Astronomia con neutrini di altissima energia.
Prof. Antonio Capone
Dottorato in Fisica, XXXVI ciclo (20 ore)
Si potrà seguire le lezioni, in modalità “telematica” tramite “Google Meet”, collegandosi al sito:
il mercoledì e venerdì dalle 10:00 alle 12:00
Programma del corso (file pdf)
Lezioni 1, 2: 28 aprile 2021 (slides utilizzate a lezione)
Description
of the course program and of the bibliography.
Primary Cosmic Rays (C.R.) intensity, energy spectrum and
composition. A power law can describe
the C.R. energy spectrum. Energy density
in C.R., in the Microwave Cosmic Background Radiation (MCBR), in the Galactic
Magnetic field. C.R. composition:
relative abundance of elements in the Earth (Solar System) and on the C.R.. The Leaky Box
Model and the spectral index of CR at Earth.
Lezioni 3, 4: 30 aprile 2021 (slides utilizzate a lezione)
Measurement
of the C.R. electromagnetic component:
primary photons and electrons: how to detect photons and electrons? Features, and experimental resolutions, of
the devices used in the detectors in space: measurements of charge, mass,
moment, energy, direction. Detection of primary cosmic rays with E <100 GeV.
Main characteristics of apparatuses on atmospheric balloons and on space, main
results.
Lezioni 5, 6: 5 maggio 2021 (slides utilizzate a lezione)
Measurement
of the C.R. electromagnetic component:
primary photons and electrons: how to detect them ? Detection of primary cosmic rays with E <
few 100 GeV. FERMI: the detector and the
obtained results. The Alpha Magnetic Spectrometer (AMS) detector on the
International Space Station: experimental capabilities, resolutions, results
obtained for: fraction e+/(e+ +
e-) and antiproton/proton ratio.
Indirect detection of photons with 50 GeV < Egamma
< 100 TeV.
Characteristics of Extensive Atmospheric Showers (EAS), measurable
quantities (energy, nature and direction of the primary, Xmax,
etc.) with detectors "at ground". Detection of EAS: detection of the
Cherenkov and "fluorescence" radiations. Cherenkov Telescopes, basic
working principle and characteristics: "effective area", angular and
energy resolutions, threshold in energy, sensitivity. "Cherenkov Imaging”
telescopes: the mono and stereo images of the EAS. Detection of VHE gamma
induced events: the background due to charged C.R. events, the signal-background separation. HEGRA, MAGIC, HESS, Veritas: detectors and
main results.
Lezioni 7, 8: 7 maggio
2021 (slides utilizzate
a lezione)
Indirect
detection of photons with 50 GeV < Eg < 100 TeV. Detection of VHE g induced EAS with Imaging Air
Cherenkov Telescopes: main results.
“Leptonic” and “Hadronic” sources of high energy photons: the Inverse
Compton process. Long term Measurement
of EAS at high quote over sea level over (the ARGO and Milagro
experiments). Ground based detectors:
detection at ground of extensive Air Showers: nature, direction and energy of
the primary C.R. The KASKADE
experiment. Detection of U.H.E. Cosmic
Rays (E>> 100 PeV) (AGASA, …).
Lezioni 9, 10: 12 maggio 2021 (slides utilizzate a lezione)
Detection
at ground of extensive Air Showers: nature, direction and energy of the primary
C.R. The KASKADE experiment. Detection of U.H.E. Cosmic Rays (E>>
100 PeV) (AGASA, …).
Detection of charged C.R. with energy > 1017 eV. The GZK expected cut-off. Feature of UHE Cosmic Rays spectrum for
E>1018 eV. Measurements
with hybrid detectors (HIRES, AUGER, Telescope Array). Spectrum and composition
of C.R. with E > 1018 eV.
The "chemical composition" of UHE C.R. as measured by hybrid
detectors at ground. Measurement of the
CR anisotropy. The role of the radio
detection technique in the HiRes and AUGER hybrid
detectors.
Lezioni 11, 12: 14 maggio 2021 (slides utilizzate a lezione)
Measurement
of astrophysical neutrinos, 1st generation detectors. Neutrinos,
very interesting particle, only weakly interacting. The first detectors for rare phenomena
(searches for proton decay, atmospheric neutrinos, …) under mountains and/or in
deep mines (Frejus, Kolar Mine, …). The second generation
detectors: Cherenkov detectors: Kamiokande, IMB;
tracking detectors: MACRO, …
Lezioni 13, 14: 19 maggio 2021 (slides utilizzate a lezione)
The third
generation (BAIKAL, AMANDA, ANTARES, IceCube,
KM3NeT…): physics goals, detection technique, properties of the Cherenkov
medium (water, ice), tracks and event reconstruction.
Lezioni 15, 16: 21 maggio 2021 (slides utilizzate a lezione)
How to
dimension a High Energy Astrophysical Neutrino Telescope (like BAIKAL, AMANDA,
ANTARES, IceCube, KM3NeT…).
Evaluation
of neutrino fluxes adopting the “hadronic model” for known point-like high
energy gamma sources. First results
Lezioni 17, 18: 26 maggio 2021 (slides utilizzate a lezione)
First
results from High Energy Astrophysical Neutrino Telescope (like BAIKAL, AMANDA,
ANTARES, IceCube, KM3NeT…). Measured cosmic diffuse neutrino fluxes:
comparison with diffuse gamma fluxes (by Fermi). Examples of multimessengers
searches (GRBs, Pulsars, mQuasars, Gravitational
waves, …). A possible point-like
neutrino source identified by multimessenger search.
Lezioni 19, 20: 28 maggio 2021 (slides utilizzate a lezione)
First
results from High Energy Astrophysical Neutrino Telescope (like BAIKAL, AMANDA,
ANTARES, IceCube, KM3NeT…). Multimessenger
searches: the GW-neutrino connection.
Other
physics items of study for Neutrino Telescopes: neutrino oscillations, neutrino
mass hyerarchy, indirect search for Dark Matter, ….
New techniques for larger detectors for higher energies (acoustic detectors, radio detectors)