanford Jan 7 2013

  15. Evolution of Cosmic Matter A. Albrecht @ Stanford Jan 7 2013

  16. Evolution of Cosmic Matter A. Albrecht @ Stanford Jan 7 2013

  17. Evolution of Cosmic Matter A. Albrecht @ Stanford Jan 7 2013

  18. The curvature feature/“problem” A. Albrecht @ Stanford Jan 7 2013

  19. The curvature feature/“problem” ! A. Albrecht @ Stanford Jan 7 2013

  20. The curvature feature/“problem” ! A. Albrecht @ Stanford Jan 7 2013

  21. The curvature feature/“problem” ! A. Albrecht @ Stanford Jan 7 2013

  22. The curvature feature/“problem” A. Albrecht @ Stanford Jan 7 2013

  23. The curvature feature/“problem” ! A. Albrecht @ Stanford Jan 7 2013

  24. i W a 1 In the SBB, flatness is an “unstable fixed point”: Dominates with time At or The “GUT scale” Require today to 55 decimal places to get I.0 What is Cosmic Inflation?

  25. i W a 1 In the SBB, flatness is an “unstable fixed point”: SBB = “Standard Big Bang” cosmology, or “cosmology without inflation”. Dominates with time At or The “GUT scale” Require today to 55 decimal places to get I.0 What is Cosmic Inflation?

  26. i Gravitational instability: The Jeans Length Average energy density Sound speed • Overdense regions of size • collapse under their own weight. • If the size is they just oscillate I.0 What is Cosmic Inflation?

  27. i SBB Homogeneity: On very large scales the Universe is highly homogeneous, despite the fact that gravity will clump matter on scales greater than RJeans At the GUT epoch the observed Universe consisted of 1079RJeanssized regions. The Universe was very smooth to start with. NB: Flatness & Homogeneity SBB Universe starts in highly unstable state. I.0 What is Cosmic Inflation?

  28. i SBB Monopoles • A GUT phase transition (or any other process) that injects stable non-relativistic matter into the universe at early times (deep in radiation era, ie Ti =1016 GeV) will *ruin* cosmology: Monopole dominated Universe I.0 What is Cosmic Inflation?

  29. The monopole “problem” A. Albrecht @ Stanford Jan 7 2013

  30. The monopole “problem” ! A. Albrecht @ Stanford Jan 7 2013

  31. i Here & Now SBB Horizon t=0 1080 causally disconnected regions at the GUT epoch Horizon: The distance light has traveled since the big bang: I.0 What is Cosmic Inflation?

  32. The flatness, homogeneity & horizon features become “problems” if one feels one must explain initial conditions. Basically, the SBB says the universe must start in a highly balanced (or “fine tuned”) state, like a pencil on its point. Must/can one explain this? Inflation says “yes” I.0 What is Cosmic Inflation?

  33. Friedmann Eqn. Dark Energy Curvature Non-relativistic Matter Relativistic Matter A. Albrecht @ Stanford Jan 7 2013

  34. Now add cosmic inflation Friedmann Eqn. Dark Energy Inflaton Curvature Non-relativistic Matter Relativistic Matter A. Albrecht @ Stanford Jan 7 2013

  35. Now add cosmic inflation Friedmann Eqn. Dark Energy Inflaton Curvature Non-relativistic Matter Relativistic Matter  A. Albrecht @ Stanford Jan 7 2013

  36. Now add cosmic inflation Friedmann Eqn. Dark Energy Inflaton Curvature Non-relativistic Matter Relativistic Matter A. Albrecht @ Stanford Jan 7 2013

  37. The inflaton: ~Homogeneous scalar field obeying Cosmic damping Coupling to ordinary matter All potentials have a “low roll” (overdamped) regime where A. Albrecht @ Stanford Jan 7 2013

  38. The inflaton: ~Homogeneous scalar field obeying Cosmic damping Coupling to ordinary matter All potentials have a “low roll” (overdamped) regime where A. Albrecht @ Stanford Jan 7 2013

  39. Add a period of Inflation: A. Albrecht @ Stanford Jan 7 2013

  40. With inflation, initially large curvature is OK: A. Albrecht @ Stanford Jan 7 2013

  41. With inflation, early production of large amounts of non-relativistic matter (monopoles) is ok : A. Albrecht @ Stanford Jan 7 2013

  42. With inflation, early production of large amounts of non-relativistic matter (monopoles) is ok : A. Albrecht @ Stanford Jan 7 2013

  43. Inflation detail: A. Albrecht @ Stanford Jan 7 2013

  44. Inflation detail: A. Albrecht @ Stanford Jan 7 2013

  45. Hubble Length A. Albrecht @ Stanford Jan 7 2013

  46. Hubble Length (aka ) A. Albrecht @ Stanford Jan 7 2013

  47. A. Albrecht @ Stanford Jan 7 2013

  48. A. Albrecht @ Stanford Jan 7 2013

  49. A. Albrecht @ Stanford Jan 7 2013

  50. A. Albrecht @ Stanford Jan 7 2013