Explosions of massive stars and the neutrino-driven wind in simulations using Boltzmann neutrino transport

Details Explosions of massive stars and the neutrino-driven wind in simulations using Boltzmann neutrino transport Explosions of massive stars and the neutrino-driven wind in simulations using Boltzmann neutrino transport

Aug 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1269..181f&link_type=abstract

THE 10TH INTERNATIONAL SYMPOSIUM ON ORIGIN OF MATTER AND EVOLUTION OF GALAXIES: OMEG-2010. AIP Conference Proceedings, Volume 1

Other

Stellar Mass, Supernovae, Neutrino, Nucleosynthesis, Neutron Stars, Masses, Supernovae, Neutrino, Muon, Pion, And Other Elementary Particles, Cosmic Rays, Origin, Formation, And Abundances Of The Elements, Neutron Stars

Scientific paper

Massive stars which end their lives in supernova explosions have long been investigated with respect to the synthesis of heavy elements. The neutrino-driven wind, which forms due to the continuous neutrino energy deposition after the explosion has been launched, is of central importance for the nucleosynthesis relevant conditions of the explosion ejecta. During the dynamical evolution, the neutrino-driven wind collides with the much slower expanding explosion ejecta. In the case of a supersonic expansion, this causes the appearance of a reverse shock known as the neutrino-driven wind termination shock. We investigate the formation of the neutrino-driven wind including the reverse shock consistently in simulations of several massive progenitor stars. We simulate more than 20 seconds after the explosions have been launched. Our model is based on spherically symmetric general relativistic radiation hydrodynamics using three flavour Boltzmann neutrino transport. Neutrino-driven explosions of massive Fe-core progenitors are obtained using enhanced neutrino opacities, where the explosion of the low mass O-Ne-Mg-core is obtained using the standard neutrino reaction rates. We investigate the conditions found in the neutrino-driven wind, in particular the possible site for the nucleosynthesis of heavy elements via the r-process, where we find that the initially during the explosion phase obtained proton-rich matter does not become neutron-rich for more than 10 seconds and the entropies per baryon found are too low. Although detailed nucleosynthesis analysis are required, we speculate that neutrino-driven explosions and the neutrino-driven wind fail to provide conditions that can explain the r-process.

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