Neutrino Oscillations and Astroparticle Physics (5) John Carr Centre de Physique des Particules de Marseille (IN2P3/CNRS) Pisa, 10 May 2002 n High Energy Astronomy Multi-Messanger Astronomy Cosmic Rays Gamma Ray Astronomy Neutrino Astronomy ( References )
Multi-Messenger Astronomy Multi-Wavelength Photons Charged Cosmic Rays Neutrinos Gravity Waves
Neutrinos (MeV: sun, SN GeV: atmosphere PeV: CR accelerators) v GeV: atmosphere w Dark matter Monopole s Cosmic ray particles -> 10 20 ev Electromagnetic radiation -> 100 TeV u Axions Grav. waves (W. Hoffmann)
Thermal Radiation from Stars Flux watts/m 2 10 6 10 2 10-2 T=6000K T=10000K 10-6 10-12 10 3 10 5 10 7 10 9 10 11 10 13 10 15 frequency(mhz) Normal Stars surface temperature ~3000 to 30000K thermal radiation: radio ultra -violet non-thermal radiation: X-rays, gamma rays ( higher in energy more extreme is the source)
Multi-Wavelength Photons Radio Ondes radio Radio télescope de Bonn Infrared Infra-rouge Satellite COBE Visible Lumière visible light Télescope du Mont Palomar Rayons X X-ray Satellite INTEGRAL Rayons Gamma gamma Ray? Satellite CGRO
Production Mechanisms of Photons Hot plasma (surface of stars) Annihilation of matter/antimatter Bremsstrahlung / Synchrotron Radiation e e - interstellar matter e e + U magnetic field Inverse Compton Scattering High energy showers p e interstellar matter e π + π 0
Non-Photonic Astronomy Antares (Toulon) Gravitational Waves Virgo (Pisa) Neutrinos Auger (Argentina) High Energy Cosmic Rays
Acceleration Mechanism of Charged Particles Simulations indicate can get ~ 50% of energy of supernova explosion Cosmic Rays by ~1000 yrs Example of Supernova Remnants Energy in ejecta Energy in cosmic rays Energy in gas ( t 0 ~1000 years)
Production Mechanism of Neutrinos p accelerated in shock waves: non-relativistic supernova remnants relativistic quasars/microquasars p interact with interstellar matter and produce showers : p/a + p/γ π 0 + π ± +... µ e e
Types of Cosmic Ray Detectors Compton Gamma Ray Obs. 0.1-10GeV BATSE Satellites top of atmosphere EGRET Ground based telescopes looking at light produced in atmosphere KASCADE p,n 0.3-100PeV Whipple >1 TeV ground level Array of particle detectors on ground Arrays of particle detectors
Charged Cosmic Ray Energy Spectrum Satellite, ballons AMS γ satellite CCGO, GLAST Ground, Air Shower Arrays CASA - KASCADE - AGASA - AUGER γ telescopes Whipple-CAT-HEGRA-CELESTE H.E.S.S.-MAGIC-VERITAS ν telescopes AMANDA, ANTARES knee Space observed Shower ankle EUSO Why these features?
Features of Cosmic Ray Spectrum E 2 dn/de [cm -2 s -1 sr -1 ev] E 2.7 knee E 3.2 Ingredients of models: source dn/de E α + δ Source acceleration: Source cut-off Diffusion models propagation α = 2.0 to 2.2,.. E <10 18 Z R B ev kpc µg δ = 0.3 to 0.6 GZK cut-off on CMB γ E 7 10 19 ev isotropic Mass composition? ankle E 2.8 E [ ev/nucleus] Conventional Wisdom : Galactic SNR E < 3 10 18 ev E > 4 10 14 ev Extragalactic E > 3 10 18 ev exotic E > 7 10 19 ev Galactic losses
Cosmic Rays Spectrum: Knee and Ankle Flux E 2.7 Flux E 3
Explanations of knee (E~3.10 15 ev) Astronomy type explanations Galactic de-confinement Single dominant source Single SNR acceleration multiple SNR acceleration Particle Physics type explanations Absorption on massive neutrinos in galaxy Various interactions invoked to give threshold at E = 3 10 15 ev. eg. p + ν e n + e, with M(ν e ) = 0.1 ev p + ν µ + ν µ,, with M(ν µ ) = 100 ev ( not very convincing due to various problems: mass, rates) New interaction effects in atmosphere
Mass composition from shower depth
Mass composition at knee Average shower depth and ratio N µ / N e sensitive to primary mass (NB. Mass composition extracted is very sensitive to Monte Carlo simulation) Flux E 2.5 KASCADE <ln A> 3.5 2.5 1.5 0.5 Mean ln(a) KASCADE CASA-BLANCA 10 15 10 16 10 17 Energy ev KASCADE series of knees at different energies: p,he,..,c,..,fe. E(Knee) Z knee due to source confinement cut-off?
GZK cutoff HE cosmic rays Interaction with background γ ( infrared and 2.7K CMBR) p γ π N 100 Mpc 10 Mpc Sources uniform in universe HE gamma rays Mrk 501 120Mpc γ γ e + e Mrk 421 120Mpc
Explanations of Ankle/ E > 10 20 ev events Astronomy type explanations Bottom-Up : acceleration - pulsars in galaxy, - radio lobes of AGN (proximity a problem due to GZK, also should see source) Particle Physics type explanations Top-Down : decay of massive particles - GUT X particles with mass > 10 20 ev and long lifetimes - Topological defects - Neutrinos as messenger particle New Physics