ABSTRACT
A variety of evolutionary sequences of models for the solar interior has been computed, corresponding to variations in input data, to obtain some idea of the uncertainties involved in predicting a solar neutrino flux. It is concluded that the neutrino flux can be estimated to within a factor of 2, the primary uncertainty being the initial homogeneous solar composition; detailed results are given. With a preferred value of the heavy-element-to-hydrogen ratio Z/X = 0.028, the helium content necessary to fit a model to the observed solar luminosity is found to be Y = 0.27.
TABLE OF CONTENTS
part 1|76 pages
Standard Model Expectations
part II|98 pages
Solar Neutrino Experiments
chapter |10 pages
National Research Council of Canada division of atomic energy
chapter |14 pages
Solar neutrinos observed by GALLEX at Gran Sasso
chapter |2 pages
GALLEX results from the first 30 solar neutrino runs
part III|88 pages
Nuclear Fusion Reactions
part IV|110 pages
Physics Beyond the Standard Model
part V|62 pages
Helioseismology
part |6 pages
Introduction
part VI|22 pages
Transition from “Problem” to Opportunity”