1. Astroparticle Physics (1)  Introduction - Origin of Elements - Big Bang - Dark Matter - Cosmic Microwave Background Radiation - Cosmic Particle Accelerators - Cosmic Rays - Multi-Messenger Astronomy  Dark Matter Searches  High Energy Astronomy John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) CERN Summer Students Lectures, 22 July 2002 following lectures:

2. What is Astroparticle physics ? Particle Physics Astronomy Astrophysics and cosmology PARTICLE ASTROPHYSICS Particle Astrophysics/Nuclear Astrophysics Use input from Particle Physics to explain universe: Big Bang, Dark Matter, …. Use techniques from Particle Physics to advance Astronomy Use particles from outer space to advance particle physics

3. Origin of Elements formed in: Big Bang Nucleo-synthesis Hot Stars Supernova Explosions Cosmic Ray Interactions

4. Big Bang time after big bang temperature of universe 3000 K 10 10 K 3 10 5 y 100 s Neutral hydrogen forms universe transparent to light fossil photon radiation frozen T (K) ~ 10 10 /t ½ (s) Equilibrium n/p ends Nucleosynthesis begins nuclei atoms

5. Particle Physics after Big Bang time since Big Bang

6. First Minute after Big Bang Production rates = Annihilation rates  equilibrium of particles and no nuclei formed N (neutron) N (proton) = e  m/kT When temperature falls below 10 10 K (1 MeV) reactions cease (  m = 1.3 MeV) In equilibrium:

7. Nucleosynthesis starts Deuterium necessary to start nucleosynthesis Helium formed from deuterium ( Difficult to continue because no stable mass 5, 8 nuclei)

8. Nucleosynthesis development tritium deuterium helium-4 helium-3 (free neutrons decay) Be, Li low levels

9. Element Production in Stars PP cycle : cold stars CNO cycle : hot stars

10. Heavy Element Production in Supernova neutrons protons CNO cycle : hot starsrp process : supernova explosions Nuclear cross-sections not well known: need accelerator measurements stable nuclei rp process

11. dark energy: 65% cold dark matter: 30% ordinary matter: 5% matter 1/3 dark energy 2/3 Composition of Universe

12. Dark Matter Evidence : Need to hold together Galaxy Clusters Explain Galaxy Rotation velocities Astronomy object candidates : Brown Dwarfs (stars mass <0.1 M sun no fusion) - some but not enough White Dwarfs ( final states of small stars) - some but not enough Neutron Stars/Black Holes ( final states of big stars.) - expected to be rarer than white dwarfs Gas clouds -  75% visible matter in the universe, but observable Particle Physics candidates: Neutrinos - Evidence for mass from oscillation, not enough Axions - Difficult to detect …. Neutralinos - Particle Physicist Favourite !

13. Nucleosynthesis rate gives baryon density Measured abundance of He, D  Fraction of baryons < 5% Must have non-baryonic particle dark matter  = N b /N , baryon number fraction

14. And number of Neutrino Families Predictions from Big Bang Nucleosynthesis Measurements from LEP of width of Z resonance N = 3

15. End of Opaque Universe After recombination universe becomes transparent. See photons as Cosmic Microwave Background Radiation redshifted by 1000 to 2.7K

16. Penzas and Wilson Discovery of Cosmic Microwave Background

17. Cosmic Microwave Background Radiation Microwaves: 31.5 GHz 53 GHz 90 GHz + 100  KTemperature variations: – 100  K

18. Ultra High Energy from Cosmic Rays 1 10 2 10 4 10 6 10 8 10 10 10 12 Energy GeV 1 10 2 10 4 10 6 10 8 10 10 10 12 Energy GeV cross-section (mb) particle flux /m 2 /st/sec/GeV From laboratory acceleratorsFrom cosmic accelerators FNAL LHC Flux of cosmic ray particles arriving on Earth Particle cross-sections measured in accelerator experiments Ultra High Energy Particles arrive from space for free: make use of them Colliders Fixed target beamlines

19. Astronomy Scales 4.5 pc450 kpc150 Mpc Nearest StarsNearest GalaxiesNearest Galaxy Clusters 1 pc= 3 light years

20. Expansion of Universe Edwin Hubble Mt. Wilson 100 Inch Telescope Velocity of galaxy proportional to distance: v= H r H ~ 70 km/sec / Mpc

21. Milky Way Galaxy Magnetic field  few  G

22. QUASAR MICROQUASAR 10 8 - 10 9    10 2 - 10 5   distant galaxies local galaxy >100 Mpc <10kpc QUASARS & MICROQUASARS

24. Supernovae and Supernova Remnants Implosion of core of red giant Expansion of matter shock wave  0.5 c Explosion of star Supernova Supernova Remnant

25. SuperNovae observed in our galaxy Date Remnant Observed 352 BC Chinese 185 AD SNR 185 Chinese 369 ? Chinese 386 Chinese 393 SNR 393 Chinese 437 ? 827 ? 902 ? 1006 SN1006 Arabic,... 1054 Crab Chinese,.. 1181 3C58 Chinese,.. 1203 ? 1230 ? 1572 Tycho Tycho Brahe 1604 Kepler Johannes Kepler 1667 Cas A not seen ?

26. Life of big star ( > 1,4 M  ) End in Supernovae of type Ib, Ic et II

27. Life of small star ( < 1,4 M  )

28. Type Ia supernovae SNe Ia sont which accrete matter from neighbour star in binary system When the mass achieves the Chandrasekhar mass (~ 1.4 M  ) star collapses to neutron star in supernova explosion.  Always same mass so always same luminosity Standard Candle for measuring universe expansion Flow of matter Red Giant White Dwarf

29. SuperNovae Remnants Vela Cas A Tycho Crab Cygnus Loop Soleil Tycho Crab Cas A Vela Kepler Cygnus SN1006 SN1054 (Crab) SN1680 (CasA)

30. charged particles protons ions electrons neutral particles photons neutrinos at ground level :~ 1/sec/m² Primary cosmic rays produce showers in high atmosphere Primary: p 80 %,  9 %, n 8 % e 2 %, heavy nuclei 1 %  0.1 %, 0.1 % ? Secondary at ground level: 68 %  30 % p, n,... 2 % 100 years after discovery by Hess origin still uncertain Cosmic Rays

31. Particle Acceleration R  10 15 km, B  10  10 T  E  1000 TeV R  10 km, B  10 T  E  10 TeV Large Hadron Collider Tycho SuperNova Remnant E  BR ( NB. E  Z  Pb/Fe higher energy)

32. Energy of particules accelerated Diameter of collider Cyclotron Berkeley 1937 Saturne, Saclay, 1964 Particle Physics  Particle Astrophysics LHC CERN, Geneva, 2005 Terrestrial AcceleratorsCosmic Accelerators Active Galactic Nuclei Binary Systems SuperNova Remnant

33. Cosmic Accelerators: ( Hillas Plot) E  Z B L  Z: Charge of particle B: Magnetic field L: Size of object  : Lorentz factor of shock wave L B GRB (artist) Crab Pulsar Vela SNR 3C47 M87, AGN Centurus A M87

34. Photons absorbed on dust and radiation Protons deviated by magnetic fields Neutrinos direct Multi-Messenger Astronomy

35. neutrino Evidence for Dark Matter - Cosmology - Strong Gravitational Lensing - Galaxy Dynamics Baryonic Dark Matter Searches - MAssive Compact Halo Object Searches - White Dwarfs Cold Dark Matter Searches - Direct - Indirect Dark Matter Searches tomorrow: