Neutron capture

  • chart of nuclides showing thermal neutron capture cross section values

    neutron capture is a nuclear reaction in which an atomic nucleus and one or more neutrons collide and merge to form a heavier nucleus.[1] since neutrons have no electric charge, they can enter a nucleus more easily than positively charged protons, which are repelled electrostatically.[1]

    neutron capture plays an important role in the cosmic nucleosynthesis of heavy elements. in stars it can proceed in two ways: as a rapid (r-process) or a slow process (s-process).[1] nuclei of masses greater than 56 cannot be formed by thermonuclear reactions (i.e. by nuclear fusion), but can be formed by neutron capture.[1] neutron capture on protons yields a line at 2.223 mev predicted[2] and commonly observed[3] in solar flares.

  • neutron capture at small neutron flux
  • neutron capture at high neutron flux
  • capture cross section
  • thermochemical significance
  • uses
  • neutron absorbers
  • see also
  • references
  • external links

Chart of nuclides showing thermal neutron capture cross section values

Neutron capture is a nuclear reaction in which an atomic nucleus and one or more neutrons collide and merge to form a heavier nucleus.[1] Since neutrons have no electric charge, they can enter a nucleus more easily than positively charged protons, which are repelled electrostatically.[1]

Neutron capture plays an important role in the cosmic nucleosynthesis of heavy elements. In stars it can proceed in two ways: as a rapid (r-process) or a slow process (s-process).[1] Nuclei of masses greater than 56 cannot be formed by thermonuclear reactions (i.e. by nuclear fusion), but can be formed by neutron capture.[1] Neutron capture on protons yields a line at 2.223 MeV predicted[2] and commonly observed[3] in solar flares.