Nucleosynthesis in neutrino-driven winds from protoneutron stars II. The r-process

Details Nucleosynthesis in neutrino-driven winds from protoneutron stars II. The r-process Nucleosynthesis in neutrino-driven winds from protoneutron stars II. The r-process

Jun 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...286..857t&link_type=abstract

Astronomy and Astrophysics 286, 857-869 (1994)

Astronomy and Astrophysics

Astrophysics

201

Nuclear Reactions, Nucleosynthesis, Abundances, Supernovae: General

Scientific paper

The preceding paper (Witti et al. 1994; Paper I) dealt with the α-process nucleosynthesis in the "hot bubble" region of a type-II supernova, and explored the possibility of a subsequent occurrence of the r-process. It was concluded that, for a successful r-processing, the entropies in the hot bubble would have to be somewhat higher than those given by the adopted hydrodynamical model. In the present work, we demonstrate that a reduction of the matter densities (i.e. an increase of the entropies) by a constant factor of about five, everywhere in the hot bubble and throughout its evolution, results in an r-process abundance distribution in the range of mass numbers A>90 that resembles that of the solar system very well. This is surprising, given the fact that the temperatures, matter densities, degrees of neutron excess, concentrations of free neutrons, and the α-processed nuclear abundances not only vary with time, but also depend considerably on the referenced mass segments inside the hot bubble. Whereas the propriety of the density scaling has yet to be verified, the reproduction of the relative, and in a sense the absolute, amounts of r-process nuclei appears too good to be a mere coincidence. Therefore, we conclude that the hot-bubble region in a type-II supernova is indeed a very promising site for the r-process.

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