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Neutron capture nucleosynthesis

Neutron capture nucleosynthesis describes two nucleosynthesis pathways: the r-process and the s-process, for rapid and slow neutron captures, respectively. R-process describes neutron capture in a region of high neutron flux, such as during supernova nucleosynthesis after core-collapse, and yields neutron-rich nuclides. S-process describes neutron capture that is slow relative to the rate of beta decay, as for stellar nucleosynthesis in some stars, and yields nuclei with stable nuclear shells. Each process is responsible for roughly half of the observed abundances of elements heavier than iron. The importance of neutron capture to the observed abundance of the chemical elements was first described in 1957 in the B2FH paper.[1]

References edit

  1. ^ Wallerstein, George; Icko Iben, Jr.; Peter Parker; Ann Merchant Boesgaard; et al. (1997). "Synthesis of the elements in stars: forty years of progress" (PDF). Reviews of Modern Physics. 69 (4): 995. Bibcode:1997RvMP...69..995W. doi:10.1103/RevModPhys.69.995. hdl:2152/61093.

Further reading edit

  • E. M. Burbidge; G. R. Burbidge; W. A. Fowler; F. Hoyle (1957). "Synthesis of the Elements in Stars". Reviews of Modern Physics. 29 (4): 547–650. Bibcode:1957RvMP...29..547B. doi:10.1103/RevModPhys.29.547.


neutron, capture, nucleosynthesis, describes, nucleosynthesis, pathways, process, process, rapid, slow, neutron, captures, respectively, process, describes, neutron, capture, region, high, neutron, flux, such, during, supernova, nucleosynthesis, after, core, c. Neutron capture nucleosynthesis describes two nucleosynthesis pathways the r process and the s process for rapid and slow neutron captures respectively R process describes neutron capture in a region of high neutron flux such as during supernova nucleosynthesis after core collapse and yields neutron rich nuclides S process describes neutron capture that is slow relative to the rate of beta decay as for stellar nucleosynthesis in some stars and yields nuclei with stable nuclear shells Each process is responsible for roughly half of the observed abundances of elements heavier than iron The importance of neutron capture to the observed abundance of the chemical elements was first described in 1957 in the B2FH paper 1 References edit Wallerstein George Icko Iben Jr Peter Parker Ann Merchant Boesgaard et al 1997 Synthesis of the elements in stars forty years of progress PDF Reviews of Modern Physics 69 4 995 Bibcode 1997RvMP 69 995W doi 10 1103 RevModPhys 69 995 hdl 2152 61093 Further reading editE M Burbidge G R Burbidge W A Fowler F Hoyle 1957 Synthesis of the Elements in Stars Reviews of Modern Physics 29 4 547 650 Bibcode 1957RvMP 29 547B doi 10 1103 RevModPhys 29 547 nbsp This nuclear chemistry related article is a stub You can help Wikipedia by expanding it vte Retrieved from https en wikipedia org w index php title Neutron capture nucleosynthesis amp oldid 1165800652, wikipedia, wiki, book, books, library,

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