Astroparticle physics Introduction and astrophysical information

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Astroparticle physicsIntroduction
andastrophysical information

• Alberto Carramiñana
• Instituto Nacional de Astrofísica, Óptica y
  Electrónica
• Tonantzintla, Puebla, México
• Xalapa, 2 August 2004

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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
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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 cosmic-rays,
  (relic neutrinos), dark matter).

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Astrophysical information carriers

• Photons radio waves to ?-rays.
• Neutrinos MeV to ZeV.
• Gravitational waves not today...
• Elementary particles cosmic-rays.

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Photons

• Electromagnetic waves solution to EM wave
  equations
• polarization vector
• dispersion relation ? wavelength / frequency
• Planck relation ? photon energy
• Electromagnetic spectrum

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Electromagnetic spectrum
Radio, mm, infrared space, infrared ground,
optical ground and space, uv, X-ray space, ?-ray
space and ground-based telescopes.
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Focusing telescopes

• Radiation is focussed to a detector (radio to a
  few keV).

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High energy telescopes

• Photoelectric effect
• Compton telescopes.
• Pair production telescopes.

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Neutrinos

• Weak force interaction ? spin
• Energy
• Flavour e, ?, ?.
• Mass!

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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.

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Gravitational waves

• Not today!

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Cosmic-rays

• Earth bombarded by high-energy particles
  cosmic-rays.
• 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
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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
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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 (gt 100 GeV).

http//www.bartol.udel.edu/neutronm/catch/cr2.htm
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