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: 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 Origin of Elements formed in: Big Bang Nucleo-synthesis Hot Stars Supernova Explosions Cosmic Ray Interactions Big Bang time after big bang temperature of universe 3000 K K y 100 s Neutral hydrogen forms universe transparent to light fossil photon radiation frozen T (K) ~ /t (s) Equilibrium n/p ends Nucleosynthesis begins nuclei atoms Particle Physics after Big Bang time since Big Bang 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 K (1 MeV) reactions cease ( m = 1.3 MeV) In equilibrium: Nucleosynthesis starts Deuterium necessary to start nucleosynthesis Helium formed from deuterium ( Difficult to continue because no stable mass 5, 8 nuclei) Nucleosynthesis development tritium deuterium helium-4 helium-3 (free neutrons decay) Be, Li low levels Element Production in Stars PP cycle : cold stars CNO cycle : hot stars 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 dark energy: 65% cold dark matter: 30% ordinary matter: 5% matter 1/3 dark energy 2/3 Composition of Universe Dark Matter Evidence : Need to hold together Galaxy Clusters Explain Galaxy Rotation velocities Astronomy object candidates : Brown Dwarfs (stars mass 100 Mpc 1,4 M ) End in Supernovae of type Ib, Ic et II Life of small star ( < 1,4 M ) 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 SuperNovae Remnants Vela Cas A Tycho Crab Cygnus Loop Soleil Tycho Crab Cas A Vela Kepler Cygnus SN1006 SN1054 (Crab) SN1680 (CasA) charged particles protons ions electrons neutral particles photons neutrinos at ground level :~ 1/sec/m 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 Particle Acceleration R 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) 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 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 Photons absorbed on dust and radiation Protons deviated by magnetic fields Neutrinos direct Multi-Messenger Astronomy 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: