![]() The previous work pushed me to assess the possibility to detect prompt neutrinos as well as to investigate their role in cosmic neutrino analyses. The potential of atmospheric neutrinos as a proxy for cosmic-ray physics was discussed. Unfortunately, the uncertainties on the data only allow to slightly favour the KASCADE-Grande knee. Two atmospheric neutrino fluxes have been computed using such primary models as input, and have been compared to the available data to discriminate the knee position. Two primary cosmic-ray flux models have been defined by fitting the data by ARGO-YBJ and KASCADE-Grande, which measure the knee of p+He at, respectively, ~700 TeV and ~5 PeV. ![]() The resulting updated luminosity constraint is more general, accurate, and powerful at connecting pp and CNO neutrinos, which are of paramount interest for solar neutrino detectors and for solving the solar metallicity problem.Ītmospheric neutrinos have been studied both as a product of cosmic rays and as a background to the cosmic neutrino analyses. We reformulated the derivation of the luminosity constraint in a simpler and clearer way, and generalised it by including the contribution of other accumulating elements and of the variation of the solar gravitational potential. Such relation is based on few assumptions, among which the stationarity of the Sun, and that 4He is the only accumulating nuclear specie. In the context of solar neutrinos, the main contribution of my work concerns the luminosity constraint, a strict relation between the solar luminosity in photons and in neutrinos. These open problems regard the fundamental properties of neutrinos, as well as their role as an astrophysical messenger, on which we focussed our efforts. ![]() In my thesis I addressed a selection of the open problems in neutrino astrophysics. Significant influence on the event rates. Mass hierarchy, and show that uncertainties in the Earth's density can have a We use recent results from the detector collaboration andīuild on previous work which considered the sensitivity of the detector to the Predict the flux of muon-type neutrino events in the Deep Core extension to the Various Earth density models are described, and these models are then used to Survival probabilities of atmospheric muon neutrinos. We give a detailed review of the resonant matter effects that determine the In the final spectra are also found to occur when the neutrino background density Intermediate dynamics can be very strongly altered. General the final neutrino spectra emerging from the inner supernova regionsįluctuations in the backgrounds in our model, while the ![]() In the neutrino density can have on the oscillation behaviour. We study the motion of twoĮxample supernova neutrino spectra and examine the differences in the dynamicsįlavour evolution that results from adding turbulent Supernova backgrounds are presented and discussed. The results of numerical simulations of supernova oscillations in turbulent Seen in numerical studies are summarized. Supernova neutrino spectra and explanations of the spectral swapping behaviour This theory is applied to the case of continuous Pendulum analogy and describe the motion that results from self-induced We discuss collective neutrino systems using the gyroscopic ![]() A survey of the theory of neutrino oscillations in dense matter and neutrinoīackgrounds is presented. ![]()
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