rule out) the QD spectrum, while a measured value of ${\mbox{$\left|  < \! m  \! > \right| \ $}}\!\! \gtap 0.03$ eV would rule out the NH spectrum [@PPSNO2bb]. Given and , the indicated upper limit on $\Sigma$ could be used to derive a rather stringent upper limit on $m_1$: using $\Sigma < 0.15~(0.12)$ eV and the current best fit values of ${\mbox{$ \Delta  m^2_{\odot}$}}\cong 5.0\times 10^{-5}~{\rm eV^2}$ and ${\mbox{$\Delta  m^2_{\mathrm{atm}}$}}\cong 3.0\times 10^{-3}~{\rm eV^2}$, we get in the case of IH spectrum: $m_1 < 0.03~(0.01)$ eV. An upper limit on $m_1$ of the order of (0.010 – 0.025) eV might be of crucial importance for establishing CP-violation due to the Majorana CP-violating phases [@BPP1; @PPW; @WR0302].

The analysis of the solar neutrino data [@SNO2; @SNO3; @SNO1; @SKsol; @Cl98], including the latest SNO results, in terms of the hypothesis of $\nu_e \rightarrow \nu_{\mu (\tau)}$ oscillations/transitions of the solar $\nu_e$ shows [@SNO2] (see also, e.g., [@BargerSNO2; @FogliSNO2]) that the data favor the LMA MSW solution with ${\mbox{$ \Delta  m^2_{\odot}$}}> 0$ and $\tan^2\theta_{\odot} < 1$. The LOW solution of the solar neutrino problem with transitions into active neutrinos is only allowed at approximately 99.73% C.L. [@SNO2]; there do not exist other solutions at 