3. NYSS-AAPT meeting SUNY - Brockport October 1, 2005 steven.manly@rochester.edu http://www.pas.rochester.edu/~manly/ Much ado about nothing: the 30 minute guide to the universe The intimate relationship between the very big and the very small Cosmology …

4. Inquiring minds want to know... Yo! What holds it together?

6. Fermi National Accelerator Laboratory (near Chicago)

7. CDFMinos

8. Stanford Linear Accelerator Center

9. Event display from the SLD experiment at SLAC

11. What forces exist in nature? What is a force? How do forces change with energy or temperature? How has the universe evolved? How do they interact?

13. qqq Baryons - proton,neutron Mesons - pion, kaon qq

14. Mini-Ph.D. – Quantum Mechanics 101 Lesson 1: Size actually does matter.

15. Determine the postion and velocity of a car … no problem

16. Determine the postion and velocity of a small particle … no problem

17. Problem! Heisenberg uncertainty principle Cannot have perfect knowledge of both the position and velocity Heisenberg

18. Dear Steve, Party relatively hard! -Al The fundamental nature of forces: virtual particles  E  t  h Heisenberg E = mc 2 Einstein e-e-

19. e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq e+e-e+e-e+e-e+e-qq qq qq e+e-e+e-e+e-e+e- qq e+e-e+e-e+e-e+e- qq qq e+e-e+e-e+e-e+e- Much ado about NOTHING: Nothing is something Nothing has energy Nothing interacts with something -R. Kolb

20. qq qq qqq The essence of inertial mass at the quantum level (quantum field theory)

21. On to the very big … 1 Mpc= 1 Megaparsec = 3x10 22 m 1 light year = 9x10 15 m Light travels from NYC to San Francisco in 1/100 second …. and it travels 1 Mpc in 3 million years Telescopes are time machines

22. Edwin Hubble (1889-1953) discovers a surprise in 1929 Galaxies that are further away appear redder Apparent Doppler shiftDoppler shift -From webphysics.davidson.edu

24. Type Ia SNe from Riess, Press and Kirshner (1996) Welcome to the “expanding universe”!! extrapolate back in time find the age of the universe  13 billion years. Light travels from NYC to San Francisco in 1/100 second …. and it travels 1 Mpc in 3 million years

25. -MSSL astrophysics group

26. Cosmic Microwave Background Penzias and Wilson - 1964 Uniform and isotropic – in as far as they could measure

27. BANG! TIME

28. Very hot, dense primordial soup of fundamental particles

29. At 0.000001 second after bang, protons and neutrons form

30. At 3 minutes, light nuclei form

31. At ~300,000 years, t = 3000 degrees, atoms form and light streams freely

32. t=~13 billion years, Ben Affleck and Jennifer Lopez break up

33. Modern accelerators study processes at energies that existed VERY early in the universe Another form of time travel ! What were forces like at those temperatures? What types of particles existed?

34. How can the universe be so isotropic? How did the structure (galaxies, clusters of galaxies) arise?? Do we know about all of the fundamental particles that exist? Why 3 families? Why is the mass spectrum of fundamental particles as it is? Why is the universe matter instead of antimatter? Many, many missing pieces … Recent progress! But new puzzles… -R. Kolb

35. We seem to be missing most of the mass in the universe! -P. Cushman

36. Very exciting development in last decade Observed fluctuations in the CMB temp WMap data on the temperature fluctuations in the CMB why structure matters

37. Einstein’s field equations: the modern laws of Genesis -R. Kolb

39. time 12 billion years17 billion years100 billion years1000 billion years Million- billion years Today Sun burns out Hell freezes over Buffalo wins the Superbowl End of universe One possible future of the universe -R. Kolb

40. “Power spectrum” (size) of temperature fluctuations sensitive to different matter/energy components of the universe

41.  M +     B +  DM +   WMAP composition of the universe -P. Cushman ~1/20

42. The elusive neutrino e + target  e - + X e + target  e - + X  + target   - + X  + target   - + X  + target   - + X  + target   - + X Flavor eigenstates – relevant for weak interaction with other particles Mass eigenstates (3 or more) 3 2 1mass 4

43. The elusive neutrino Quantum mechanical mixing of states: |  > = Σ i U *  i | i > Weak flavor eigenstate Mass eigenstate Unitary leptonic mixing matrix Analogous to CKM matrix for quarks Neutrino with momentum p evolves with time: |  (t)> = Σ i U *  i | i >e -iE i (p)t/h Neutrino of definite flavor is a superposition of several mass eigenstates whose different masses cause them to propagate differently changing the mixture of the mass eigenstates, i.e. neutrino oscillations in vacuum

44. Solar neutrino puzzle Solar neutrinos (only e produced in core of sun) Homestake Mine, Davis et al. 100,000 Gal tetrachloroethylene 37 Cl  37 Ar  e (Homestake)/  e (theory) ~ 0.34+-0.06 Homestake only sensitive to high E tail of e flux Fisher, Kayser, McFarland, Ann. Rev. Nucl. Part. Sci. 49, (1999) 481.

45. Neutrinos physics in the last decade Sudbury Neutrino Observatory (SNO) 1000 metric tons of D 2 O in 12 m acrylic vessel

46. SNO:  e +   =5.44+-0.99x10 6 cm -2 s -1 Bahcall:  total ~ 5.05x10 6 cm -2 s -1 SNO:  e /(  total ) ~ 0.34 Neutrinos oscillate and have mass … solar puzzle solved!

47. Neutrinos physics in the last decade SuperKamiodande 50,000 tons of pure H 2 O

49. Atmospheric neutrinos Cosmic rays interact in atmosphere and produce e and  neutrinos

50. Accelerator neutrinos K2K experiment M.H. Ahn et al., PRL 90 (2003) 041801

51. Reactor neutrinos KamLAND experiment D. Eguchi et al., PRL 90 (2003) 021802

52. Evidence for a sterile neutrino? MiniBooNE results in late summer or early fall …

53. The future Long baseline Two detectors – one near, one far High statistics – challenge for accelerator and detector On and off axis Need to minimize systematic errors

54. Large Hadron Collider (LHC) Videos from ATLAS Collaboration website

55. SuperNova Acceleration Probe

56. Thanks to: Priscilla Cushman, CDMS, G-2, Univ. of Minnesota Rocky Kolb, Fermilab and University of Chicago Stanford Linear Accelerator Center CERN, European Center for Particle Physics Fermi National Accelerator Laboratory Brookhaven National Laboratory Davidson University webphysics project WMAP project Hubble Space Telescope project Ned Wright, UCLA MSSL astrophysics group Newton, Einstein, Heisenberg, Plank, etc. And whoever else I forgot to mention … We live in exciting times!