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Prog. Theor. Phys. Vol. 114 No. 5 (2005) pp. 995-1020

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Effects of Magnetic Fields on Proto-Neutron Star Winds

Hirotaka Ito,1 Shoichi Yamada,1,2 Kohsuke Sumiyoshi3 and Shigehiro Nagataki4

1Department of Physics, Science, and Engineering, Waseda University, Tokyo 169-8555, Japan
2Advanced Research Institute for Science and Engineering, Waseda University, Tokyo 169-8555, Japan
3Numazu College of Technology, Numazu 410-8501, Japan
and
Division of Theoretical Astronomy, National Astronomical Observatory of Japan, Mitaka 181-8588, Japan
4Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan

(Received April 1, 2005)

Abstract:

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 1012G to 5 ×1015G) perpendicular to the radial direction and examine the dependence of the three key quantities (the dynamical time scale τ dyn, electron fraction Ye, 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, ∼1015G, 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.


URL : http://ptp.ipap.jp/link?PTP/114/995/
DOI : 10.1143/PTP.114.995

[ Full Text PDF : FREE ACCESS (2591K) ] Citation:

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