Supernova Nucleosynthesis

Details Supernova Nucleosynthesis Supernova Nucleosynthesis

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aps..dnp4wb001h&link_type=abstract

American Physical Society, Division of Nuclear Physics Fall Meeting, October 30 - November 1, 2003, Tucson, Arizona, MEETING ID:

Physics

Nuclear Physics

Scientific paper

At the end of a massive star's life, or if a smaller mass stellar remnant accretes enough mass, it may encounter a powerful explosion -- a supernova -- and eject most or all of the ashes of preceding nuclear burning stages back into space, yet its composition modified by the explosion itself. These supernovae are the main source of oxygen and heavier elements ("metals") in the universe. A detailed understanding of the composition of these ejecta is thus an essential ingredient to understand the present composition of our solar system as well as the chemical evolution of galaxies and the universe as a whole. We will review the nucleosynthesis in thermonuclear and core collapse supernovae. Special emphasis will be given to the production of heavy elements beyond the iron group, the gamma-process and the neutrino-process, for which we will also present detailed calculations following all isotopes up to bismuth for the entire life and terminal explosion of the star.

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