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    Solar fusion III: New data and theory for hydrogen-burning stars

    B. Acharya, M. Aliotta, A. B. Balantekin, D. Bemmerer, C. A. Bertulani, A. Best, C. R. Brune, R. Buompane, L. Gialanella et al.

    B. Acharya

    • Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA

    M. Aliotta

    • SUPA, School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3FD, United Kingdom

    A. B. Balantekin

    • Department of Physics, University of Wisconsin–Madison, Madison, Wisconsin 53706, USA

    D. Bemmerer

    • Helmholtz-Zentrum Dresden-Rossendorf, 01328 Dresden, Germany

    C. A. Bertulani

    • Department of Physics and Astronomy, Texas A&M University–Commerce, Commerce, Texas 75429-3011, USA

    A. Best

    • University of Napoli Federico II, 80126 Napoli, Italy and Istituto Nazionale di Fisica Nucleare–Napoli, 80126 Napoli, Italy

    C. R. Brune

    • Edwards Accelerator Laboratory, Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA

    R. Buompane and L. Gialanella

    • Dipartimento di Matematica e Fisica, Università degli Studi della Campania “Luigi Vanvitelli,” 81100 Caserta, Italy and Istituto Nazionale di Fisica Nucleare–Napoli, 80126 Napoli, Italy

    F. Cavanna

    • Istituto Nazionale di Fisica Nucleare–Torino, 10125 Torino, Italy

    J. W. Chen

    • Department of Physics and Center for Theoretical Physics, National Taiwan University, Taipei 10617, Taiwan and Physics Division, National Center for Theoretical Sciences, Taipei 10617, Taiwan

    J. Colgan

    • Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA

    A. Czarnecki

    • Department of Physics, University of Alberta, Edmonton, Alberta T6G 2E1, Canada

    B. Davids

    • TRIUMF, Vancouver, British Columbia V6T 2A3, Canada and Department of Physics, Simon Fraser University, Burnaby, British Columbia V5A 1S6, Canada

    R. J. deBoer

    • Department of Physics and Astronomy and the Joint Institute for Nuclear Astrophysics, University of Notre Dame, Notre Dame, Indiana 46556, USA

    F. Delahaye

    • Observatoire de Paris–PSL, Sorbonne Université, 5 Place Jules Janssen, 92195 Meudon Cedex, France

    R. Depalo and A. Guglielmetti

    • Università degli Studi di Milano, 20133 Milano, Italy and Istituto Nazionale di Fisica Nucleare-Milano, 20133 Milano, Italy

    A. García and R. G. H. Robertson

    • Department of Physics and Center for Experimental Nuclear Physics and Astrophysics, University of Washington, Seattle, Washington 98195, USA

    M. Gatu Johnson

    • Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA

    D. Gazit

    • Racah Institute of Physics, The Hebrew University, The Edmond J. Safra Campus, Givat Ram, Jerusalem 9190401, Israel

    U. Greife

    • Colorado School of Mines, Golden, Colorado 80401, USA

    D. Guffanti

    • Dipartimento di Fisica, Università degli Studi e INFN Milano-Bicocca, 20126 Milano, Italy

    K. Hambleton

    • Department of Physics, University of California, Berkeley, California 94720, USA

    W. C. Haxton*

    • Department of Physics, University of California, Berkeley, California 94720, USA and Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA

    Y. Herrera and A. Serenelli

    • Institute of Space Sciences, 08193 Cerdanyola del Vallès, Barcelona, Spain and Institut d’Estudis Espacials de Catalunya, 08034 Barcelona, Spain

    M. Huang

    • Department of Physics and Astronomy, Iowa State University, Ames, Iowa 50011, USA and Lawrence Livermore National Laboratory, P.O. Box 808, L-414, Livermore, California 94551, USA

    C. Iliadis

    • Department of Physics and Astronomy, University of North Carolina at Chapel Hill, Chapel Hill, North Carolina 27599-3255, USA and Triangle Universities Nuclear Laboratory (TUNL), Duke University, Durham, North Carolina 27708, USA

    K. Kravvaris

    • Lawrence Livermore National Laboratory, P.O. Box 808, L-414, Livermore, California 94551, USA

