2012ApJ...758....9N -
Astrophys. J., 758, 9 (2012/October-2)
Nucleosynthesis in core-collapse supernova explosions triggered by a quark-hadron phase transition.
NISHIMURA N., FISCHER T., THIELEMANN F.-K., FROHLICH C., HEMPEL M., KAPPELI R., MARTINEZ-PINEDO G., RAUSCHER T., SAGERT I. and WINTELER C.
Abstract (from CDS):
We explore heavy-element nucleosynthesis in the explosion of massive stars that are triggered by a quark-hadron phase transition during the early post-bounce phase of core-collapse supernovae. The present study is based on general-relativistic radiation hydrodynamics simulations with three-flavor Boltzmann neutrino transport in spherical symmetry, which utilize a quark-hadron hybrid equation of state based on the MIT bag model for strange quark matter. The quark-hadron phase transition inside the stellar core forms a shock wave propagating toward the surface of the proto-neutron star. This shock wave results in an explosion and ejects neutron-rich matter from the outer accreted layers of the proto-neutron star. Later, during the cooling phase, the proto-neutron star develops a proton-rich neutrino-driven wind. We present a detailed analysis of the nucleosynthesis outcome in both neutron-rich and proton-rich ejecta and compare our integrated nucleosynthesis with observations of the solar system and metal-poor stars. For our standard scenario, we find that a "weak" r-process occurs and elements up to the second peak (A ∼ 130) are successfully synthesized. Furthermore, uncertainties in the explosion dynamics could barely allow us to obtain the strong r-process which produces heavier isotopes, including the third peak (A ∼ 195) and actinide elements.
Abstract Copyright:
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Journal keyword(s):
dense matter - nuclear reactions, nucleosynthesis, abundances - stars: neutron - supernovae: general
Simbad objects:
3
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