r-Process Nucleosynthesis in Supernova Explosions : From Unstable Nuclei to Observation of Stars
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概要
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We have studied the r-process elements produced from supernovae by performing the numerical simulations of hydrodynamics coupled with the nuclear reaction network. We have found that r-process can take place in two scenarios probably depending on the mass of presupernova stars from the mass range of 10 〜 30M⊙. For small mass stars with small Fe core, r-process happens in the material ejected during prompt explosions. The layers of neutron-rich material dynamically ejected from near the surface of the neutron star contribute to the r-process elements of both the 2nd and 3rd peaks. For large mass stars, r-process takes place in the mass loss through the neutrino-driven winds above the hot neutron star born in the delayed explosion mechanism. The layers gradually evaporated from the neutron star surface by neutrino heating contribute to the r-process nucleosynthesis up to the 2nd or the 3rd peak depending on the supernova environment. It is found that the dynamics of outward flow significantly depends on the outer pressure of gas above the wind and alters the outcome of r-process, besides the effects of different neutrino luminosities and neutron star masses and radii. The success of r-process in these scenarios contributes to pin down which supernova event is responsible for r-process elements. If the abundance patterns in two scenarios are clearly different each other, supernova events in different mass ranges may contribute to the r-process abundance pattern in different ways. Therefore, it is important to evaluate the r-process products in a quantitative manner for supernova explosions in a wide mass range by performing careful numerical simulations of hydrodynamics and neutrino transfer. Full hydrodynamical simulations with neutrino transfer is currently being performed by us with the relativistic EOS table.
- 理論物理学刊行会の論文
- 2002-12-26
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