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Simulations of Core-collapse Supernovae in Spatial Axisymmetry with Full Boltzmann Neutrino Transport
http://hdl.handle.net/2241/00153100
a703d39a-ce27-486b-9459-f3e6e6195dd8
名前 / ファイル | ライセンス | Actions | |
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item type | Journal Article(1) | |||||
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公開日 | 2018-08-23 | |||||
タイトル | ||||||
タイトル | Simulations of Core-collapse Supernovae in Spatial Axisymmetry with Full Boltzmann Neutrino Transport | |||||
言語 | ||||||
言語 | eng | |||||
資源タイプ | ||||||
タイプ | journal article | |||||
著者 |
Nagakura, Hiroki
× Nagakura, Hiroki× Iwakami, Wakana× Furusawa, Shun× Okawa, Hirotada× Harada, Akira× Sumiyoshi, Kohsuke× Yamada, Shoichi× Matsufuru, Hideo× Imakura, Akira |
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著者別名 |
今倉, 暁
× 今倉, 暁 |
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抄録 | ||||||
内容記述 | 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. | |||||
書誌情報 |
The Astrophysical Journal 巻 854, 号 2, p. 136, 発行日 2018-02 |
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ISSN | ||||||
収録物識別子 | 0004-637X | |||||
ISSN | ||||||
収録物識別子 | 1538-4357 | |||||
書誌レコードID | ||||||
収録物識別子 | AA00553253 | |||||
DOI | ||||||
権利 | ||||||
権利情報 | © 2018. The American Astronomical Society. | |||||
権利 | ||||||
権利情報 | 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. | |||||
著者版フラグ | ||||||
値 | publisher | |||||
出版者 | ||||||
出版者 | IOP Publishing |