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  1. システム情報系 (Faculty of Engineering, Information and Systems)
  2. 今倉 暁 (Imakura Akira)
  1. コンテンツタイプ (Contents Type)
  2. 雑誌発表論文等 (Journal article, etc.)
  3. A~
  4. Astrophysical journal

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

http://hdl.handle.net/2241/00153100
a703d39a-ce27-486b-9459-f3e6e6195dd8
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AJ_854-2-136.pdf AJ_854-2-136 (4.5 MB)
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item type Journal Article(1)
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

WEKO 201308

Nagakura, Hiroki

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Iwakami, Wakana

× Iwakami, Wakana

WEKO 201309

Iwakami, Wakana

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Furusawa, Shun

× Furusawa, Shun

WEKO 201310

Furusawa, Shun

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Okawa, Hirotada

× Okawa, Hirotada

WEKO 201311

Okawa, Hirotada

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Harada, Akira

× Harada, Akira

WEKO 201312

Harada, Akira

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Sumiyoshi, Kohsuke

× Sumiyoshi, Kohsuke

WEKO 201313

Sumiyoshi, Kohsuke

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Yamada, Shoichi

× Yamada, Shoichi

WEKO 201314

Yamada, Shoichi

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Matsufuru, Hideo

× Matsufuru, Hideo

WEKO 201315

Matsufuru, Hideo

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Imakura, Akira

× Imakura, Akira

WEKO 201316

Imakura, Akira

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著者別名 今倉, 暁

× 今倉, 暁

WEKO 201384
e-Rad 60610045
筑波大学研究者総覧 0000003376

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
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
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