Effects of Magnetic Fields on Proto-Neutron Star Winds(Astrophysics and Relativity)
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概要
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We investigate the effects of magnetic fields on proto-neutron star winds by performing numerical simulations. We assume that the atmosphere of a proto-neutron star has a homogenous magnetic field (ranging from 10^<12>G to 5×10^<15>G) perpendicular to the radial direction and examine the dependence of the three key quantities (the dynamical time scale T_<dyn>, electron fraction Y_e, and entropy per baryon s) for the successful r-process on the magnetic field strength. Our results show that even with a magneter-class field strength, 〜10^<15>G, the features of the wind dynamics differ only little from those of non-magnetic winds and that the conditions for an effective r-process are not realized.
- 理論物理学刊行会の論文
- 2005-11-25
著者
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NAGATAKI Shigehiro
Yukawa Institute for Theoretical Physics, Kyoto University
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Nagataki Shigehiro
Yukawa Institute For Theoretical Physics Kyoto University
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Ito Hirotaka
Department Of Otorhinolaryngology Nagoya City University Medical School
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Ito Hirotaka
Department Of Physics Science And Engineering Waseda University
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SUMIYOSHI Kohsuke
Numazu College of Technology
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YAMADA Shoichi
Department of Physics, Science, and Engineering, Waseda University
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Yamada Shoichi
Department Of Physics The University Of Tokyo
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Yamada Shoichi
Department Of Physics School Of Science The University Of Tokyo
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Shoichi Yamada
Department Of Physics Science And Engineering Waseda University:advanced Research Institute For Scie
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Nagataki Shigehiro
Yukawa Inst. Theoretical Physics Kyoto
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Nagataki Shigehiro
Hiroshima Univ. Higashi‐hiroshima Jpn
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Sumiyoshi Kohsuke
Numazu Coll. Technol. Numazu Jpn
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YAMADA Shoichi
Department of Physics, Science, and Engineering, Waseda University:Advanced Research Institute for Science and Engineering, Waseda University
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Ito Hirotaka
Department of Neurosurgery, Tokyo Metropolitan Neurological Hospital, Japan
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Yamada Shoichi
Department of Chemistry, University of Tsukuba
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