  In a Dynamic Solar Model (DSM) the temperature dependences of the pp cycle
neutrinos will be different from the ones determined by solar model
calculations with the luminosity constraint. Instead of the usual neutrino
fluxes pp ~ T^{-1/2}, Be ~ T^8, B ~ T^{18}, we determined by the nuclear
reaction rates formulas pp ~ T^{4.2}, Be ~ T^{-1/2}, B ~ T^{13.5}, for $\tau <
10^2$ years. These latter relations have high significance at estimating the
uncertainties of the solar central temperatures without assuming the luminosity
constraint. Although the purely astrophysical solutions seem to be ruled out,
this is not the case for a model in which astrophysical effects are included
besides the neutrino oscillations. Therefore a combined, DSM+MSW model is
suggested to calculate the observed solar neutrino fluxes. The combined SSM+MSW
fits to the rates+spectra+D/N changes give a bad fit to the total rates,
indicating the need to include the astrophysical factors besides the MSW
effect. The DSM suggest that the core dynamics is induced by intermittent
events of dissipation of rotational energy in the solar core, in relation to
angular momentum dissipation arising from the relative motion of the Sun and
the mass center of the Solar System, and it shifts the allowed ranges of the
MSW parameters into a more acceptable region. The role of the astrophysical
factors in the solar neutrino problem is behind the fact why the ``smoking
guns'' of neutrino oscillations are not found yet.
