1. Georges LeMaitre theorized The Big Bang in 1927 two years before
NOTES:
Proofs of the Hot Big Bang (of Georges LeMaitre):
1. The red shift of distant galaxies.
2. The cosmic microwave background. Penzias and Wilson 1976.
A black body curve at T = 2.7 K results from electrons combining with protons
to make hydrogen. Ultraviolet stretched to microwave
with the expanding universe. This has small lumps in different directions of
about 1 part in 10,000 indicating early inflation.
3. Nucleosynthesis–Burbidge, Fowler, and Hoyle in 1960 calculated
Big Bang made 75% He, 25% He–observed in unrecycled material.
Georges LeMaitre
theorized
The Big Bang in 1927
two years before
Hubble observed it.

2. Proofs of the Hot Big Bang: 1. The red shift of distant galaxies
Implies Hubble’s Law

3. Proofs of the Hot Big Bang:
2. The cosmic microwave background.
observed and identified by Penzias and Wilson in 1965.
Predicted by Cosmologist
George Gamov in 1948

4. A black body curve at T = 2.7 K results from electrons combining with protons
to make hydrogen. Ultraviolet stretched to microwave
with the expanding universe.

5. WMAP Satellite—observes the microwave
Background.
This has small lumps in temperature in
different directions of about 1 part in 10,000
indicating early inflation.

6. Proofs of the Hot Big Bang:
3. Nucleosynthesis–in 1960 Burbidge, Burbidge, Fowler, and Hoyle calculated Big Bang made 75% H, 25% He–observed in unrecycled material.

7. For about a second, the Big Bang was hotter than 10 million K,
and fused 25% of H into He.

8. The ‘primordial soup’
Was thus 75% H and 25%
He by mass.

9. –A funny energy in space
Post-1998 Cosmology
–A funny energy in space
At the present epoch the velocity of receding galaxies is given
by Hubble’s Law: v = Ho d , where Ho is the Hubble constant.
1. This holds only for galaxies at moderately low distances.

10. In actuality, the straight line of Hubble’s law curves gently
downward at greater distances as indicated by
supernova Ia measurements of explosions up to about
11 billion years ago (Perlmutter’s and Schmidt’s groups
--post 1998).
Saul Perlmutter, Berkeley
Brian Schmidt, Harvard (at first)

11. At first, it was East Coast vs West Coast!@*#!

13. a) The velocities are given by the redshifts of the galaxies they
are in.
b) The distances are given by standard peak luminosity of
supernovae Ia, which is always the same.

14. The data
implies the universe
is speeding up.

15. The universal expansion is accelerating. It will expand forever
in such a way that it implies:
a) The mass in the universe is not sufficient to turn the
expansion around, even with dark matter included,
If I throw my keys up, they slow down.
gravity normally decelerates!

16. b) There is a funny energy in space (usually called dark energy) driving the acceleration like a compressed sponge when released.

17. If Einstein’s General Theory holds, this energy
may be in the form of Einstein’s cosmological constant, Λ.
In 1917, he postulated that this constant outward force
was necessary in a static universe to keep the galaxies from
falling into each other.
The universe was not found to be expanding until 1929.

18. Dark energy may also be a time varying component of space
called quintessence--the fifth element. However, for now,
data closely matches the cosmological constant.

20. Cosmic History

21. 10-32 sec

22. 1 second
Big Freeze Out
                                                                                                                             
The First Atomic Nuclei

23. The decoupling era (recombination)
Decoupling of light and matter. 380,000 years ABB
(After Big Bang) D
The decoupling era (recombination)
H atoms can form, because light escapes.

25. Chapter 23 The Beginning of Time

26. 23.1 The Big Bang Our goals for learning
What were conditions like in the early universe?
What is the history of the universe according to the Big Bang theory?

27. What were conditions like in the early universe?

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

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

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

32. Planck Era
Before Planck time (~10-43 sec)
No theory of quantum gravity

33. Do forces unify at high temperatures?
Four known forces
in universe:
Strong Force
Electromagnetism
Weak Force
Gravity

34. Do forces unify at high temperatures?
Four known forces
in universe:
Strong Force
Electromagnetism
Weak Force
Gravity
Yes!
(Electroweak)

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

36. 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)

37. GUT Era
Lasts from Planck time (~10-43 sec) to end of GUT force (~10-38 sec)

38. Electroweak Era
Lasts from end of GUT force (~10-38 sec) to end of electroweak force (~10-10 sec)

39. Particle Era
Amounts of matter and antimatter nearly equal
(Roughly 1 extra proton for every 109 proton-antiproton pairs!)

40. Era of Nucleo-synthesis
Begins when matter annihilates remaining antimatter at
~ sec
Nuclei begin to fuse

41. Era of Nuclei
Helium nuclei form at age
~ 3 minutes
Universe has become too cool to blast helium apart

42. Era of Atoms
Atoms form at age ~ 380,000 years
Background radiation released

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

44. Primary Evidence
We have detected the leftover radiation from the Big Bang. CMB = Cosmic Microwave Background.
The Big Bang theory correctly predicts the abundance of helium and other light elements.

45. 23.2 Evidence for the Big Bang
Our goals for learning
How do we observe the radiation left over from the Big Bang?
How do the abundances of elements support the Big Bang theory?

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

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

48. Background radiation from Big Bang has been freely streaming across universe since atoms formed at temperature ~ 3,000 K: visible/IR. Electron + proton = Hydrogen plus light (UV)

49. Background has perfect thermal radiation spectrum at temperature 2
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

50. WMAP (Wilkenson Microwave Anisotropy Project) gives us detailed baby pictures of structure in the universe (380, 000 years after Big Bang)

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

52. Protons and neutrons combined to make long-lasting helium nuclei before universe was ~ 3 minutes old (> 10 mill. K)

53. Big Bang theory prediction: 75% H, 25% He (by mass)
(Burbidge, Burbidge, Fowler and Hoyle—primordial nucleosynthesis) Matches observations of early gasses.

54. Abundances of other light elements agree with Big Bang model having 4
Abundances of other light elements agree with Big Bang model having 4.4% normal matter – more evidence for WIMPS!

55. 23.3 Inflation Our goals for learning
What aspects of the universe were originally unexplained with the Big Bang theory?
How does inflation explain these features?
How can we test the idea of inflation?

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

57. 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?

58. 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!

59. 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

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

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

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

63. 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

64. How can we test the idea of inflation?

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

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

67. “Seeds” 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

68. “Seeds” 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!

69. 23.4 Observing the Big Bang for Yourself
Our goals for learning
Why is the darkness of the night sky evidence for the Big Bang?

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

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

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

73. 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

74. 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