Variations of Core Luminosity and Solar Neutrino Fluxes
  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. 
Attila Grandpierre