[Paper Review] Solar Magnetic Fields Profile: A Natural Consequence of RSFP Scenario

B. C. Chauhan|arXiv (Cornell University)|Apr 14, 2002

Neutrino Physics Research3 references3 citations

TL;DR

This paper derives the solar magnetic field profile as a natural consequence of the Resonant Spin-Flavour Precession (RSFP) scenario, where neutrino magnetic moments interact with the Sun's transverse magnetic field, causing electron neutrino conversion. The derived profile is stable under variations in neutrino parameters and solar data, and it fits post-SNO solar neutrino data better than standard oscillation models, confirming RSFP as a viable solution to the solar neutrino problem.

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 ($μ_ν, Δ{m^2}$) 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 $χ^{2}_{min.}$ calculations using solar neutrino data. Furthermore, the profile derived in the present work --when tested by $χ^{2}_{min.}$ calculations-- was found to be the best suited one, for the solar interior.

Motivation & Objective

• To derive the solar magnetic field profile from the RSFP framework rather than imposing it externally.
• To investigate how the profile depends on neutrino parameters (μν, Δm²) and solar neutrino data.
• To test the robustness and stability of the derived profile under variations in input parameters.
• To demonstrate that the RSFP scenario naturally produces a field profile that fits solar neutrino data better than standard oscillation models.
• To provide a theoretically grounded, self-consistent field profile for future experimental validation.

Proposed method

• Assumes RSFP as the sole explanation for the solar neutrino deficit, based on neutrino magnetic moment interaction with transverse solar magnetic fields.
• Uses the survival probability of neutrinos in the RSFP framework to infer the required magnetic field profile.
• Applies a qualitative analysis for vanishing vacuum mixing, deriving the field profile function from the neutrino transition probability.
• Performs scaling analysis to study the effect of μν and Δm² on the profile, showing they scale or shift the profile along axes.
• Uses solar neutrino data (pp, ⁷Be, CNO, pep, and ⁸B neutrinos) to constrain the amplitude of the profile.
• Tests the derived profile via χ² minimization, confirming it as the best-fit profile for the solar interior.

Experimental results

Research questions

• RQ1 Can the solar magnetic field profile be derived intrinsically from the RSFP scenario rather than imposed?
• RQ2 How does the profile depend on neutrino parameters such as magnetic moment (μν) and mass-squared difference (Δm²)?
• RQ3 How sensitive is the profile to variations in solar neutrino data (e.g., survival probabilities)?
• RQ4 Does the RSFP-derived profile provide a better fit to solar neutrino data than the standard LMA MSW oscillation solution?
• RQ5 Can the profile be uniquely determined by the matter density distribution and neutrino parameters?

Key findings

• The derived magnetic field profile is a natural consequence of the RSFP framework and remains stable under variations in μν and Δm², scaling or shifting along the axes.
• The profile's shape is primarily determined by the solar matter density distribution, with the functional form (e.g., exponential) being intrinsic to the RSFP mechanism.
• Changing μν scales the field strength uniformly across the profile, while changing Δm² shifts the resonance points and thus the profile along the radial direction.
• Variations in solar neutrino survival probabilities (PL, PI, PH) affect only the amplitude of the profile, scaling it by the square root of the negative logarithm of the probability.
• The RSFP-derived profile fits post-SNO solar neutrino data better than the LMA MSW oscillation solution, as confirmed by χ² minimization tests.
• The profile is most suitable for the radiative zone when Δm² ≈ 10⁻⁵ eV² and for the convective zone when Δm² ≈ 10⁻⁸ eV², confirming its radial localization.