General relativistic magnetohydrodynamic simulations of collapsars: Rotating black hole cases

Y. Mizuno, Shoichi Yamada, S. Koide, K. Shibata

    Research output: Contribution to journalArticle

    Abstract

    We have performed 2.5-dimensional general relativistic magnetohy-drodynamic (MHD) simulations of collapsars including a rotating black hole. Initially, we assume that the core collapse has failed in this star. A rotating black hole of a few solar masses is inserted by hand into the calculation. The simulation results show the formation of a disklike structure and the generation of a jetlike outflow near the central black hole. The jetlike outflow propagates and accelerated mainly by the magnetic field. The total jet velocity is ∼ 0.3c. When the rotation of the black hole is faster, the magnetic field is twisted strongly owing to the frame-dragging effect. The magnetic energy stored by the twisting magnetic field is directly converted to kinetic energy of the jet rather than propagating as an Alfvén wave. Thus, as the rotation of the black hole becomes faster, the poloidal velocity of the jet becomes faster.

    Original languageEnglish
    Pages (from-to)423-426
    Number of pages4
    JournalNuovo Cimento della Societa Italiana di Fisica C
    Volume28
    Issue number3
    DOIs
    Publication statusPublished - 2005 May

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    magnetohydrodynamic simulation
    magnetic fields
    twisting
    simulation
    kinetic energy
    stars

    ASJC Scopus subject areas

    • Astronomy and Astrophysics
    • Physics and Astronomy (miscellaneous)

    Cite this

    General relativistic magnetohydrodynamic simulations of collapsars : Rotating black hole cases. / Mizuno, Y.; Yamada, Shoichi; Koide, S.; Shibata, K.

    In: Nuovo Cimento della Societa Italiana di Fisica C, Vol. 28, No. 3, 05.2005, p. 423-426.

    Research output: Contribution to journalArticle

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