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

Harada, Akira and Nagakura, Hiroki and Iwakami, Wakana and Okawa, Hirotada and Furusawa, Shun and Matsufuru, Hideo and Sumiyoshi, Kohsuke and Yamada, Shoichi (2019) On the Neutrino Distributions in Phase Space for the Rotating Core-collapse Supernova Simulated with a Boltzmann-neutrino-radiation-hydrodynamics Code. Astrophysical Journal, 872 (2). Art. No. 181. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20190225-092533902

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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, 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 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 ~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.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/ab0203DOIArticle
https://arxiv.org/abs/1810.12316arXivDiscussion Paper
ORCID:
AuthorORCID
Nagakura, Hiroki0000-0002-7205-6367
Iwakami, Wakana0000-0003-4959-069X
Sumiyoshi, Kohsuke0000-0002-9224-9449
Yamada, Shoichi0000-0002-2166-5605
Additional Information:© 2019 The American Astronomical Society. Received 2018 October 27; revised 2019 January 11; accepted 2019 January 25; published 2019 February 25. We thank Yu Yamamoto for providing us with a subroutine that calculates internal energy of electrons and positrons. This research used high-performance computing resources of the K-computer and the FX10 of the HPCI system provided by the AICS and the University of Tokyo through the HPCI System Research Project (Project ID: hp160071, hp170031, and hp180111), the Computing Research Center in KEK, JLDG on SINET4 of NII, the Research Center for Nuclear Physics at Osaka University, the Yukawa Institute of Theoretical Physics at Kyoto University, and the Information Technology Center at the University of Tokyo. This work was supported by the Grant-in-Aid for Scientific Research (26104006, 15K05093, 16H03986), Grant-in-Aid for Innovative Areas (24103006), and Grant-in-Aid for Scientific Research on Innovative areas "Gravitational wave physics and astronomy:Genesis" (17H06357, 17H06365) from the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan. This work was also partly supported by research programs at K-computer of the RIKEN AICS, HPCI Strategic Program of Japanese MEXT, "Priority Issue on Post-K-computer" (Elucidation of the Fundamental Laws and Evolution of the Universe), and Joint Institute for Computational Fundamental Sciences (JICFus). A.H. was supported in part by the Advanced Leading Graduate Course for Photon Science (ALPS) at the University of Tokyo and Grant-in-Aid for JSPS Research Fellow (JP17J04422). H.N. was supported partially by JSPS Postdoctoral Fellowships for Research Abroad No. 27-348, Caltech through NSF award No. TCAN AST-1333520, and DOE SciDAC4 Grant DE-SC0018297 (subaward 00009650). Software: gnuplot Williams et al. (2013).
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
Ministry of Education, Culture, Sports, Science and Technology (MEXT)26104006
Ministry of Education, Culture, Sports, Science and Technology (MEXT)15K05093
Ministry of Education, Culture, Sports, Science and Technology (MEXT)16H03986
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24103006
Ministry of Education, Culture, Sports, Science and Technology (MEXT)17H06357
Ministry of Education, Culture, Sports, Science and Technology (MEXT)17H06365
University of TokyoUNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP17J04422
Japan Society for the Promotion of Science (JSPS)27-348
NSFAST-1333520
Department of Energy (DOE)DE-SC0018297
Department of Energy (DOE)00009650
Subject Keywords:methods: numerical – neutrinos – radiative transfer – shock waves – supernovae: general
Record Number:CaltechAUTHORS:20190225-092533902
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190225-092533902
Official Citation:Akira Harada et al 2019 ApJ 872 181
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:93202
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:25 Feb 2019 17:46
Last Modified:25 Feb 2019 17:46

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