Constraining the $^7$Be($p,\gamma$)$^8$B $S$-factor with the new precise $^7$Be solar neutrino flux from Borexino

TL;DR

This paper uses precise measurements of solar neutrino fluxes from Borexino and the Standard Solar Model to constrain the $^7$Be($p, abla$)$^8$B astrophysical $S$-factor at solar energies, reducing uncertainties from direct measurements.

Contribution

It introduces a novel method to determine the $^7$Be($p, abla$)$^8$B $S$-factor using neutrino flux data and solar models, bypassing the need for low-energy experimental data.

Findings

The $^7$Be($p, abla$)$^8$B $S$-factor is constrained at solar energies.

The $^3$He($ abla$,$ abla$)$^7$Be $S$-factor is re-evaluated using a similar approach.

Uncertainties in the $S$-factor extrapolation are significantly reduced.

Abstract

Among the solar fusion reactions, the rate of the $^7$Be($p,\gamma$)$^8$B reaction is one of the most difficult to determine rates. In a number of previous experiments, its astrophysical $S$-factor has been measured at $E$ = 0.1-2.5 MeV center-of-mass energy. However, no experimental data is available below 0.1 MeV. Thus, an extrapolation to solar energies is necessary, resulting in significant uncertainty for the extrapolated $S$-factor. On the other hand, the measured solar neutrino fluxes are now very precise. Therefore, the problem of the $S$-factor determination is turned around here: Using the measured $^7$Be and $^8$B neutrino fluxes and the Standard Solar Model, the $^7$Be($p,\gamma$)$^8$B astrophysical $S$-factor is determined at the solar Gamow peak. In addition, the $^3$He($\alpha$,$\gamma$)$^7$Be $S$-factor is redetermined with a similar method.