Neutrino Effects before, during, and after the Freezeout of the r-Process

Details Neutrino Effects before, during, and after the Freezeout of the r-Process Neutrino Effects before, during, and after the Freezeout of the r-Process

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...608..470t&link_type=abstract

The Astrophysical Journal, Volume 608, Issue 1, pp. 470-479.

Astronomy and Astrophysics

Astronomy

13

Neutrinos, Nuclear Reactions, Nucleosynthesis, Abundances

Scientific paper

We study the effects of neutrino interactions before, during, and after the operation of the r-process in the context of a relativistic hydrodynamic neutrino-energized wind model that includes a Boltzmann solver for the dominant neutrino transport. We also employ newly available charged- and neutral-current interaction rates. Studies are made in a model with a short dynamical timescale that gives a fair reproduction of the solar system r-process abundance curve and hence could be a fair approximation to the true supernova environment. We confirm that charged- and neutral-current interactions can have specific unique effects on the final abundances. Early on, charged-current interactions determine the electron fraction, while later on, neutrino-induced neutron emission can continue to provide a slight neutron exposure even after the freezeout of the r-process. We propose two new potentially observable effects that derive from the use of a more realistic hydrodynamic model and/or new neutrino interaction rates. One is an enhanced odd-even effect in the final abundances, and the other is an enhancement of light A=68-76 nuclei in the final abundances. These effects are consistent with some recent observations of r-process abundances in metal-poor halo stars and might help to identify the neutrino fluxes present near the freezeout of the r-process.

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