Primary Cosmic rays phenomenology. Propagation and interaction mechanism. Antiprotons and positrons : secondary production and possible sources.
Ultra High Energy cosmic rays : phenomenology and detectors.
UHE neutrinos and neutrino telescope.
M.S. Longair, ‘High Energy Astrophysics’, Cambridge University Press; D.H. Perkins, ‘Particle Astrophysics’, Oxford University Press.
Learning Objectives
Knowledge acquired:
Phenomenology of cosmic rays at every energy. Knowledge of experimental methods for cosmic rays.
Competence acquired :
Phenomenology of cosmic rays at every energy. Knowledge of experimental methods for cosmic rays.
Skills acquired
Calculation of expected fluxes. Determination of the main parameters involved in cosmic rays detectors design.
Teaching Methods
6 CFU
Lectures hours: 48
Further information
Office hours
S. Bottai: 15-17 Lun-Ven
P. Papini: 15-17 Lun Ven
Website: --
Type of Assessment
Oral test
Course program
MODULO I :
Phenomenology of cosmic rays, the method of flow measurement of cosmic rays, the definition and use of the geometric factor. Influence of the Earth's magnetic field and solar activity on cosmic rays measured on Earth. Nuclear composition of cosmic rays, comparison with the abundances and local transport equation of cosmic rays in the galaxy. Simplified model of propagation (leaky box model) and study of the characteristics of cosmic rays through the measurements of the relative abundances (through material composition at the source, spectral index, acceleration and re-acceleration, lifetime of cosmic rays). Flow of electrons in cosmic rays, electromagnetic emission and galactic halo. • Flow of antimatter (antiprotons, positrons and research antinuclei) and links with any primary sources. Energy balance of cosmic rays and the Fermi acceleration mechanism in relation to the physics of supernova.
MODULO II:
Ultra high energy cosmic rays. Phenomenology of atmospheric showers and detection techniques. Fluxes of cosmic rays with energy more than 1014 eV. Mechanism of Fermi energy and maximum reach. The problem of acceleration to energies above the knee and explanation of the shape of the spectrum of cosmic rays at the knee. The propagation of extragalactic particles and the GZK cutoff expected in the spectrum of cosmic rays of extreme energy. Discussion of possible extragalactic sources of cosmic rays of energy E> 1019 eV and the models for the interpretation of data. Astronomy in ultra-high energy neutrinos. Reasons astronomy in ultra high energy neutrinos. Calculation of cash flows and upper limits of diffuse neutrino fluxes peri extragalactic sources (WB limit and limit MPR). Detection of neutrinos of astrophysical high energy consumption: calculation of the frequency of events expected, size and type of detectors. Atmospheric neutrino phenomenology, detection and oscillation of neutrinos. Solar neutrinos: phenomenology, detection and oscillation of neutrinos.