Recent Work on Standard Solar Models

Recent results on standard solar models are reviewed. I shall summarize briefly three of the themes that I stressed at the Neutrino '92 Conference: 1) Different solar model codes give the same answers when the same input data are used; 2) Improved calculations of standard solar models include helium diffusion, the Livermore radiative opacity, the meteoritic iron abundance, and a variety of other corrections; and 3) There are a few basic rules that should be followed in using standard solar models. At the Neutrino '92 Conference, I reviewed in more detail the recent work on standard solar models by Marc Pinsonneault and myself. This work has by now appeared in print (Rev. Mod. Phys. 64, 885, 1992, hereafter Paper I, and ApJ Letters, 69, 717, 1992, Paper II). Therefore, there is no need for me to repeat the details here.Comment: 4 pages, Institute for Advanced Study number AST 92/5

What Do Solar Models Tell Us About Solar Neutrino Experiments?

If the published event rates of the chlorine and Kamiokande solar neutrino experiments are correct, then the energy spectrum of neutrinos produced by the decay of $^8$B in the sun must be different from the energy spectrum determined from laboratory nuclear physics measurements. This change in the energy spectrum requires physics beyond the standard electroweak model. In addition, the GALLEX and SAGE experiments, which currently have large statistical uncertainties, differ from the predictions of the standard solar model by $2 \sigma$ and $3 \sigma$, respectively.Comment: 4 pages (LaTeX file, figures not included

Solar Neutrinos: Where We Are, Where We Are Going

This talk answers a series of questions. Why study solar neutrinos? What does the combined standard model (solar plus electroweak) predict for solar neutrinos? Why are the calculations of neutrino fluxes robust? What are the three solar neutrino problems? What have we learned in the first thirty years of solar neutrino research? For the next decade, what are the most important solvable problems in the physics of solar neutrinos? What are the most important problems in the astrophysics of solar neutrinos?Comment: uuencoded Z-compressed postscript file; 36 pages with figures. To be published in the Astrophysical Journa

Solar Neutrinos: What Next?

I summarize the current state of solar neutrino research and then give my answer to the question: What should we do next?Comment: NNN99 Workshop, viewgraphs and related information at http://www.sns.ias.edu/~jn

Solar Neutrinos. I. Theoretical

The principal energy source for main-sequence stars like the sun is believed to be the fusion, in the deep interior of the star, of four protons to form an alpha particle. The fusion reactions are thought to be initiated by the sequence ^1H(p, e^(+)v)^2H(p,γ)^(3)He and terminated by the following sequences: (i) ^(3)He(^(3)He, 2p)^(4)He; (ii) ^(3)He(α,γ)^(7)Be(e^(-)v)^(7)Li(p,α)^(4)He; and (iii) ^(3)He(α,γ)^(7)Be(p,γ)^(8)B(e^(+)v)^(8)Be*(α)^(4)He. No direct evidence for the existence of nuclear reactions in the interiors of stars has yet been obtained because the mean free path for photons emitted in the center of a star is typically less than 10^(-10) of the radius of the star. Only neutrinos, with their extremely small interaction cross sections, can enable us to see into the interior of a star and thus verify directly the hypothesis of nuclear energy generation in stars

Solar Models: An Historical Overview

I summarize in four slides the 40 years of development of the standard solar model that is used to predict solar neutrino fluxes and then describe the current uncertainties in the predictions. I next dispel the misconception that the p-p neutrino flux is determined by the solar luminosity and present a related formula that gives, in terms of the p-p and 7Be neutrino fluxes, the ratio of the rates of the two primary ways of terminating the p-p fusion chain. I will also attempt to explain why it took so long, about three and a half decades, to reach a consensus view that new physics is being learned from solar neutrino experiments. Finally, I close with a personal confession.Comment: Invited talk, Neutrino 2002, Munich, May 2002 (corrected typographical errors