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More on the A-Word

More on the A-Word. Credit: Anthony Aguirre, Martin Rees, Frank Wilczek Blame: Max Tegmark. dse. Big Bang Zoom. Four gradual discoveries: The Universe is much larger than once imagined The Universe can be well described mathematically

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More on the A-Word

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  1. More on the A-Word Credit: Anthony Aguirre, Martin Rees, Frank Wilczek Blame: Max Tegmark

  2. dse

  3. Big Bang Zoom • Four gradual discoveries: • The Universe is much larger than once imagined • The Universe can be well described mathematically • In most theories, we can’t observe everything that exists • There are selection effects

  4. Big Bang Zoom How big is our Universe?

  5. Big Bang Zoom • Four gradual discoveries: • The Universe is much larger than once imagined • The Universe can be well described mathematically • In most theories, we can’t observe everything that exists • There are selection effects • - probability that a random point in our observable universe is near the surface of a planet ~ 10-43

  6. Big Bang Zoom • If we want to test a mathematical theory predicting a larger universe than we can observe, then we’re forced to compute anthropic selection effects. • That this is hard isn’t Alex Vilenkin’s fault! So we shouldn’t vent our frustrations on those who try to work on the problem..

  7. Cmbgg OmOl The Standard Model Lagrangian L= (From T.D. Gutierrez)

  8. Cmbgg OmOl  C = h = G = kb = qe = 1 Particle physics Standard model parameters: Required Cosmology Optional

  9. Cmbgg OmOl How measure? Particle physics Standard model parameters: Why these values? Required Cosmology Optional

  10. Cmbgg OmOl

  11. Cmbgg OmOl

  12. (Graphics from Gary Hinshaw/WMAP team)

  13. Brief History of the Universe Fluctuation generator Fluctuation amplifier Hot Dense Smooth Cool Rarefied Clumpy (Graphics from Gary Hinshaw/WMAP team)

  14. MATTER BUDGET Required (Q) Optional INITIAL CONDITIONS tot

  15. OUR TOOLS

  16. Smorgasbord

  17. Measuring clustering

  18. History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496

  19. Boomzoom z = 1000

  20. Boomzoom z = 2.4 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

  21. Boomzoom z = 0.8 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

  22. Boomzoom z = 0 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

  23. 1parmovies LSS

  24. 1parmovies Clusters LSS Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  25. 1parmovies CMB Clusters LSS Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  26. 1parmovies CMB Clusters LSS Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  27. 1parmovies CMB Clusters LSS Lensing Ly Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  28. 1parmovies CMB Clusters LSS Lensing Lya Tegmark & Zaldarriaga, astro-ph/0207047 + updates

  29. ? Cosmological data Cosmological Parameters Why these particular values? Nature of dark matter? Nature of dark energy? Fundamental theory Nature of early Universe?

  30. PREDICTING

  31. PREDICTING It's tough to make predictions, especially about the future. Yogi Berra

  32. Cmbgg OmOl Parameter status?

  33. Cmbgg OmOl Parameter status? Environmental Environmental Fundamental? Fundamental?

  34. Big Bang Zoom What are the 4 multiverse levels like? Same effective laws of physics, different initial conditions Same fundamental laws of physics, different effective laws Nothing qualitatively new Different fundamental laws of physics

  35. Cmbgg OmOl Motivates B What determines the constants of nature? What do the constants of nature determine? Most of our paper Certified 100% philosophy free!

  36. Cmbgg OmOl Three little numbers:

  37. Cmbgg OmOl R~ /mp M~ mp Weisskopf 1975 Carr & Rees 1979

  38. Cmbgg OmOl R~ 1/1/21/2mp2 M~ 3/23/2 /mp2

  39. Cmbgg OmOl R~1/mp21/2 M~ 3/2 /mp2 Weisskopf 1975 Carr & Rees 1979

  40. Cmbgg OmOl R~ /mp3/23/4 M~ 3/4 /mp1/2 Carr & Rees 1979

  41. Cmbgg OmOl

  42. Cmbgg OmOl M~ /mp2 Weisskopf 1975 Carr & Rees 1979

  43. Cmbgg OmOl R~ 3 /mp33/2 M~ 5 /mp31/2 Carr & Rees 1979

  44. Cmbgg OmOl R~ /mp5 M~ /mp5 Carr & Rees 1979

  45. Cmbgg OmOl Based on Carr & Rees 1979, Barrow & Tipler 1986 Inside black hole Below quantum limit

  46. Cmbgg OmOl Fine-tuning? NO! Based on Carr & Rees 1979, Barrow & Tipler 1986 Inside black hole Below quantum limit

  47. Big Bang Zoom MT 1998,gr-qc/9704009, Ann. Phys., 270, 1-51

  48. Cmbgg OmOl Most spectacular fine tuning known outside cosmology is arguably in nuclear physics

  49. Cmbgg OmOl Savas will return to this! Effect of Higgs VEV v=246 GeV: Agrawal, Barr, Donoghue & Seckel 1998, PRL, 80, 1822 • v/v0<0.5: protons (uud) decay into neutrons (udd) • v/v0<0.8: diproton & dineutron • v/v0=1: we are here • v/v0>2: deuterium unstable • v/v0>5: neutrons (udd) unstable even in nuclei • v/v0>103: protons (uud) decay to ++ (uuu)

  50. Cmbgg OmOl Oberhummer, Csoto & Schlattl, astro-ph/0007178, Science, 289, 88 + 8Be 8Be+ 12C 12C+ 16O C & O yield given by one parameter that depends on , mu/QCD, md/QCD : Jeltema & Sher, hep-ph/9905494 oxygen carbon oxygen carbon carbon oxygen 5 Msun 1.3 Msun 20 Msun

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