Solar Neutrinos The First Thirty Years [Paperback]

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.Frontiers in Physics -- Editors Foreword -- Preface to the 2002 Paperback Edition -- Standard Model Expectations -- Introduction -- Standard Model Expectations -- Solar Neutrinos. I. Theoretical* -- Calcium-37 -- New Delayed-Proton Emitters: Ti44, Ca37, AND Ar33 -- Neutrino Opacity I. Neutrino-Lepton Scattering* -- Absorption Of Solar Neutrinos In Deuterium* -- Solar Neutrinos* -- Prediction For Neutrino-Electron Cross-Sections In Weinbergs Model Of Weak Interactions -- Solar neutrino experiments -- Solar Neutrino Flux* -- Helium Content And Neutrino Fluxes In Solar Models* -- A Study Of Solar Evolution -- On the Problem of Detecting Solar Neutrinos -- Present Status of the Theoretical Predictions for the 36Cl Solar-Neutrino Experiment * -- Solar Neutrinos and the Solar Helium Abundance * -- Sensitivity of the Solar-Neutrino Fluxes * -- More Solar Models and Neutrino Fluxes * -- Standard solar models and the uncertainties in predicted capture rates of solar neutrinos -- Solar models, neutrino experiments, and helioseismology -- Our Sun. I. The Standard Model -- Standard solar models, with and without helium diffusion, and the solor neutrino problem -- On the depletion of lithium in the Sun -- Standard solar models with CESAM code -- Toward a Unified Classical model of the Sun: on the Sensitivity of Neutrinos and Helioseismology to the Microscopic Physics -- Solar neutrinos and nuclear reactionsl³'