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Synthesis of the Elements in Stars
Man inhabits a universe composed of a great variety of elements and their isotopes. In Table I,1 a count of the stable and radioactive elements and isotopes is listed. Ninety elements are found
Lithium and the s-process in red-giant stars
Red giant star s-process and subsequent delayed electron capture, accounting for large Li abundances
Stellar weak interaction rates for intermediate mass nuclei. III. Rate tables for the free nucleons and nuclei with A = 21 TO A = 60
Stellar electron and positron emission rates and continuum electron and positron capture rates, as well as the associated neutrino energy loss rates, are tabulated for the free nucleons and 226
Stellar weak interaction rates for intermediate-mass nuclei. IV - Interpolation procedures for rapidly varying lepton capture rates using effective log (ft)-values
Simple expressions for continuum electron and positron capture phase space factors and the associated neutrino energy loss integrals are presented in terms of standard Fermi integrals. Continuous
The quest for the origin of the elements.
  • W. Fowler
  • Physics, Education
    Science
  • 1 March 1984
All life on Earth depends on the energy in sunlight, which comes initially from the nuclear fusion of hydrogen into helium deep in the solar interior. But the sun did not produce the chemical
Neutrino processes and pair formation in massive stars and supernovae.
Abstract : The paper traces the physical properties of matter inside highly evolved stars, on the assumption that the whole material of the star is non-degenerate and that the star is in
Stellar weak-interaction rates for sd-shell nuclei. I - Nuclear matrix element systematics with application to Al-26 and selected nuclei of importance to the supernova problem
Astrophysical positron emission, continuum electron capture, and neutrino energy loss rates are calculated for 26 A1—> 26 Mg, 30 P—» 30 Si, 31 S—> 31 P, 32 S—> 32 P, 33 S-> 33 P, and 35 C1-* 35 S.
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