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Simulations of Core-collapse Supernovae in Spatial Axisymmetry with Full Boltzmann Neutrino Transport

Nagakura, Hiroki and Iwakami, Wakana and Furusawa, Shun and Okawa, Hirotada and Harada, Akira and Sumiyoshi, Kohsuke and Yamada, Shoichi and Matsufuru, Hideo and Imakura, Akira (2018) Simulations of Core-collapse Supernovae in Spatial Axisymmetry with Full Boltzmann Neutrino Transport. Astrophysical Journal, 854 (2). Art. No. 136. ISSN 1538-4357. http://resolver.caltech.edu/CaltechAUTHORS:20180222-105004915

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Abstract

We present the first results of our spatially axisymmetric core-collapse supernova simulations with full Boltzmann neutrino transport, which amount to a time-dependent five-dimensional (two in space and three in momentum space) problem. Special relativistic effects are fully taken into account with a two-energy-grid technique. We performed two simulations for a progenitor of 11.2 M☉, employing different nuclear equations of state (EOSs): Lattimer and Swesty's EOS with the incompressibility of K = 220 MeV (LS EOS) and Furusawa's EOS based on the relativistic mean field theory with the TM1 parameter set (FS EOS). In the LS EOS, the shock wave reaches ~700 km at 300 ms after bounce and is still expanding, whereas in the FS EOS it stalled at ~200 km and has started to recede by the same time. This seems to be due to more vigorous turbulent motions in the former during the entire postbounce phase, which leads to higher neutrino-heating efficiency in the neutrino-driven convection. We also look into the neutrino distributions in momentum space, which is the advantage of the Boltzmann transport over other approximate methods. We find nonaxisymmetric angular distributions with respect to the local radial direction, which also generate off-diagonal components of the Eddington tensor. We find that the rθ component reaches ~10% of the dominant rr component and, more importantly, it dictates the evolution of lateral neutrino fluxes, dominating over the θθ component, in the semitransparent region. These data will be useful to further test and possibly improve the prescriptions used in the approximate methods.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-4357/aaac29DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/aaac29/metaPublisherArticle
https://arxiv.org/abs/1702.01752arXivDiscussion 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:© 2018 The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2017 June 30; revised 2018 January 16; accepted 2018 January 29; published 2018 February 21. H.N. acknowledges C. D. Ott, S. Richers, L. Roberts, D. Radice, M. Shibata, Y. Sekiguchi, K. Kiuchi, and T. Takiwaki for valuable comments and discussions. The numerical computations were performed on the K computer, at AICS, FX10 at the Information Technology Center of Tokyo University, on SR16000 at YITP of Kyoto University, on SR16000 and Blue Gene/Q at KEK under the support of its Large Scale Simulation Program (14/15-17, 15/16-08, 16/17-11), Research Center for Nuclear Physics (RCNP) at Osaka University, and on the XC30 and the general common use computer system at the Center for Computational Astrophysics, CfCA, the National Astronomical Observatory of Japan. Large-scale storage of numerical data is supported by JLDG constructed over SINET4 of NII. H.N. and S.F. were supported in part by JSPS Postdoctoral Fellowships for Research Abroad No. 27-348 and 28-472, and H.N. was partially supported at Caltech through NSF award No. TCAN AST-1333520. This work was supported by a Grant-in-Aid for Scientific Research from the Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan (15K05093, 24103006, 24105008, 24740165, 24244036, 25870099, 26104006, 16H03986, 17H06357, 17H06365) and the HPCI Strategic Program of Japanese MEXT and K computer at the RIKEN and Post-K project (Project ID: hp 140211, 150225, 160071, 160211, 170230, 170031, 170304).
Group:TAPIR, Walter Burke Institute for Theoretical Physics
Funders:
Funding AgencyGrant Number
Japan Society for the Promotion of Science (JSPS)27-348
Japan Society for the Promotion of Science (JSPS)28-472
NSFAST-1333520
Ministry of Education, Culture, Sports, Science and Technology (MEXT)15K05093
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24103006
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24105008
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24740165
Ministry of Education, Culture, Sports, Science and Technology (MEXT)24244036
Ministry of Education, Culture, Sports, Science and Technology (MEXT)25870099
Ministry of Education, Culture, Sports, Science and Technology (MEXT)26104006
Ministry of Education, Culture, Sports, Science and Technology (MEXT)16H03986
Ministry of Education, Culture, Sports, Science and Technology (MEXT)17H06357
Ministry of Education, Culture, Sports, Science and Technology (MEXT)17H06365
Subject Keywords:hydrodynamics – neutrinos – supernovae: general
Record Number:CaltechAUTHORS:20180222-105004915
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20180222-105004915
Official Citation:Hiroki Nagakura et al 2018 ApJ 854 136
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:84921
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:22 Feb 2018 19:09
Last Modified:22 Feb 2018 19:09

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