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Synthesis of the elements in stars: forty years of progress

George Wallerstein, Icko Iben, , Jr., Peter Parker, Ann Merchant Boesgaard, Gerald M. Hale, Arthur E. Champagne, Charles A. Barnes, Franz Käppeler, Verne V. Smith et al.

George Wallerstein

  • Department of Astronomy, University of Washington, Seattle, Washington 98195

Icko Iben, , Jr.

  • University of Illinois, 1002 West Green Street, Urbana, Illinois 61801

Peter Parker

  • Yale University, New Haven, Connecticut 06520-8124

Ann Merchant Boesgaard

  • Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, Hawaii 96822

Gerald M. Hale

  • Los Alamos National Laboratory, Los Alamos, New Mexico 87544

Arthur E. Champagne

  • University of North Carolina at Chapel Hill, Chapel Hill, North Carolina 27594
  • Triangle Universities Nuclear Laboratory, Duke University, Durham, North Carolina 27706

Charles A. Barnes

  • California Institute of Technology, Pasadena, California 91125

Franz Käppeler

  • Forschungzentrum, Karlsruhe, D-76021, Germany

Verne V. Smith

  • University of Texas at El Paso, El Paso, Texas 79968-0515

Robert D. Hoffman

  • Steward Observatory, University of Arizona, Tucson, Arizona 85721

Frank X. Timmes

  • University of California at Santa Cruz, California 95064

Chris Sneden

  • University of Texas, Austin, Texas 78712

Richard N. Boyd

  • Ohio State University, Columbus, Ohio 43210

Bradley S. Meyer

  • Clemson University, Clemson, South Carolina 29630

David L. Lambert

  • University of Texas, Austin, Texas 78712

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Rev. Mod. Phys. 69, 995 – Published 1 October, 1997

DOI: https://doi.org/10.1103/RevModPhys.69.995

Abstract

Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B2FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments.

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