期刊
ASTROPHYSICAL JOURNAL
卷 872, 期 2, 页码 -出版社
IOP Publishing Ltd
DOI: 10.3847/1538-4357/ab0203
关键词
methods: numerical; neutrinos; radiative transfer; shock waves; supernovae: general
资金
- University of Tokyo through the HPCI System Research Project [hp160071, hp170031, hp180111]
- Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan [26104006, 15K05093, 16H03986, 24103006, 17H06357, 17H06365]
- RIKEN AICS
- HPCI Strategic Program of Japanese MEXT
- Priority Issue on Post-K-computer (Elucidation of the Fundamental Laws and Evolution of the Universe)
- Joint Institute for Computational Fundamental Sciences (JICFus)
- Advanced Leading Graduate Course for Photon Science (ALPS) at the University of Tokyo
- JSPS [27348]
- Caltech through NSF [TCAN AST-1333520]
- DOE SciDAC4 [DE-SC0018297, 00009650]
- [JP17J04422]
With the Boltzmann-radiation-hydrodynamics code, which we have developed to solve numerically the Boltzmann equations for neutrino transfer, the Newtonian hydrodynamics equations, and the Newtonian self-gravity simultaneously and consistently, we simulate the collapse of a rotating core of the progenitor with a zero-age- main-sequence mass of 11.2 M-circle dot and a shellular rotation of 1 rad s(-1) at the center. We pay particular attention in this paper to the neutrino distribution in phase space, which is affected by the rotation. By solving the Boltzmann equations directly, we can assess the rotation-induced distortion of the angular distribution in momentum space, which gives rise to the rotational component of the neutrino flux. We compare the Eddington tensors calculated both from the raw data and from the M1-closure approximation. We demonstrate that the Eddington tensor is determined by complicated interplays of the fluid velocity and the neutrino interactions and that the M1-closure, which assumes that the Eddington factor is determined by the flux factor, fails to fully capture this aspect, especially in the vicinity of the shock. We find that the error in the Eddington factor reaches similar to 20% in our simulation. This is due not to the resolution but to the different dependence of the Eddington and flux factors on the angular profile of the neutrino distribution function, and hence modification to the closure relation is needed.
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