THE R-PROCESS AND NEUTRINO-HEATED SUPERNOVA EJECTA

As a neutron star is formed by the collapse of the iron core of a massive star, its Kelvin-Helmholtz evolution is characterized by the release of gravitational binding energy as neutrinos. The interaction of these neutrinos with heated material above the neutron star generates a hot bubble in an atmosphere that is nearly in hydrostatic equilibrium and heated, after approximately 10 s, to an entropy of S/N(A) k greater than or similar to 400. The neutron-to-proton ratio for material moving outward through this bubble is set by the balance between neutrino and antineutrino capture on nucleons. Because the electron antineutrino spectrum at this time is hotter than the electron neutrino spectrum, the bubble is neutron-rich (0.38 less than or similar to Y(e) less than or similar to 0.47). Previous work using a schematic model has shown that these conditions are well suited to the production of heavy elements by the r-process. In this paper we have advanced the numerical modeling of a 20 M. ''delayed'' supernova explosion to the point that we can follow the detailed evolution of material moving through the bubble at the late times appropriate to r-process nucleosynthesis. The supernova model predicts a final kinetic energy for the ejecta of 1.5 x 10(51) ergs and leaves behind a remnant with a baryon mass of 1.50 M. (and a gravitational mass of 1.445 M.). We follow the thermodynamic and compositional evolution of 40 trajectories in rho(t), T(t), Y(e)(t) for a logarithmic grid of mass elements for the last almost-equal-to 0.03 M. to be ejected by the proto-neutron star down to the last <10(-6) M. of material expelled at up to almost-equal-to 18 s after core collapse. We find that an excellent fit to the solar r-process abundance distribution is obtained with no adjustable parameters in the nucleosynthesis calculations. Moreover, the abundances are produced in the quantities required to account for the present Galactic abundances. However, at earlier times, this one-dimensional model ejects too much material with entropies S/N(A) k approximately 50 and Y(e) approximately 0.46. This leads to an unacceptable overproduction of N = 50 nuclei, particularly Sr-88, Y-89, and Zr-90, relative to their solar abundances. We speculate on various means to avoid the early overproduction and/or ejection of N = 50 isotonic nuclei while still producing and ejecting the correct amount of r-process material.