Transcript Astroparticle physics 1. stellar astrophysics and solar neutrinos

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
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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