Chiral corrections to the Adler-Weisberger sum rule

TL;DR

This paper calculates the leading chiral corrections to the Adler-Weisberger sum rule for nucleon axial charge, compares it with experimental data, and refines the value of g_A considering various uncertainties.

Contribution

It provides the first systematic derivation of universal chiral corrections to the sum rule using chiral perturbation theory and confronts the corrected sum rule with experimental data.

Findings

Calculated g_A as 1.248 with combined uncertainties.

Quantified the impact of chiral corrections on the sum rule.

Validated the sum rule against recent experimental and theoretical inputs.

Abstract

The Adler-Weisberger sum rule for the nucleon axial-vector charge, $g_A$, offers a unique signature of chiral symmetry and its breaking in QCD. Its derivation relies on both algebraic aspects of chiral symmetry, which guarantee the convergence of the sum rule, and dynamical aspects of chiral symmetry breaking---as exploited using chiral perturbation theory---which allow the rigorous inclusion of explicit chiral symmetry breaking effects due to light-quark masses. The original derivations obtained the sum rule in the chiral limit and, without the benefit of chiral perturbation theory, made various attempts at extrapolating to non-vanishing pion masses. In this paper, the leading, universal, chiral corrections to the chiral-limit sum rule are obtained. Using PDG data, a recent parametrization of the pion-nucleon total cross-sections in the resonance region given by the SAID group, as well as recent Roy-Steiner equation determinations of subthreshold amplitudes, threshold parameters, and correlated low-energy constants, the Adler-Weisberger sum rule is confronted with experimental data. With uncertainty estimates associated with the cross-section parameterization, the Goldberger-Treimann discrepancy, and the truncation of the sum rule at $\mathcal{O}(M_\pi^4)$ in the chiral expansion, this work finds $g_A = 1.248 \pm 0.010 \pm \ 0.007 \pm 0.013$.