出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：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.
