Solar seismic models and the neutrino predictions

This paper focuses on the solar neutrino fluxes, the g-mode predictions, and the possible impact of the magnetic fields on the neutrino emission and transport. The Solar and Heliospheric Observatory (SOHO) spacecraft has allowed astrophysicists to achieve a major breakthrough in the knowledge of the solar core. Both GOLF and MDI instruments on SOHO have significantly improved the accuracy of the sound speed profile, mainly by the detection of low-degree low-order p-modes. Our study (Turck-Chièze and coworkers) has lead to precise neutrino predictions through constructing a seismic solar model that is in good agreement with the sound speed profile inferred by helioseismology in the radiative interior of the Sun. In this paper we present the details of this study and investigate new solar models validated by the acoustic modes. These new models are primarily used to derive the emitted neutrino fluxes. We show that these fluxes do not depend strongly on the modified physics as far as the model is consistent with the helioseismic observations in the core. We also show that an internal large-scale magnetic field cannot exceed a maximum strength of ≃3 × 10⁷ G in the radiative zone and may increase the emitted ⁸B neutrino flux only by ≃2%. All the neutrino predictions here are compatible with the Sudbury Neutrino Observatory results, assuming three neutrino flavors. We deduce the electron and neutron radial densities that are needed to calculate the neutrino oscillation properties. Finally, we discuss how the magnetic fields may influence the neutrino transport through the RSFP process, for different values of Δm².