Speaker
Nobuya Nishimura
(YITP, Kyoto University)
Description
The r-process nucleosynthesis has been considered to occur in explosive astronomical phenomena relevant to neutron stars, e.g. core-collapse supernovae and mergers of compact-object (neutron stars/black holes) binaries. However, detailed quantitative properties in astrophysical models for the r-process are not completely understood yet. In this talk, I will show recent results of r-process nucleosynthesis in neutron star mergers, based on our collaboration. As mass ejection through neutron star mergers has several phases with different nucleosynthesis composition, I will focus on nucleosynthesis yields on neutrino-driven ejecta in the post-merger phase, based on the hydrodynamical models by Fujibayashi et al. (2018), ApJ (in press, arXiv:1711.02093). The neutrino irradiated ejecta in the later phase is expected to be less neutron-rich and produce lighter and medium mass r-process nuclei. I will our results basically agree with the recent observation for the early blue component of kilonova associated with GW170817.
Primary author
Nobuya Nishimura
(YITP, Kyoto University)
Co-authors
Kenta Kiuchi
(Kyoto University)
Masaru Shibata
(Kyoto University)
Sho Fujibayashi
(Kyoto University)
Yuichiro Sekiguchi
(Toho University)
