Theoretical aspects of neutrino oscillations

Abstract

I review some aspects concerning the physics of neutrino mixing and oscillations. I discuss in some detail the physical neutrino oscillations parameter space in the case of two and three family mixing, and briefly describe the current knowledge of neutrino mixing parameters according to the present solar, atmospheric, and reactor neutrino data. I also briefly comment on the possibility of solving the LNSD anomaly together with the solar and atmospheric ones. I conclude by emphasising that that even though in five to ten years time a lot will be learnt from the next round of neutrino experiments, a great deal about neutrino masses and neutrino mixing will remain unknown.

Entrevista ao arquiteto Egas José Vieira

“…In the previous expression, P 2νe e (E) gives the survival probability of electron neutrinos in the two neutrino flavour model (θ 13 = 0), P γ computes the probability jumps coming from the non-adiabatic correction, and θ m = θ m (r s ) is the matter mixing angle [64]. θ m is evaluated in the neutrino production (source) region located at a distance r s from the Sun's centre [e.g., 65,66].…”