Creation of the iron-group elements in a supernova explosion

Details Creation of the iron-group elements in a supernova explosion Creation of the iron-group elements in a supernova explosion

Feb 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980pazh....6..110p&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 6, Feb. 1980, p. 110-115.) Soviet Astronomy Letters, vol. 6, Jan.-Feb. 1980, p. 61-64.

Astronomy and Astrophysics

Astrophysics

1

Astrophysics, Nuclear Explosions, Nuclear Fusion, Supernovae, Transition Metals, Abundance, Iron, Isotopes, Stellar Models

Scientific paper

The possibility of an equilibrium synthesis of iron-peaked elements, with atomic number between 22 and 30, is examined in terms of a model for a type II supernova explosion in which the degree of neutronization and the density-temperature relationship are determined by model calculations. The equilibrium concentrations of the elements are computed for a certain radial region of the star where the e-process ought to operate, with neutronization determined by the kinetics of the beta-processes. Results for an equilibrium temperature of 3.5 x 10 to the 9th K in the stellar region intermediate between the core, where r-process is thought to operate and the surface, in which explosive nucleosynthesis is present, are shown to agree well with cosmic abundances.

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