    M. La Cognata

    • Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali del Sud, 95123 Catania, Italy

    K. Langanke

    • GSI Helmholtzzentrum für Schwerionenforschung, Darmstadt, Germany and Institut für Kernphysik, Technical University Darmstadt, Darmstadt, Germany

    L. E. Marcucci

    • Department of Physics “E. Fermi,” University of Pisa, 56127 Pisa, Italy and Istituto Nazionale di Fisica Nucleare–Pisa, 56127 Pisa, Italy

    T. Nagayama

    • Sandia National Laboratories, Albuquerque, New Mexico 87123, USA

    K. M. Nollett

    • Department of Physics, San Diego State University, San Diego, California 92182, USA

    D. Odell

    • Department of Physics and Astronomy, Ohio University, Athens, Ohio 45701, USA

    G. D. Orebi Gann

    • University of California, Berkeley, California 94720, USA and Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA

    D. Piatti

    • Università degli Studi di Padova, Via Francesco Marzolo 8, 35131 Padova, Italy and INFN, Sezione di Padova, Via Francesco Marzolo 8, 35131 Padova, Italy

    M. Pinsonneault

    • Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, Ohio 43210, USA and Center for Cosmology and AstroParticle Physics, The Ohio State University, 191 West Woodruff Avenue, Columbus, Ohio 43210, USA

    L. Platter

    • Department of Physics and Astronomy, University of Tennessee, Knoxville, Tennessee 37996, USA and Physics Division, Oak Ridge National Laboratory, Oak Ridge, Tennessee 37831, USA

    G. Rupak

    • Department of Physics and Astronomy and HPC2 Center for Computational Sciences, Mississippi State University, Mississippi State, Mississippi 39762, USA

    M. Sferrazza

    • Université Libre de Bruxelles, Bruxelles, Belgium

    T. Szücs

    • HUN-REN Institute for Nuclear Research (HUN-REN ATOMKI), 4026 Debrecen, Hungary

    X. Tang

    • IMP Chinese Academy of Science, Lanzhou, China

    A. Tumino

    • Dipartimento di Ingegneria e Architettura, Università degli Studi di Enna “Kore,” Enna, Italy and Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali del Sud, 95123 Catania, Italy

    F. L. Villante

    • Dipartimento di Scienze Fisiche e Chimiche, Università dell’Aquila, 67100 L’Aquila, Italy and Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali del Gran Sasso, 67100 Assergi (AQ), Italy

    A. Walker-Loud

    • Nuclear Science Division, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA

    X. Zhang

    • Facility for Rare Isotope Beams, Michigan State University, East Lansing, Michigan 48824, USA

    K. Zuber

    • Institute for Nuclear and Particle Physics, Technical University of Dresden, 01062 Dresden, Germany

    • *Contact author: haxton@berkeley.edu

    Rev. Mod. Phys. 97, 035002 – Published 4 September, 2025

    DOI: https://doi.org/10.1103/8lm7-gs18

    Abstract

    In stars that lie on the main sequence in the Hertzsprung-Russell diagram, like our Sun, hydrogen is fused to helium in a number of nuclear reaction chains and series, such as the proton-proton chain and the carbon-nitrogen-oxygen cycles. Precisely determined thermonuclear rates of these reactions lie at the foundation of the standard solar model. This review, the third decadal evaluation of the nuclear physics of hydrogen-burning stars, is motivated by the great advances made in recent years by solar neutrino observatories, putting experimental knowledge of the proton-proton (pp)-chain neutrino fluxes in the few-percent precision range. The basis of the review is a one-week community meeting held in July 2022 in Berkeley, California, and many subsequent digital meetings and exchanges. The relevant reactions of solar and stellar hydrogen burning are reviewed here from both theoretical and experimental perspectives. Recommendations for the state of the art of the astrophysical S factor and its uncertainty are formulated for each of them. Several other topics of paramount importance for the solar model are reviewed as well: recent and future neutrino experiments, electron screening, radiative opacities, and current and upcoming experimental facilities. In addition to reaction-specific recommendations, general recommendations are also formed.

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