Constraints on proton-proton fusion from helioseismology

2002/07/03 by K. I. T. Brown, Kevin I. T. Brown, M. N. Butler +4 · 1 citation
Environmental Science · Physics and Astronomy · #Astrophysics (astro-ph) #FOS: Physical sciences #Gamma-ray bursts and supernovae #Methane Hydrates and Related Phenomena #Nuclear Theory (nucl-th) #Solar and Space Plasma Dynamics #astro-ph #nucl-th

paper · pdf · doi:10.48550/arxiv.nucl-th/0207008

14 pages, 3 figures, uses RevTeX 4

arxiv created 2002/07/03 · openalex publication_date 2002/07/03 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28

Abstract

The proton-proton (pp) fusion cross-section found at the heart of solar models is unconstrained experimentally and relies solely on theoretical calculations. Effective field theory provides an opportunity to constrain the pp cross-section experimentally, however, this method is complicated by the appearance of two-nucleon effects in the form of an unknown parameter L_1,A. We present a method to constrain L_1,A using the Standard Solar Model and helioseismology. Using this method, we determine a value of L_1,A = 7.0 fm³ with a range of 1.6 to 12.4 fm³. These results are consistent with theoretical estimates of L_1,A ≈ 6 fm³.

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