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J-GLOBAL ID：201702267428202928   整理番号：17A0935457

P30(p , γ)31反応速度の重要な共鳴状態の測定と新星爆発における中間質量元素の生産【Powered by NICT】

Measurement of key resonance states for the P 30 ( p , γ ) S 31 reaction rate, and the production of intermediate-mass elements in nova explosions

著者 (54件)： Kankainen A. (University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom) ,  Woods P.J. (University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom) ,  Schatz H. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Schatz H. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Schatz H. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA) ,  Poxon-Pearson T. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Poxon-Pearson T. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Poxon-Pearson T. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA) ,  Doherty D.T. (University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom) ,  Bader V. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Bader V. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Baugher T. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Bazin D. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Brown B.A. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Brown B.A. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Brown B.A. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA) ,  Browne J. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Browne J. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Browne J. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA) ,  Estrade A. (University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom) ,  Gade A. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Gade A. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Jose J. (Departament de Fisica, EEBE, Universitat Politecnica de Catalunya, E-08019 Barcelona, Spain) ,  Jose J. (Institut d’Estudis Espacials de Catalunya, E-08034 Barcelona, Spain) ,  Kontos A. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Langer C. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Lotay G. (University of Edinburgh, Edinburgh EH9 3JZ, United Kingdom) ,  Meisel Z. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Meisel Z. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Meisel Z. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA) ,  Montes F. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Montes F. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA) ,  Noji S. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Nunes F. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Nunes F. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Nunes F. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA) ,  Perdikakis G. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA) ,  Perdikakis G. (Central Michigan University, Mount Pleasant, MI 48859, USA) ,  Pereira J. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Pereira J. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA) ,  Recchia F. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Redpath T. (Central Michigan University, Mount Pleasant, MI 48859, USA) ,  Stroberg R. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Stroberg R. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Scott M. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Scott M. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Seweryniak D. (Argonne National Laboratory, Argonne, IL 60439, USA) ,  Stevens J. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Stevens J. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA) ,  Weisshaar D. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Wimmer K. (Central Michigan University, Mount Pleasant, MI 48859, USA) ,  Zegers R. (National Superconducting Cyclotron Laboratory, Michigan State University, East Lansing, MI 48824, USA) ,  Zegers R. (Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA) ,  Zegers R. (JINA Center for the Evolution of the Elements, Michigan State University, East Lansing, MI 48824, USA)
資料名： Physics Letters. B  (Physics Letters. B)
巻： 769  ページ： 549-553  発行年： 2017年 
JST資料番号： B0779A  ISSN： 0370-2693  CODEN： PYLBA  資料種別： 逐次刊行物 (A)
記事区分： 原著論文  発行国： オランダ (NLD)  言語： 英語 (EN)

抄録/ポイント： 新星噴出物中のCaまでの中間質量元素の生産を決定するための臨界30(p , γ)31反応における重要な共鳴の分光学的因子と強度に関する最初の実験制約条件を報告した。P30(d , n)31反応は陽子しきい値より上の状態の角度積分断面積を測定するためにGRETINAγ線アレイを用いた逆運動学で研究した。一般に,負パリティ状態が最も強く生成することが分かったが,分光学的因子の絶対値は典型的に負パリティ状態に対するWBPハミルトニアンを用いた殻模型計算による予測より1桁低かった。結果は新星燃焼T≒0.10 0.17GK領域における196keVでの単一3/2 共鳴状態の優位性を示し,新星元素合成のための関心領域内で明らかになった。新星爆発の流体力学的シミュレーションは,新星噴出物の組成に及ぼす効果を実証するために実行した。Copyright 2017 Elsevier B.V., Amsterdam. All rights reserved. Translated from English into Japanese by JST.【Powered by NICT】

シソーラス用語： 火山噴出物 ,  殻模型 ,  陽子 ,  *反応速度 ,  シミュレーション ,  パリティ ,  カルシウム ,  元素合成 ,  γ線 ,  *新星 ,  ハミルトニアン ,  分光学的因子 ,  流体力学
準シソーラス用語： 逆運動学 ,  *共鳴状態 , 【Automatic Indexing@JST】

分類 (1件)： 宇宙線起源  (DB02020Q)

タイトルに関連する用語 (4件)： 反応速度 ,  共鳴状態 ,  質量 ,  元素