Abstract
We present an update of the determination of the solar neutrino fluxes from a global analysis of the solar and terrestrial neutrino data in the framework of three-neutrino mixing. Using a Bayesian analysis we reconstruct the posterior probability distribution function for the eight normalization parameters of the solar neutrino fluxes plus the relevant masses and mixing, with and without imposing the luminosity constraint. We then use these results to compare the description provided by different Standard Solar Models. Our results show that, at present, both models with low and high metallicity can describe the data with equivalent statistical agreement. We also argue that even with the present experimental precision the solar neutrino data have the potential to improve the accuracy of the solar model predictions.
Highlights
The produced neutrinos, given their weak interactions, can exit the Sun practically unaffected, and enable us to see into the solar interior and verify directly our understanding of the Sun [11]
We present an update of the determination of the solar neutrino fluxes from a global analysis of the solar and terrestrial neutrino data in the framework of three-neutrino mixing
We argue that even with the present experimental precision the solar neutrino data have the potential to improve the accuracy of the solar model predictions
Summary
In the analysis of solar neutrino experiments we include the total rates from the radiochemical experiments Chlorine [26], Gallex/GNO [27] and SAGE [28]. In our model-independent analysis we assume a uniform prior probability complemented by a set of constraints to ensure consistency in the pp-chain and CNO-cycle, as well as some relations from nuclear physics [25] concerns the prior on the ratio of pep to pp fluxes, which is constrained to match the average of the GS98 and AGSS09 predictions with 1σ uncertainty given by the difference between the two values: with the models in ref. [25] we perform two analysis which differ in the inclusion of the so-called “luminosity constraint”, i.e., the requirement that the sum of the thermal energy generation rates associated with each of the solar neutrino fluxes coincides with the solar luminosity [55]. We finish by reminding the reader that all these conditions from consistency and nuclear physics relations as well as eq (2.5) are constraints on some linear combinations of the solar fluxes and they are model independent, i.e., they do not impose any prior bias favoring either of the SSMs
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