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

Moorean Absurdities and Iterated Beliefs

Published in Journal of Philosophical Research, 2007, 32, 144-168. https://doi.org/10.5840/jpr20073236</p

Why Do Solar Neutrino Experiments Below 1 Mev

I discuss why we need solar neutrino experiments below 1 MeV. I also express my prejudices about the desired number and types of such experiments, emphasizing the importance of p-p solar neutrino experimentsComment: To be published in the proceedings of the Second International Workshop on Low Energy Solar Neutrinos, University of Tokyo, Tokyo, Japan, December 4 and 5, 2000 (World Scientific

Neutrino Opacity I. Neutrino-Lepton Scattering

The contribution of neutrino-lepton scattering to the total neutrino opacity of matter is investigated; it is found that, contrary to previous beliefs, neutrino scattering dominates the neutrino opacity for many astrophysically important conditions. The rates for neutrino-electron scattering and antineutrino-electron scattering are given for a variety of conditions, including both degenerate and nondegenerate gases; the rates for some related reactions are also presented. Formulas are given for the mean scattering angle and the mean energy loss in neutrino and antineutrino scattering. Applications are made to the following problems: (a) the detection of solar neutrinos; (b) the escape of neutrinos from stars; (c) neutrino scattering in cosmology; and (d) energy deposition in supernova explosions

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