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Astroparticle physics Introduction and astrophysical information Alberto Carramiñana Instituto Nacional de Astrofísica, Óptica y Electrónica Tonantzintla, Puebla, México Xalapa, 2 August 2004 The composition of the Universe • Planets. • Stars: nuclear burning & degenerate corpses. • Gas, dust (magnetic fields (cosmic-rays)). • Galaxies: normal, active. • Cosmological background(s). • Protons, neutrons baryons. • Electrons, muons leptons. • Neutrinos. • Mesons hadrons quarks. Early Universe / Cosmic-rays / astrophysical neutrinos / non baryonic dark matter / dark energy Astroparticle physics • • • • • Astrophysics oriented course. Astrophysical information. Stellar physics (solar neutrinos). Interstellar medium (cosmic-rays). Supernovae and degenerate stars (cosmic-rays, neutrinos). • Beyond our galaxy (high energy cosmicrays, (relic neutrinos), dark matter). Astrophysical information carriers • Photons: radio waves to -rays. • Neutrinos: MeV to ZeV. • Gravitational waves: not today... • Elementary particles: cosmic-rays. Photons • Electromagnetic waves: solution to EM wave equations: – polarization vector – dispersion relation wavelength / frequency – Planck relation photon energy • Electromagnetic spectrum Electromagnetic spectrum Radio, mm, infrared space, infrared ground, optical ground and space, uv, X-ray space, -ray space and ground-based telescopes. Focusing telescopes • Radiation is focussed to a detector (radio to a few keV). High energy telescopes • Photoelectric effect • Compton telescopes. • Pair production telescopes. Neutrinos • Weak force interaction spin • Energy • Flavour: e, , . • Mass! Neutrino detectors • Chemical – Chlorine: – Gallium: • e-scattering Cerenkov: Kamiokande & Super-Kamiokande (water). • Charged and neutral current: Sudbury Neutrino Observatory (D2O) flavour sensitive. • Very high energy -cascades: Pierre Auger. Gravitational waves Not today! Cosmic-rays • Earth “bombarded” by highenergy particles: cosmicrays. • Charged particles do not conserve direction in the Galaxy. • Observed energies: below 108eV to 1020.5 eV. – low and intermediate energies (1015eV) from balloon or space. – high energy (above 1015eV) from ground. astro.uchicago.edu/~smoneil/background.html Cosmic-rays from space Composition Solar particles Solar modulation At Spacelab 2 Grunsfeld et al. 1988 Access: Advanced Cosmic-ray Composition Experiment for the Space Station hep.uchicago.edu/~swordy/access.html Cosmic-rays from ground • Particle cascades from incoming cosmic-ray. – Direct detection of secondary particles (e,) at ground level. – Atmospheric fluorescence emission. • Cerenkov emission very high energy -ray telescopes (> 100 GeV). http://www.bartol.udel.edu/~neutronm/catch/cr2.html