Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...304..431r&link_type=abstract
Astronomy and Astrophysics, v.304, p.431
Astronomy and Astrophysics
Astrophysics
1
Stars: Interiors, Sun: Interior, Elementary Particles, Sun: Particle Emission
Scientific paper
The results from two solar model calculations using the "energy.for" energy generation and neutrino flux code (Bahcall & Pinsonneault 1992) are presented. The models of the present Sun were generated using the program described in the first three papers of this series and using only the helium abundance profile from the Bahcall & Ulrich (1988) (BU) standard model in the present model structure calculations. One model is a simulation of the BU model and yields a ^37^Cl solar neutrino counting rate of 7.0SNU (compared to 7.9SNU for the BU model) and a ^71^Ga neutrino experiment counting rate between 112 and 137SNU (compared to 132SNU for the BU model). The second model has a postulated small high-Z core (Rouse 1983) and yields a ^37^Cl neutrino experiment counting rate of 2.45SNU that is within one sigma of the Homestake Collaboration observed rate of (2.55+/-0.25)SNU (see Parke 1995). It yields a ^71^Ga neutrino experiment counting rate between 89 and 103SNU that is within one sigma of the GALLEX Collaboration neutrino experiment observed rate of (79+/-12)SNU (see Parke 1995). The theoretical ^8^B solar neutrino flux and the observed Kamiokande ^8^B flux (Hirata et al. 1989) are discussed regarding the puzzle of explaining both the chlorine 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 formation from pre-stellar nuclei (Krat 1952; Urey 1956; Huang 1957) is suggested.
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