  Predicted rates for solar neutrino experiments that are obtained with a
modified stellar evolution code originally developed to study the advanced
stages of stellar evolution are shown to be in agreement with other
recently-calculated precise solar models to about 2% (0.2 SNU for the chlorine
experiment). Different scenarios for pre-main sequence evolution are explored
and are found to change the predicted rates for solar neutrino experiments by
less than or of order 1%. The influence of the depth of the solar convective
zone on the predicted solar neutrino fluxes is established by direct
calculation. It is shown that a change in the calculated depth of the
convective zone that is five times larger than the quoted helioseismological
measurement uncertainty determined by Christensen-Dalsgaard, Gough, & Thompson
causes a change in the predicted $^8$B neutrino flux of less than 7% and a
change in the $^7$Be neutrino flux of less than 4%. Additionally, it is shown
that the radiative opacities near the depth of the convective zone cannot
differ from the standard OPAL values by more than about 12% without causing the
calculated and measured depths of the convective zone to differ by more than
five times the helioseismological measurement uncertainty.
