Effects of magnetic fields on proto-neutron star winds

Hirotaka Ito, Shoichi Yamada, Kohsuke Sumiyoshi, Shigehiro Nagataki

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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.

    Original languageEnglish
    Pages (from-to)995-1020
    Number of pages26
    JournalProgress of Theoretical Physics
    Volume114
    Issue number5
    Publication statusPublished - 2005 Nov

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    ASJC Scopus subject areas

    • Physics and Astronomy(all)

    Cite this

    Ito, H., Yamada, S., Sumiyoshi, K., & Nagataki, S. (2005). Effects of magnetic fields on proto-neutron star winds. Progress of Theoretical Physics, 114(5), 995-1020.