Effects of magnetic fields on proto-neutron star winds

Hirotaka Ito; Shoichi Yamada; Kohsuke Sumiyoshi; Shigehiro Nagataki

doi:10.1143/PTP.114.995

Effects of magnetic fields on proto-neutron star winds

Hirotaka Ito^*, Shoichi Yamada, Kohsuke Sumiyoshi, Shigehiro Nagataki

^*Corresponding author for this work

School of Advanced Science and Engineering

Research output: Contribution to journal › Article › peer-review

2 Citations (Scopus)

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 10 ¹²G 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 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 ¹⁵G, 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.

Original language	English
Pages (from-to)	995-1020
Number of pages	26
Journal	Progress of Theoretical Physics
Volume	114
Issue number	5
DOIs	https://doi.org/10.1143/PTP.114.995
Publication status	Published - 2005 Nov

ASJC Scopus subject areas

Physics and Astronomy (miscellaneous)

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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 10 12G to 5 × 1015G) perpendicular to the radial direction and examine the dependence of the three key quantities (the dynamical time scale τdyn, 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, ∼ 10 15G, 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.",

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Effects of magnetic fields on proto-neutron star winds

Abstract

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