  The Solar Neutrino Problems (SNP's) are analysed within the Standard Solar
Model (BP2000) supplemented by the reduction of the solar neutrino fluxes
through the decrease of the solar core temperature. The former can be realized
through the enhancement of the astrophysical factor for solar proton burning.
The enhancement, the upper bound of which is restricted by the
helioseismological data, goes dynamically due to low-energy nuclear forces
described at the quantum field theoretic level. The agreement of the reduced
solar neutrino fluxes with the experimental data is obtained within the
scenario of vacuum two-flavour neutrino oscillations. We show that by fitting
the mean value of the solar neutrino flux measured by HOMESTAKE Collaboration
we predict the high energy solar neutrino flux measured by SNO Collaboration
Phi(SNO(Boron))_th = 1.84 X 10^6 cm^(-2) s^(-1) in good agreement with the
experimental value Phi(SNO(Boron))_exp = 1.75(0.14) X 10^6 cm^(-2) s^(-1)
obtained via the measurement of the rate of reaction nu_e + D -> p + p +
electron produced by boron solar neutrinos. The theoretical flux for low-energy
neutrino flux measured by GALLIUM (GALLEX, GNO and SAGE) Collaborations
S(Ga)_th = 65 SNU agrees with the experimental data averaged over experiments
S(Ga)_exp = 75.6(4.8) SNU.
