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Title: On the Neutrino Distributions in Phase Space for the Rotating Core-collapse Supernova Simulated with a Boltzmann-neutrino-radiation-hydrodynamics Code

Abstract

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, in this work we simulate the collapse of a rotating core of the progenitor with a zero-age- main-sequence mass of 11.2 M and a shellular rotation of $$1\,\mathrm{rad}\,{{\rm{s}}}^{-1}$$ 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 ~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.

Authors:
 [1]; ORCiD logo [2]; ORCiD logo [3];  [3];  [4];  [5]; ORCiD logo [6]; ORCiD logo [7]
  1. Univ. of Tokyo (Japan)
  2. Princeton Univ., NJ (United States); California Inst. of Technology (CalTech), Pasadena, CA (United States)
  3. Kyoto Univ. (Japan); Waseda Univ., Tokyo (Japan)
  4. RIKEN, Saitama (Japan). Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS)
  5. High Energy Accelerator Research Organization, Ibaraki (Japan)
  6. Numazu College of Technology (Japan)
  7. Waseda Univ., Tokyo (Japan)
Publication Date:
Research Org.:
Univ. of California, Oakland, CA (United States)
Sponsoring Org.:
Ministry of Education, Culture, Sports, Science and Technology (MEXT); Japan Society for the Promotion of Science (JSPS); National Science Foundation (NSF); USDOE Office of Science (SC), Advanced Scientific Computing Research (ASCR). Scientific Discovery through Advanced Computing (SciDAC)
OSTI Identifier:
1612911
Grant/Contract Number:  
SC0018297; 26104006; 15K05093; 16H03986; 24103006; 17H06357; 17H06365; JP17J04422; TCAN AST-1333520
Resource Type:
Accepted Manuscript
Journal Name:
The Astrophysical Journal (Online)
Additional Journal Information:
Journal Name: The Astrophysical Journal (Online); Journal Volume: 872; Journal Issue: 2; Journal ID: ISSN 1538-4357
Publisher:
Institute of Physics (IOP)
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS; astronomy & astrophysics; methods: numerical; neutrinos; radiative transfer; shock waves; supernovae: general

Citation Formats

Harada, Akira, Nagakura, Hiroki, Iwakami, Wakana, Okawa, Hirotada, Furusawa, Shun, Matsufuru, Hideo, Sumiyoshi, Kohsuke, and Yamada, Shoichi. On the Neutrino Distributions in Phase Space for the Rotating Core-collapse Supernova Simulated with a Boltzmann-neutrino-radiation-hydrodynamics Code. United States: N. p., 2019. Web. doi:10.3847/1538-4357/ab0203.
Harada, Akira, Nagakura, Hiroki, Iwakami, Wakana, Okawa, Hirotada, Furusawa, Shun, Matsufuru, Hideo, Sumiyoshi, Kohsuke, & Yamada, Shoichi. On the Neutrino Distributions in Phase Space for the Rotating Core-collapse Supernova Simulated with a Boltzmann-neutrino-radiation-hydrodynamics Code. United States. https://doi.org/10.3847/1538-4357/ab0203
Harada, Akira, Nagakura, Hiroki, Iwakami, Wakana, Okawa, Hirotada, Furusawa, Shun, Matsufuru, Hideo, Sumiyoshi, Kohsuke, and Yamada, Shoichi. Mon . "On the Neutrino Distributions in Phase Space for the Rotating Core-collapse Supernova Simulated with a Boltzmann-neutrino-radiation-hydrodynamics Code". United States. https://doi.org/10.3847/1538-4357/ab0203. https://www.osti.gov/servlets/purl/1612911.
@article{osti_1612911,
title = {On the Neutrino Distributions in Phase Space for the Rotating Core-collapse Supernova Simulated with a Boltzmann-neutrino-radiation-hydrodynamics Code},
author = {Harada, Akira and Nagakura, Hiroki and Iwakami, Wakana and Okawa, Hirotada and Furusawa, Shun and Matsufuru, Hideo and Sumiyoshi, Kohsuke and Yamada, Shoichi},
abstractNote = {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, in this work we simulate the collapse of a rotating core of the progenitor with a zero-age- main-sequence mass of 11.2 M⊙ and a shellular rotation of $1\,\mathrm{rad}\,{{\rm{s}}}^{-1}$ 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 ~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.},
doi = {10.3847/1538-4357/ab0203},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 872,
place = {United States},
year = {Mon Feb 25 00:00:00 EST 2019},
month = {Mon Feb 25 00:00:00 EST 2019}
}

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text, January 2018


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Works referencing / citing this record:

Fast-pairwise Collective Neutrino Oscillations Associated with Asymmetric Neutrino Emissions in Core-collapse Supernovae
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