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【1.17】科技创新论坛(282)Impact of Neutron Star Mergers vs. Supernovae on Explosive Nucleosynthesis and Neutrino Physics
2017-12-11|文章来源: |【
 

高能所科技创新论坛(282)

报告题目:Impact of Neutron Star Mergers vs. Supernovae on Explosive Nucleosynthesis and Neutrino Physics
报告人:Toshitaka Kajino (Beihang University/University of Tokyo/National Astronomical Observatory of Japan)
主持人:曹俊 研究员
时间:1月17号上午10点
地点:化学楼C305

报告摘要:
宇宙中的黄金是怎么合成的?是来自中子星并合,还是超新星爆发?
梶野敏貴教授是北京航空航天大学的“千人计划”教授,将报告中子星并合与超新星爆发中的核合成,以及中微子振荡对核合成的影响。
GW170817 was really an event of the century that has opened the window to the frontier of multi-messenger astronomy and astrophysics. Gravitational waves from most likely the merging neutron stars were detected in LIGO-Virgo collaboration, GRB was observed in Fermi-GBM, and observed optical and near-infrared emissions in several Telescopes are consistent with those from radiative decays of r-process nuclei which are predicted theoretically in the nucleosynthesis calculation. Neutrinos were not detected unfortunately because of their too low flux from GW170817 that occurred at a distance 0.13 Gly away. We now await a nearby GW event (probably once per one-to-ten thousand years in our Milky Way) for spectroscopic observation of still unidentified r-process elements from neutron star mergers (NSMs).

In addition to the NSMs, core-collapse supernovae (of both magneto-hydrodynamic jet supernovae; MHD Jet-SNe, and neutrino-driven wind supernovae; nu-SNe) are viable candidates for the r-process sites. Supernova nucleosynthesis is expected to imprint significant evidence for the roles of neutrino interactions with matter including flavor oscillations. NSMs could not contribute to the early Galaxy for cosmologically long merging time-scale for slow GW radiation, while MHD Jet-SNe can explain the “universality” in the observed abundance pattern in metal poor stars. However, the NSM is still a possible nucleosynthetic site for the solar-system abundance. We would like to propose a novel solution to this twisted problem by carrying out both NSM and SN r-process nucleosynthesis calculations and numerical simulation of Galactic chemo-dynamical evolution. We will also discuss the impact of the SN nucleosynthesis on the physics of neutrino oscillations (including MSW, collective and vacuum oscillations).

报告人简介:
Professor Toshitaka Kajino is a distingushed professor of the "Thousand Talents Plan", and director of the International Research Center for Big-Bang Cosmology and Element Genesis in Beihang University. He is also the professor of Astronomy in the University of Tokyo and National Astronomical Observatory of Japan. Professor Kajino obtained his doctor's degree from the University of Tokyo in 1984, and then served as an assistant professor in Tokyo Metropolitan University from 1984 to 1993. After that, he moved to the University of Tokyo and National Astronomical Observatory of Japan as an full professor. Professor Kajino's main research topic lies in the creation of particles and nuclei and their roles in the cosmological and astrophysical environments. He has been working on the nucleosynthesis in Big Bang, supernova bursts and neutron star mergers, the cosmic chemical and dynamical evolution, and the origin of Galactic and extragalactic cosmic rays.

 

高能所科研计划处、党政联合办、教育处
2018年1月7日


 
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