CALCULATION OF STELLAR STRUCTURE .4. RESULTS USING A DETAILED ENERGY GENERATION SUBROUTINE

The results from two solar model calculations using the energy.for ene rgy generation and neutrino flux code (Bahcall & Pinsonneault 1992) ar e presented. The models of the present Sun were generated using the pr ogram described in the first three papers of this series and using onl y the helium abundance profile from the Bahcall & Ulrich (1988) (BU) s tandard model in the present model structure calculations. One model i s a simulation of the BU model and yields a Cl-37 solar neutrino count ing rate of 7.0 SNU (compared to 7.9 SNU for the BU model) and a Ga-71 neutrino experiment counting rate between 112 and 137 SNU (compared t o 132 SNU for the BU model). The second model has a postulated small h igh-Z core (Rouse 1983) and yields a Cl-37 neutrino experiment countin g rate of 2.45 SNU that is within one sigma of the Homestake Collabora tion observed rate of (2.55 +/- 0.25) SNU (see Parke 1995). It yields a Ga-71 neutrino experiment counting rate between 89 and 103 SNU that is within one sigma of the GALLEX Collaboration neutrino experiment ob served rate of (79 +/- 12) SNU (see Parke 1995). The theoretical B-8 s olar neutrino flux and the observed Kamiokande B-8 flux (Hirata et al. 1989) are discussed regarding the puzzle of explaining both the chlor ine experiment results and the Kamiokande results. The modification of the energy.for code for use in the current Rouse program is described . Consistency of a high-Z core solar model with theories of star forma tion from pre-stellar nuclei (Krat 1952; Urey 1956; Huang 1957) is sug gested.