Effects of magnetic fields on proto-neutron star winds

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

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

2 Citations (Scopus)


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.

Original languageEnglish
Pages (from-to)995-1020
Number of pages26
JournalProgress of Theoretical Physics
Issue number5
Publication statusPublished - 2005 Nov

ASJC Scopus subject areas

  • Physics and Astronomy (miscellaneous)


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