Massive stars whose mass exceed 10 times the solar mass evolve until the Fe-core is formed. Since the nuclear reactions in the Fe-core do not proceed further, the core begins to collapse, which leads to the catastrophic explosion. The nucleosynthesis during the evolutions and subsequent explosions is responsible for the heavy element enrichment in our galaxy. We calculate heavy element nucleosynthesis during the magneto-hydrodynamical (MHD) explosion of supernova of a massive star. We consistently calculate all stages of the collapse of the Fe-core, the core bounce, and the shock wave propagation. When the shock wave propagate in the oxygen-neon layers, the p-process nucleosynthesis should occur. Until now, the p-process has been studied with use of spherical explosion models where significant deficiencies in some light p-elements compared to solar ones have been found. We present nonspherical effects on the production of p-elements using adiabatic MHD explosion model.
|ジャーナル||Proceedings of Science|
|出版ステータス||Published - 2006 12月 1|
|イベント||9th International Symposium on Nuclear Astrophysics - Nuclei in the Cosmos, NIC 2006 - Geneva, Switzerland|
継続期間: 2006 6月 25 → 2006 6月 30
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