High resolution numerical relativity simulations for the merger of binary magnetized neutron stars

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Abstract

連星中性子星の合体とブラックホールの進化過程に新解釈 -スーパーコンピュータ「京」で磁場の増幅機構が明らかに-. 京都大学プレスリリース. 2014-09-01.

We perform high-resolution magnetohydrodynamics simulations of binary neutron star mergers in numerical relativity on the Japanese supercomputer K. The neutron stars and merger remnants are covered by a grid spacing of 70 m, which yields the highest-resolution results among those derived so far. By an in-depth resolution study, we clarify several amplification mechanisms of magnetic fields during the binary neutron star merger for the first time. First, the Kelvin-Helmholtz instability developed in the shear layer at the onset of the merger significantly amplifies the magnetic fields. A hypermassive neutron star (HMNS) formed after the merger is then subject to the nonaxisymmetric magnetorotational instability, which amplifies the magnetic field in the HMNS. These two amplification mechanisms cannot be found with insufficient-resolution runs. We also show that the HMNS eventually collapses to a black hole surrounded by an accretion torus which is strongly magnetized at birth.

Journal

  • Physical Review D

    Physical Review D 90(4), 2014-08-28

    American Physical Society

Codes

  • NII Article ID (NAID)
    120005469581
  • NII NACSIS-CAT ID (NCID)
    AA00773624
  • Text Lang
    ENG
  • Article Type
    journal article
  • ISSN
    1550-7998
  • Data Source
    IR 
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