Effects of Magnetic Fields on Proto-Neutron Star Winds | Zendy

Hirotaka Ito | Zendy; S. Yamada | Zendy; Kohsuke Sumiyoshi | Zendy; Shigehiro Nagataki | Zendy

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Effects of Magnetic Fields on Proto-Neutron Star Winds

Author(s) -

Hirotaka Ito,

S. Yamada,

Kohsuke Sumiyoshi,

Shigehiro Nagataki

Publication year - 2005

Publication title -

progress of theoretical physics

Language(s) - English

Resource type - Journals

eISSN - 1347-4081

pISSN - 0033-068X

DOI - 10.1143/ptp.114.995

Subject(s) - physics , magnetic field , neutron star , field strength , baryon , neutron , astrophysics , magnetohydrodynamics , computational physics , nuclear physics , quantum mechanics

We discuss effects of magnetic fields on proto-neutron star winds by performing numerical simulation. We assume that the atmosphere of proto-neutron star has a homogenous magnetic field (ranging from ~10^{12} G to ~10^{15} G) perpendicular to the radial direction and examine the dependence of the three key quantities (dynamical time scale, electron fraction, and entropy per baryon) 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 feature of the wind dynamics varies only little from that of non-magnetic winds, and that the condition for successful r-process is not realized

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