Chapter 22 The Beginning of Time

1. Chapter 22The Beginning of Time

2. The Big Bang Run the expansion of the universe backward in time and you reach the moment of the beginning (The term creation implies a metaphysical event.) This moment is now called the Big Bang. The beginning is tied to the ending by everything in between. So everything has to fit together here. This is the subject of cosmology.

3. What were conditions like in the early universe?

4. The early universe must have been extremely hot and dense

5. Pair Production Photons converted into particle-antiparticle pairs and vice-versa E = mc2 Early universe was full of particles and radiation because of its high temperature

6. What is the history of the universe according to the Big Bang theory?

7. Planck Era Before Planck time (~10-43 sec) No theory of quantum gravity so we cannot yet describe this time. Ended when gravity separated from GUT force

8. Do forces unify at high temperatures? Four known forces in universe: Strong Force Electromagnetism Weak Force Gravity Yes! (Electroweak) Maybe (GUT) Who knows? (String Theory)

9. GUT Era Lasts from Planck time (~10-43 sec) to end of GUT force (~10-38 sec) Only slightly better understood than the Plank Era Ends with inflation.

10. Electroweak Era Lasts from end of GUT force (~10-38 sec) to end of electroweak force (~10-10 sec) We have created temps ~ to what existed at the end of the Electroweak Era inside of supercolliders. First time we can recreate the conditions that might have been.

11. Particle Era Amounts of matter and antimatter nearly equal Creation of subatomic particles. (Roughly 1 extra proton for every 109 proton-antiproton pairs!) Ends when pair production stops.

12. Era of Nucleo-synthesis Begins when matter annihilates remaining antimatter at ~ 0.001 sec Nuclei begin to fuse Composition of the normal matter in the universe set. 75% Hydrogen 25% Helium

13. Era of Nuclei To hot for electrons to bind to nuclei to create atoms. Photons bounce between electrons being absorbed and reemitted. Opaque universe Ends with the creation of atoms at 380,000 yrs and 3000K.

14. Era of Atoms Atoms form at age ~ 380,000 years When atoms from the universe becomes transparent. Background radiation released.

15. Era of Galaxies Galaxies form at age ~ 1 billion years

16. Primary Evidence We have detected the leftover radiation from the Big Bang. The Big Bang theory correctly predicts the abundance of helium and other light elements.

17. How do we observe the radiation left over from the Big Bang?

18. The cosmic microwave background – the radiation left over from the Big Bang – was detected by Penzias & Wilson in 1965

19. Background radiation from Big Bang has been freely streaming across universe since atoms formed at temperature ~ 3,000 K: visible/IR

20. Background has perfect thermal radiation spectrum at temperature 2.73 K Expansion of universe has redshifted thermal radiation from that time to ~1000 times longer wavelength: microwaves

21. WMAP gives us detailed baby pictures of structure in the universe

22. How do the abundances of elements support the Big Bang theory?

23. Protons and neutrons combined to make long-lasting helium nuclei when universe was ~ 3 minutes old

24. Big Bang theory prediction: 75% H, 25% He (by mass) Matches observations of nearly primordial gases

25. Abundances of other light elements agree with Big Bang model having 4.4% normal matter – more evidence for WIMPS!

26. What aspects of the universe were originally unexplained with the Big Bang theory?

27. Mysteries Needing Explanation Where does structure come from? Why is the overall distribution of matter so uniform? Why is the density of the universe so close to the critical density? An early episode of rapid inflation can solve all three mysteries!

28. 0 Problems with the Classical, Decelerating Universe: • The flatness problem: The universe seems to be nearly flat. Even a tiny deviation from perfect flatness at the time of the Big Bang should have been amplified to a huge deviation today. => Extreme fine tuning required!

29. 2) The Horizon Problem, The isotropy of the cosmic background: If information can only travel through the universe at the speed of light, then structure in the cosmic background should not be correlated over large angular scales! • Contradiction to almost perfect isotropy of the cosmic background!

30. Inflation can make all the structure by stretching tiny quantum ripples to enormous size These ripples in density then become the seeds for all structures

31. How can microwave temperature be nearly identical on opposite sides of the sky?

32. Regions now on opposite sides of the sky were close together before inflation pushed them far apart

33. Inflation solves the horizon problem They are in equilibrium because they were in contact to start.

34. Overall geometry of the universe is closely related to total density of matter & energy Density = Critical Density > Critical Density < Critical

35. Inflation of universe flattens overall geometry like the inflation of a balloon, causing overall density of matter plus energy to be very close to critical density

36. Inflation solves the flatness problem A curved universe of large radius can not be distinguished from a flat universe. The universe appears flat because it is precisely flat.

37. How can we test the idea of inflation?

38. Patterns of structure observed by WMAP show us the “seeds” of universe

39. Observed patterns of structure in universe agree (so far) with the “seeds” that inflation would produce

40. 0 Fluctuations in the Cosmic Microwave Background Angular size of the CMB fluctuations allows us to probe the geometry of space-time! CMB fluctuations have a characteristic size of 1 degree.

41. 0 Analysis of the Cosmic Background Fluctuations Analyze frequency of occurrence of fluctuations on a particular angular scale Universe has a flat geometry

42. BUT a flat universe means total density is exactly critical. Result. Most of matter is dark matter. But most of cosmic density is not even matter. “The best match to data is a critical-density universe comprising 27% matter (4% baryonic,23% dark) and 73% dark energy.

43. Inferred from CMB • Overall geometry is flat • Total mass+energy has critical density • Ordinary matter ~ 4.4% of total • Total matter is ~ 27% of total • Dark matter is ~ 23% of total • Dark energy is ~ 73% of total • Age of 13.7 billion years In excellent agreement with observations of present-day universe and models involving inflation and WIMPs!

44. Why is the darkness of the night sky evidence for the Big Bang?

45. Olbers’ Paradox If universe were 1) infinite 2) unchanging 3) everywhere the same Then, stars would cover the night sky

46. Olbers’ Paradox If universe were 1) infinite 2) unchanging 3) everywhere the same Then, stars would cover the night sky

47. Night sky is dark because the universe changes with time As we look out in space, we can look back to a time when there were no stars

48. Olber’s Paradox Now if also infinite in spatial extension and infinite in lifetime. Olber’s Paradox isn’t a paradox or Olber’s. Thomas Digges, 1576 Kepler,1610; Halley,1721 Solution by Edgar Allan Poe 1848. The universe isn’t infinitely old.

49. Night sky is dark because the universe changes with time As we look out in space, we can look back to a time when there were no stars