Vito Antonelli

Neutrino mass parameters from Kamland, SNO, and other solar evidence

An updated analysis of all available neutrino oscillation evidence in reactor (Kamland, first 145 days of data) and solar experiments (SK day and night spectra, global rates from Homestake, SAGE, and GALLEX) including the SNOCC and NC data is presented. In the framework of two active neutrino oscillations we determine the allowed regions in neutrino parameter space; we obtain, from the Kamland spectral shape and global signal, the following antineutrino best solution parameters:

Resummation of thrust distributions in DIS

\ensuremath{\Delta}{m}_{\mathrm{kl}}^{2}=7.7\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}5}{\mathrm{eV}}^{2},{\mathrm{tan}}^{2}{\ensuremath{\theta}}_{\mathrm{kl}}=0.98.

Determination of Neutrino mixing parameters after SNO oscillation evidence

The overall effect of the measured observed ratio

Global analysis of Solar neutrino oscillation evidence including SNO and implications for Borexino

R\ensuremath{\sim}0.6

Solar neutrino experiments and Borexino perspectives

is that the large mixing angle (LMA) region remains the only one that is still favored. Combining Kamland and solar data and assuming CPT invariance, i.e., the same mass matrix for neutrinos and antineutrinos, we obtain the following antineutrino best solution parameters (LMAI solution):

KamLAND, solar antineutrinos and their magnetic moment

\ensuremath{\Delta}{m}^{2}=7.1\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}5}{\mathrm{eV}}^{2},{\mathrm{tan}}^{2}\ensuremath{\theta}=0.47.

Advancements in solar neutrino physics

A second solution (LMAII) appears for values

After SNO and before KamLAND: present and future of Solar and Reactor Neutrino Physics

\ensuremath{\Delta}{m}^{2}=1.5\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}4}{\mathrm{eV}}^{2},{\mathrm{tan}}^{2}\ensuremath{\theta}=0.48.

Tests of the Standard Model with Low–Energy Neutrino Beams

We determine additionally individual neutrino mixing parameters and their errors from fits to marginal likelihood distributions; the values are compatible with previous results. In both methods,

The resummed thrust distribution in DIS

{\ensuremath{\chi}}^{2}