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

Abstract

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 $1-4\%$ 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''.

9 pages, 3 figures

References in corpus (10)

• The chemical make-up of the Sun: A 2020 vision
• Superallowed 0+ to 0+ nuclear beta decays: A new survey with precision tests of the conserved vector current hypothesis and the standard model
• A new Generation of Standard Solar Models
• Three-Nucleon Low-Energy Constants from the Consistency of Interactions and Currents in Chiral Effective Field Theory
• Observational constraints on the origin of the elements. IV: The standard composition of the Sun
• Measurement of the Weak Axial-Vector Coupling Constant in the Decay of Free Neutrons Using a Pulsed Cold Neutron Beam
• High Statistics Analysis using Anisotropic Clover Lattices: (II) Three-Baryon Systems
• Power Counting of Contact-Range Currents in Effective Field Theory
• Proton-proton fusion in pionless effective theory
• The proton-deuteron system in pionless EFT revisited

Cited by in corpus (1)

• Role of spin-isospin symmetries in nuclear $\beta$-decays