The Universe: What We Know and What we Don t. Fundamental Physics Cosmology Elementary Particle Physics

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1 The Universe: What We Know and What we Don t Fundamental Physics Cosmology Elementary Particle Physics 1

2 Cosmology Study of the universe at the largest scale How big is the universe? Where What Are did the universe come from? is the fate of the universe? there other universes? How many? What is dark matter? What is dark energy? 2

3 Elementary Particle Physics Study of the small scale structure of the universe What are the basic building blocks? How do they interact with one another? Is there a smallest amount of space and time? Is there a theory of everything?

4 Particle-Wave Duality Energy inversely proportional to wavelength E / 1 lower energy higher energy 4

5 Study of small distances requires high energy probes Large Hadron Collider Energy scale 10 3 GeV Distance scale m Temperature K 5

6 Big Bang 14 billion years ago the universe was much denser and hotter than today Has been expanding and cooling ever since To know the state of the universe at earlier and earlier times, need to know physics at higher and higher energy scales (smaller and smaller distances) K s after Big Bang 6

7 What we Know Physics down to a distance scale of m Physics down to a time of s after the Big Bang 7

8 How big is the universe? We don t know At least about 100 times larger than the visible universe Could be infinite 8

9 Steady State Universe Pre 20th century Stars fixed points in space Universe unchanging 9

10 General Relativity Eistein 1915 Gravity due to curvature of space-time 10

11 Friedman Equation Alexander Friedman 1922 Applied general relativity to the whole universe v r 2 energy density What is energy density due to? E = mc 2 about one hydrogen atom per cubic meter 1GeV/m 3 11

12 Cosmological Constant fudge factor v 2 ar = 8 G 3 m Prevents the universe from expanding (or contracting) matter energy density 12

13 velocity Hubble Expansion Hubble 1927 The universe is expanding distance 13

14 An Expanding Universe original expanded by 5% each dot represents a galaxy in the Universe 14

15 An Expanding Universe velocity is proportional to distance: Hubble s Law! original 15

16 An Expanding Universe everyone sees the same relationship: Hubble s Law is universal! original 16

17 Cosmic Microwave Background Radiation Penzias and Wilson 1965 Remnant radiation (photons) left over from 380,000 years after the Big Bang Cooled from 3000 K to 2.7 K Why? 17

18 Something Wrong H 2 0 = v 2 ar = 8 G 3 m H 2 0 /H 2 0 = 8 G 3 m /H 2 0 = m m =

19 Curvature positive curvature negative curvature zero curvature (flat) K = Kc 2 R 2 /H2 0 19

20 Cosmology in = m + K Expansion dominated by negative curvature Relatively small R This is wrong Dark Matter Dark Energy 20

21 Dark Matter About 80% of the matter in the universe is dark 21

22 Evidence for Dark Matter (1) Rotational curve of galaxy 22

23 Evidence for Dark Matter (2) Gravitational lensing 23

24 Evidence for Dark Matter (3) Bullet Cluster 24

25 Evolution of the Universe different pasts and futures depend on gravity and the contents of the Universe 25

26 Riess, Perlmutter, Schmidt 1998 Dark Energy Type Ia supernova 26

27 Accelerated Expansion of Universe 27

28 Evolution of the Universe different pasts and futures depend on gravity and the contents of the Universe DENSITY DESTINY cosmic acceleration! 28

29 Cosmology in = m + dm + + K Dark Energy largest contribution to expansion Universe is nearly or completely flat How big is the universe? 29

30 Vacuum Energy Dark energy is the energy of vacuum It has a fixed energy density that doesn t change as the universe expands is constant 30

31 20 Billion Years from Now m = 8 G 3 m 1 a 3 dm = 8 G 3 dm 1 a 3 = 8 G 3 constant 1 = m + dm + + K Expansion completely dominated by Dark Energy 31

32 Exponential Expansion Far in the future dm = m =0 =1 v r 2 = 8 G 3 = v r = p v = dr dt = p r p r e t 32

33 The Future of the Universe a cosmological constant leads to exponential growth more precise measurements here are still needed to help answer these questions! why so small? why now? 33

34 How Far Back Can We See? 34

35 Hubble Deep Field 35

36 Evolution of the Universe 36

37 Abundance of Light Nuclei 37

38 What Happened Before Recombination s K limit of our knowledge of physics 10-6 s K protons and neutrons form 1 s K matter anti-matter annihilate 10 s K photon dominance (e + e- annihilation) 3 min 10 9 K nucleosynthesis 4 x 10 5 y 3000 K atoms form (CMB from this era) What happened before s? 38

39 Problems with Simple Big Bang Theory 1) Where are magnetic monopoles? 2) Why is the universe so flat? 3) Why are distant parts of the universe in thermal equilibrium? The horizon problem? 39

40 CMB 2.7 K microwave photons streaming to us from there recombination era 380,000 years after the Big Bang non-uniformities 1 part in

41 Inflation Around s universe increased in size by more than Doubling time s not exactly zero Current doubling time years What was driving the exponential expansion? Vacuum energy Cosmological constant 41

42 Planck Scale Planck s constant (quantum mechanics): ~ c G Speed of light (special relativity): Universal gravitation constant: m Pl = r ~c G =0.02 mg E Pl = m Pl c 2 = r ~c 5 G =1019 GeV l Pl = ~ m pl c = r ~c G =10 35 m t Pl = l Pl c = r G~ c 5 =10 43 s 42

43 Cosmological Constant Problem Natural value for : Planck energy in Planck cube GeV (10 35 m) 3 =10124 GeV/m 3 Measured value for : 1GeV/m 3 Off by 124 orders of magnitude!!! Biggest mistake in all of physics! science 43

44 Limit of Cosmological Constant Steven Weiberg 1987 Calculated the upper limit of cosmological constant that would allow for us to be here. Larger values would cause the universe to expand to quickly for galaxies, stars, planets, life to evolve. Calculated value in excellent agreement with the value measured in

45 Anthropic Principle The universe is the way it is because we are here Gives the appearance that the laws of physics are fine tuned for our existence. We live in a Goldilocks universe. One of a huge number of universes in which we couldn t exist 45

46 Multiverse 46

47 Multiverse Vacuum energy different in different universes 47

48 Outstanding Problems Why is the vacuum energy so small? What is the physics at m? What is the quantum gravity? Is there any new physics between m and m? Why are the parameters of the universe so finely tuned? Why is there an excess of matter over antimatter? Are space and time fundamental? 48

49 To Learn More Cornell Messenger Lectures Nima Arkani-Hamed Lenny Susskind 49

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