Explosive Nucleosynthesis in Magnetohydrodynamical Jets from Collapsars(Astrophysics and Cosmology)

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概要

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• We investigate the nucleosynthesis of a massive star whose mass in the main sequence stage is M_<ms>=70M_⊙ that corresponds to the helium core or helium star of M_α=32M_⊙. Numerical calculations of the nucleosynthesis are performed during the stage of hydrostatic stellar evolution until the core composed of iron-group nuclei (Fe core) begins to collapse. A collapsar model whose jets are driven by two-dimensional magnetohydrodynamical effects of a differentially rotating core is constructed. The explosive nucleosynthesis inside the jets of a specified collapsar model is followed along the trajectories of stream lines. We combine the results of both detailed hydrostatic and explosive nucleosyntheses to compare the solar system abundances. We show that the agreement is considerably improved compared with the case without the detailed hydrostatic nucleosynthesis included. We suggest that many radioactive nuclei such as ^<44>Ti and ^<56,57>Ni are produced if the jets continue for more than 10s, which would become crucial for the observation of abundance distribution in young supernova remnants.

• 理論物理学刊行会の論文
• 2009-09-25

著者

• HASHIMOTO Masa-aki

  Department of Physics, Kyushu University

• Ono Masaomi

  Department of Physics, Kyushu University

• Hashimoto Masa-aki

  Department Of Physics Kyushu University

• Hashimoto Masa-aki

  Department Of Earth Science And Astronomy College Of Arts And Sciences University Of Tokyo

• Hashimoto Masa-aki

  Department Of Physics Faculty Of Science Kyusyu University

• Ono Masaomi

  Department Of Physics Kyushu University

• Fujimoto Shin-ichiro

  Kumamoto National College Of Technology

• Hashimoto Masa‐aki

  Kyushu Univ. Fukuoka

• Hashimoto M

  Department Of Physics Kyushu University

• KOTAKE Kei

  Division of Theoretical Astronomy National Astronomical Observatory of Japan

• YAMADA Shoichi

  Advanced Research Institute for Science and Engineering, Waseda University

• Kotake Kei

  Division Of Theoretical Astronomy National Astronomical Observatory Of Japan:center For Computationa

• Yamada Shoichi

  Advanced Research Institute For Science And Engineering Waseda University

• KOTAKE Kei

  Division of Theoretical Astronomy National Astronomical Observatory of Japan:Center for Computational Astrophysics, National Astronomical Observatory of Japan

• ONO Masaomi

  Yukawa Institute for Theoretical Physics, Kyoto University:Department of Physics, Kyushu University

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