Solar Magnetic Fields Profile: A Natural Consequence of RSFP Scenario

TL;DR

This paper derives a stable solar magnetic field profile based on the RSFP scenario, linking neutrino magnetic interactions with solar magnetic fields, and validates it against solar neutrino data.

Contribution

It presents a novel method to derive the solar magnetic field profile from neutrino data without relying on chi-squared minimization, emphasizing the profile's stability and dependence on solar matter density.

Findings

Derived a stable solar magnetic field profile consistent with neutrino data.

Profile is scalable with neutrino parameters and data, indicating robustness.

Tested profile fits solar interior conditions effectively.

Abstract

Assuming the solar neutrino deficit is resolved by the resonant interaction of the neutrino magnetic moment with the solar magnetic field --in the framework of Resonant Spin Flavour Precession (RSFP) scenario-- the solar magnetic field profile function has been derived from the scenario in the light of solar neutrino data. An approximate qualitative analysis has been done for vanishing vacuum mixing and it has been found that the profile derived is quite stable in nature. As because on changing the neutrino parameters ($\mu_{\nu}, \Delta{m^2}$) and the solar neutrino data the profile is just scaled along the axes. In principle, the nature of the profile is strongly dependent on the solar matter density distribution function. The current approach is quite different from the usual one- in which the best field profile is discovered by performing $\chi^{2}_{min.}$ calculations using solar neutrino data. Furthermore, the profile derived in the present work --when tested by $\chi^{2}_{min.}$ calculations-- was found to be the best suited one, for the solar interior.