Neutrino oscillation workshop 2000: conference summary

Abstract

The NOW2000 Workshop summarized the present status and future possibilities for all aspects of neutrino physics and astrophysics. Neutrino oscillation physics has truly come of age in the last few years. It is now data driven (analogous to cosmology and much of high energy physics in general). Experimental techniques and the theoretical interpretation have developed dramatically. An example of the latter includes the more realistic analysis of neutrino oscillations in the framework of 3 or more mass eigenstates. The phenomenological emphasis has shifted from degenerate to hierarchical neutrino spectra.

Neutrinos in cosmology

“…For example, the number density of deuterium is determined in equilibrium by the equality of chemical potentials, µ d = µ p + µ n . From that and the expression (30) we obtain: …”

“…For reviews on physics of (possibly massive) neutrinos see e.g. the papers [24]- [30]. Direct observational bounds on neutrino masses, found kinematically, are: m νe < 2.8 − 2.5 eV [31,32], 10 eV (other groups, see [10]) ,…”

Neutrino Masses in Supersymmetric Models with R-Symmetry

“…The simplest supersymmetric model to explain the masses of the left-handed neutrinos is known as the minimal supersymmetric standard model with third generation righthanded neutrinos (MSSMRH). The particle content of this model is the same as MSSM with the addition of the right-handed neutrinos Ni ∼ (1, 0) (see, e.g., [4,[68][69][70]). The superpotential of the MSSMRH is given by…”

Effects of Heavy Majorana Neutrinos at Lepton-Proton Colliders

“…In theories extending the Standard Model the seesaw mechanism is often used to provide a natural generation of small neutrino masses (for a review, see, e.g., [5,6]). Unlike the usual way of Dirac mass generation through weak SU(2)breaking, this mechanism doesn't need extremely small Yukawa couplings ( < ∼ 10 −12 ).…”