協辦單位
NMNS
協辦單位
ASIAA
贊助單位
MOST
會徽Logo
名稱Title
2019天文年會
國立自然科學博物館
5月17日至19日

論文摘要

GRMHD Simulation of Binary Neutron Star Merger and the Mixing of Kilonova Ejecta

[ Oral ]

Chia-Hui Lin(Department of Physics, National Taiwan University);Ke-Jung Chen(Institute of Astronomy and Astrophysics, Academia Sinica);Meng-Ru Wu(Institute of Physics, Academia Sinica);Kuo-Chuan Pan(Institute of Astronomy, National Tsing Hua University)

Binary neutron star (BNS) merger is rich in fundamental physics with GW signals and electro-magnetic(EM) counterparts, and it is believed to be the main source of making r-process elements, whose radiative decay power the kilonovae. We present 3D GRMHD simulations of BNS and the comparison of different evo- lution methods with various initial setups by using a full GR code, Einsteintoolkit . We found the simulation without consideration of magnetic field emits more unbound outflow and the merger gravitational wave signal can be detected by LIGO if the merger site is shorter than 5 Mpc. For making predictions for future observations, we extend our simulations by using FLASH to produce synthetic observations of the kilonovae. In order to investigate the ejcta of nuclear heating from the decay of r-process ele- ments on the outflow. We perform the local mixing of kilonova ejecta with 2-layer model in different situations. The relation of instability merging rate and different physical variables such as velocity, heating rate, density and temperature is present. On conclusion, both the universal view of BNS and local view of mixing of ejecta are investgated. Testing various types of mixing with at physical scale is worth of future exploration.