A Semi-Analytical Computation of the Theoretical Uncertainties of the Solar Neutrino Flux

Abstract

We present a comparison between Monte Carlo simulations and a semi-analytical approach that reproduces the theoretical probability distribution functions of the solar neutrino fluxes, stemming from the $pp$, $pep$, $hep$, ${}^7\mathrm{Be}$, ${}^8\mathrm{B}$, ${}^{13}\mathrm{N}$, ${}^{15}\mathrm{O}$, and ${}^{17}\mathrm{F}$ source reactions. We obtain good agreement between the two approaches. Thus, the semi-analytical method yields confidence intervals that closely match those found, based on Monte Carlo simulations, and points towards the same general symmetries of the investigated probability distribution functions. Furthermore, the negligible computational cost of this method is a clear advantage over Monte Carlo simulations, making it trivial to take new observational constraints on the input parameters into account.

5 pages, 2 figures

References in corpus (5)

• A new Generation of Standard Solar Models
• ASTEC -- the Aarhus STellar Evolution Code
• CN-Cycle Solar Neutrinos and Sun's Primordial Core Metalicity
• Detailed Abundances of Planet-Hosting Wide Binaries. I. Did Planet Formation Imprint Chemical Signatures in the Atmospheres of HD 20782/81?
• Solar neutrinos and the solar composition problem

Cited by in corpus (3)

• Solar structure and evolution
• Investigating surface correction relations for RGB stars
• Bayesian inference of stellar parameters based on 1D stellar models coupled with 3D envelopes