Search for important weak interaction nuclei in presupernova evolution

Details Search for important weak interaction nuclei in presupernova evolution Search for important weak interaction nuclei in presupernova evolution

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apjs...91..389a&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 91, no. 1, p. 389-417

Astronomy and Astrophysics

Astrophysics

85

Abundance, Beta Particles, Decay Rates, Electron Capture, Equilibrium, Isotopes, Massive Stars, Stellar Evolution, Stellar Interiors, Supernovae, Tables (Data), Weak Interactions (Field Theory), Ranking, Silicon, Statistical Analysis, Stellar Temperature

Scientific paper

A search is made for the most important electron captures and beta-decays after core silicon burning in massive stars. A nuclear statistical equilibrium code is used to compute isotopic abundances. Electron capture and beta-decay rates are estimated for the 150 most abundant isotopes in a simplified fashion which generally includes the strongest transitions. These estimates are made for nuclei in the fp-shell and use techniques similar to Fuller, Fowler, & Newman (1982a), and are compared to them. The general behavior of the rate of change of Ye is examined. These methods are then used to follow a typical stellar trajectory, seeking the most important weak interactions during the formation of the iron core. Ranked lists of nuclei are given, to prioritize more detailed studies on individual nuclei. Beta-decays are found to ben an important modification to the evolution below the rate of change of Ye approx. = 0.46 as the core approaches a state of dynamic equilibrium between electron captures and beta-decays.

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