Theoretical evaluation of solar proton-proton fusion reaction rate and its uncertainties

The weak proton-proton fusion into a deuteron (${}^2$H) is the driving reaction in the energy production in the Sun, as well as similar main sequence stars. Its reaction rate in the solar interior is determined only theoretically. Here, we provide a new determination of the rate of this reaction in solar conditions $S^{11}(0)$, and analyze theoretical and experimental sources for uncertainties, using effective field theory of quantum chromo-dynamics without explicit pions at next-to-leading order. We find an enhancement of $S^{11}$ by $1-4\mathrm{\%}$ over the previously recommended value. This change reduces the calculated fluxes of neutrinos originating in ${}^8$B and ${}^7$Be nuclear reactions in the Sun, thus favoring higher abundances for metallic photospheric elements, in the tension between different composition determination, known as the ``Solar Composition Problem’'.